SkyTour - The Sun - Astro Potpourri

Along with Tara and Marc, perhaps we will also hear from "Snappy" the program director as we talk astronomy and new objects people are seeing. We will talk about 3I/ATLAS

Episode Transcript

Speaker 1 (00:14):
The universes called the universe is calling.

Speaker 2 (00:29):
It speaks both.

Speaker 3 (00:31):
Day and night.

Speaker 2 (00:37):
It's fall of door.

Speaker 1 (00:40):
Can Hey, hey, I'm okay, everybody, welcome to Skyter Radio.

(01:12):
I am Marked Antonio, and you know that is as
Tara and tonight we are at our new place in time.
We are running from eight to ten on Wednesday nights
now and that's going to give us a chance to
do more live shows because the weekend sometimes gets crowded,
and so we've had the replays. Absolutely don't like doing those,

(01:34):
so now we have a better opportunity. And she demanded
it anyway, So.

Speaker 4 (01:39):
It was her. That's right.

Speaker 1 (01:41):
She wants she wants to be seen on camera all
the time.

Speaker 4 (01:44):
No, no, I want to hear about the universe the secrets,
but I want answers if you don't mind.

Speaker 1 (01:52):
Oh no, no, you're absolutely right, And tonight we're gonna
do that. My shirt actually says that, I mean, I
have answers on the shirt. But I was telling terror,
really right, let's use all these equations at one time
or another, oh mostly another, but that the tonight is

(02:12):
skyte Radio's debut, as I said, and it's now we're
gonna do a little it's sort of a presentation. But
we're gonna Tara and I are gonna go back and
forth on a bunch of things. We're gonna be talking
about planets around the other stars, extra planets, and I'm
gonna give you a little bit more data than I've
ever given you before on this We've never gone down
this particular path, and you'll get to see a little

(02:34):
more detail what we're talking about.

Speaker 4 (02:37):
So that no test later, is there?

Speaker 1 (02:43):
Oh no, okay, okay, yes, yes, no quiz yeah, pop
quiz right, yeah, as soon as the quiz comes out,
you pop out of the room. Uh no. So I
just wanted to share with you for those that saw
the video I produced of the Benson site, I put
it up on Facebook, I believe. I don't know if

(03:06):
you got to see that, Tara, yeah, face yeah, and
I it was big, so I couldn't just send it,
you know, that was part of the problem. So that
just wanted to show you some of the photos when
you go out to the news site. We have you know,
skyter Livestream remote observatories as you know, and STLs one

(03:29):
is out in the Sonoran Desert. Okay, it's western Phoenix
by about seventy five miles. Tara knows the site well,
she's been out there a thousand times. You know, without her,
that would never have been set up. Her and Marianne
rob you know, I never yeah, I would have never
had fun.

Speaker 4 (03:45):
Was very fun.

Speaker 1 (03:47):
Yeah, And now we have a second site thanks to
the people that are provided donations and stuff that help us,
because we are a five oh one c three nonprofit
organization all so thanks in part to that one over there.
You know, we couldn't have done one out to read there.
And the Benson site in Benson, Arizona is actually a

(04:11):
site where we're on a high plateau and there's ten
observatories up there, actually twelve observatories up there, and there's
ten in a long row. And that long row looks
like this. Okay. Each of those cubes that you see
are an observatory where the roof rolls off and telescope

(04:33):
inside can now peer up and look at the sky
and do its thing. The closest one here in this picture,
which is right there, to the to the to the
well this way here okay. Yeah. On the other hand,
it's just on right here, okay. Is this is a
door to a storage closet and where I'm actually with

(04:54):
my hand. That's our observatory is a little bit more
this way. But that one right next to us that
you see past that door, that is a very active
astronomer who's on almost every clear night he's doing analysis
of the night sky. And then further down there's another
astronomer that has a telescope in there. I've seen him

(05:16):
and met him. Now. The thing that's interesting when I
say seen them and met them, these guys are all
running remotely from wherever they are in the country or
even the world. And so I'm in Connecticut, okay, and
I'm running the one in Benson, which is about twenty
five hundred miles away, and so I run it from here.

(05:39):
But then we have the one in the Sonoran Desert,
which is about twenty six hundred miles away, but they
run that from here too, And many times if I
have Benson open, I have the sky Tours Sonoran opened
as well. And we have two different telescopes. Right, we
have the wide field one that shows big, giant, expansive

(06:00):
views of the sky. In fact, the picture behind us
in this image here, okay, this big vast picture behind us,
it was taken with our sky Tour Sonarin telescope the
sky to a Sonoran telescope. With that wide field, it's
three full moons across and one full moon tall, two
full moons across and one full moon tall in size,

(06:21):
and we see that giant swath of sky. So we
get all these nebulas and all these things very very quickly.
The telescope runs very fast, you know, photographically. The Benson telescope,
on the other hand, that one's a little more technical
because we have a much smaller field of view. So
we've been only be looking at a section of this
nebula that we're looking at here and behind us, okay,

(06:45):
and these images would be or would be shown at
the same time as we're looking at, say this wide object,
we'd show a close up of that same object, and
we do in the Benson telescope, so they have both options.
People watching from wherever they are. We've got people from China, Thailand, Columbia, Chile, Mexico,

(07:08):
United States, of course, Japan, Yeah, Australia, that's right, we
got some we got facts from Dan and right, and
you know, those folks wherever they're watching from, they get
to see two views of the same thing, one close
up and one a much wider field view, and we

(07:30):
make all those photos available to everybody for free. Now,
the benefit of giving them away for free is because
they are the raw photos, the photos we take out
of the camera, and they just get saved up to
our server which you have access to. And our server
is located at at a place that everybody knows, and

(07:51):
it's skyterlive dot org right there, Okay, that's our portal.
And so we make the photos available to everybody. And
when they see these photos, they're free to download them.
But if they join our Patreon and they end up
coming in and you know, subscribing monthly to us, then

(08:12):
what we do is that's effectively you paying me and
several other people that we have to process the photos
and produce highly competent finished pieces of art. Okay, we don't.
We don't jeopardize the data so you could use it
for scientific purposes. In fact, one of our viewers is

(08:34):
using our data, okay, in conjunction with another professional astrophysicist
data and finding stars that seem to have been missing.
And what she's doing is she is actually correlating the
old historic plates combined with viewing our plates combined with

(08:55):
viewing this astrophysicist plates and seeing the differences and seeing
what's going on and what has been going on historically
in these regions in the sky. It's amazing how things change.

Speaker 4 (09:07):
How fun that would be to do. I mean, it
seems like you're be Tenius had to be interesting. Really
it is.

Speaker 1 (09:14):
It is, you know, and people know her as Isabella
in our chat and she is one of the most
dedicated people. She wrote our app, which will be on
the iPhone, Android and PC and mac. Okay, we already
have it on the PC just as a test base.
I've got it on my phone as a test base too,

(09:35):
And we have all of our observations for all the
years we've been doing this, almost all in one place.
You can search every time we photograph this thing behind
us right now, This is the lagoon Nebula over there
buying Tara. Behind me is the Chinese dragon Nebula. It's
a summertime sky onzec. Well, you can go look up

(09:56):
every single time we photograph them and look at all
the pictures of the times we and then you could
compare them to each other and see what's different. You
might find an asteroid, okay, because an interloper and they
would show up. It is like a little star, little dot. Okay.
And if it's missing from one of them and it's

(10:16):
in the other, well you found something that wasn't there
because they weren't taken at the same time. They were
taken usually months apart, so or even weeks. So it's
pretty cool. And so we can do real science now
with our skyterro life telescopes, and if all goes well,
we'll be able to have a spectrograph in addition on

(10:39):
our Benson telescope. And I wants a spectrograph. Well, if
you look at the sun, if you were just.

Speaker 5 (10:45):
To look at the sun, don't do it, don't do it,
but look at the sun.

Speaker 1 (10:49):
If you theoretically, hypothetically look at the sun, you'll find
that you take a prism and you'll see that the
Sun's light breaks up into these colors right red, orange, yellow, green, blue, indigo,
and violet. Okay, we call that Roy G Biff. Right now,

(11:09):
if you can generate those colors, one of the things
you'll see with the sun is that there are lines,
the vertical lines in that spectrum as well. Now, what
are those? Okay? Well, I can show you here is
an example. The light the source of light right there,

(11:30):
that's the that's the Sun's core. Yeah, the hot source,
that's the that's break my face. Okay, that hot little source,
that's the Sun's core. And then that next thing called
this says gas right there, that's actually the outer atmosphere
of the sun. The core of the Sun is you know,
over ten million degrees celsius, okay, and this gas is

(11:57):
only about ten thousand degrees celsius or so. And so
what happens is when the hot radiation passes through a
relatively cooler gas, that relatively cool gas will absorb some
of the energy and make what we see on the

(12:17):
right there an absorption spectrum. Will see dark lines. Now
what are those lines? Those lines are lines that exist
from the chemical compounds in this outer the I should say,
the nuclei of these at the nuclei the atoms. The
atoms can exist in the hot gas. It's all plasma.

(12:40):
The nuclei are absorbing some of this energy, and like prinstance,
hydrogen atoms absorbed in a specific location in the spectrum,
calcium absorbs in a specific location in the spectrum, et cetera.
Et cetera. So where they appear in the spectrum is

(13:00):
absolutely dependent on what element we're seeing. Okay, the are
it's almost like a fingerprint of the star, all right,
and in our star it's so reliably the same. We
call it the Fraunhoffer spectrum. It's actually a spectrum that
has been seen ever since we were looking at spectrum
of the sun. Now, if you look just at the

(13:21):
sun without you know, looking if you look only at
the hot source, we'd see just the colors like this
that I showed you, Okay, but we don't we see
this because we're always not that. Okay, we see this
because we're always looking through the outer shell of the
gas around that hot core. Now, if you could actually,

(13:44):
uh look at just the hot gas on the outside
of the sun and block out the hot core, then
you see different lines. You see things called emission lines,
these emission spectra. Okay, and I'll take this so you
can see it. These are emissions spectrum. Again, Hydrogen and
helium and calcium and magnesium and potassium. They all have

(14:08):
a specific place in the spectrum that they show up oxygen,
you know, and so we would see them look like
a bright line spectrum. Okay, So you'll notice it's the
notice the line of sight thing. If you're looking at
the hot source and then you're looking at this cooler
gas to the right of it, right and the hot

(14:30):
sources behind it, you'll get the absorption spectrum. You see
dark lines, and if you actually look at the gas alone,
you'll see a mission spectrum, okay, and a mission spectra.
And you know this is something very very important, and
so yeah, ahead.

Speaker 4 (14:49):
So is that how you tell how you know what
you're looking at if you're looking at something in deep space,
if it comes back to a black line or a
colored line, can you tell if you flip it through gas.

Speaker 1 (15:02):
Or yes, that's a very good question, and let's do.
And let me show you another chart to show that. Okay,
when we look at stars, other stars elsewhere, well, what
we'll see at the same time is we're going to
see absorption lines from them too, because we're looking at
their stellar cores, which are in the middle, and they
have that outer shell of gas, and all that's coming

(15:24):
to us is the absorption spectra. So if you look here, okay,
you may recognize the letters on the left side. If
we rid of the numbers oh, be a go ahead,
says be a fine girl or guy kiss me. That's

(15:47):
what we learned when we were getting our astronomy degrees.
They and they said a tongue and cheek. It wasn't
actually something we had to memorize, but and within we did,
obviously because it was silly. Yeah. And so within each one,
within each one of the stellar spectra, like O stars
are the hottest in the bluest okay, and the B

(16:09):
stars are next, all right, the A stars are next,
and then of course F, G, K and M. All right. Well,
if you look each one of those, each one of
those letters has a uh A one through nine rating okay,
and zero through nine rating okay, So uh an O
one star would be literally probably one of the hottest

(16:32):
stars in the universe because those are the hottest and bluest,
and then an M nine star would be one of
the coolest and and dimmest stars in the universe. But
you'll notice the look at the look at the absorption
spectrum there right, yeah, those black vertical lines again, the
elements in the outer atmosphere of the star absorbing some

(16:56):
of the energy coming from the stars hot core and
as it passes through that relatively cool gas outside the core,
it steals some of the energy. And when it steals
some of the energy, it shows up in the spectrum
as a dark vertical line, and that's the absorption spectrum
because the elements, those atomic nuclei in the outer atmosphere

(17:20):
of the star are absorbing some of that energy. You'll
notice that we have in some of the red stars. Okay,
like right down here, you see the red star right there,
M two. Okay, the M two star. Look at all
the dark lines in there. But notice also, if you
look carefully, you can see that we also have we

(17:42):
also have titanium oxide TiO. That's a molecule, right, And
usually you don't get molecules in the outer atmosphere of
a star because the stars are extremely hot and they
is so high that the gas in the star is

(18:02):
almost always a plasma, except under certain conditions. All right, Now,
what's a plasma. A plasma is when let's say you
have a hydrogen atom. Okay, a hydrogen atom is a
proton and an electron, right, and that's all there is,
just a proton and electron. Okay, Okay, So a proton electron, well,
if you hit it with high energy. The proton gets

(18:26):
hit with high energy, the electron gets hit with high energy,
the electronic absorbs it and leaves the atom. It's called ionization,
and that ionization process will take the electron off the atom,
and now all its left is the proton running around, okay,
And the electrons are all freely running around around them
and everything. But the temperature is too high to allow

(18:46):
those electrons to come back in, so they just keep
going around and around and around and right, and they're
very yes, that's correct and so, and that's why if
you look at them just alone, that's why you would
see the emission spectrum down here at the bottom there. Okay,
you'd see in the mission spectrum, you'd see stuff characteristic

(19:07):
of hydrogen. You'd see stuff characteristic of other elements too. Okay. Now,
the thing is those protons running around with electrons zipping
all over the place. Those are free and the Sun
has this radiation pressure. It's pushing out, pushing out, pushing
out all this stuff, and it mobilizes these protons and

(19:27):
electrons to leave the Sun and race away, and they
race all out into space in all directions, and especially
when there's a solar flare. Okay. A solar flare is
a giant expulsion of the center b out into space,
and if it comes right at us, okay, we have
a couple of days and then we get hit with

(19:48):
many protons and electrons from the Sun and that's called
solar wind. And when you have a lot of it
coming at you at the same time, that's a coronal
mass ejection from a flare. So big flare shoots this
stuff off. And if we're in the position where we're
in the line of fire, well then we're gonna get

(20:09):
hit with all these highly charged particles member protons or
plus one charge, electrons are minus one charge. When they
leave the Sun, they stream at high speed to our planet.
I can't remember which equation that is in here, but
when they get here, they spiral around our poles, and
as they come down to our pole, they will interact

(20:30):
with our oxygen and nitrogen molecules in the atmosphere and
cause the Aurora Borealis the northern lights, and down the
south pole the Aurora Australis. So we have you've seen
many nights recently in the last few months where people
as far south as northern Mexico have seen auroras, right,

(20:55):
And that's because of the high amount of the protons
and electrons streaming off the Sun and hitting our planet, okay,
from a coronal mass ejection. We just were in the
fortunate position where we could get hit by it. Now,
if we get hit by a lot of it, that's
a lot of charge. And when it dives into the
ground after reaching you know, the poles dives into the ground,

(21:17):
travels through the bedrock, and especially in the northern hemisphere,
it travels through and because there's not a whole lot
of population in Antarctica, it doesn't really matter. But in
the northern hemisphere, we've got Europe, we've got the United States, okay,
and you know this is a problem. So once those

(21:37):
charge particles get into the bedrock, they travel and they
knock out electrical systems, They knock down power grids, okay sometimes,
and there was a famous one called the Carrington event,
which is really really really strong, powerful flare that led
to tremendous power outages. And I have seen full sky

(21:59):
auroras right here. I live in Connecticut, and on the
same night we had a full sky aur Just a
few months ago, I checked out our Sonoran sky to
a livestream telescope because I have an all skycam there
and it records all night long and makes a video
at the end of the night. And guess what I saw.
Aurora is dancing around in a northern horizon. It was

(22:20):
beautiful even from Arizona. So okay, So that's the charged
particles that are out in the Sun. Those are the
things that are responsible for absorbing energy, the different types
of elements in the outer atmosphere of the Sun that
give us the different absorption lines that we see. So

(22:40):
this all goes to say that, you know, if all
goes well, this is our telescope out there right now.
This telescope, we're going to add what's called a spectrograph
to the system, and that's going to be one that
will actually allow us to look at nebulae, supernova and
stars and be able to get these kinds of results

(23:04):
and see the different dark lines that are created by
different types of stars. And these are very instrumental. These
can actually help identify all kinds of things. You know,
we'd be able to identify, for instance, different types of
supernova and from a distant galaxies light we could look

(23:24):
at that and see what elements are present in its
spectrum and say, aha, that's a type one A supernova. Okay,
where you have a white dwarf sitting by a red
super giant and the white dwarf goes off under certain conditions,
that's a type one A supernova Roman numeral one I,
you know, a little A so type one A and

(23:47):
so I. We'll be able to identify that, and that
allows us to do some actually some very valuable confirmation stuff.
So that's kind of cool. You know. So that telescope
is up and running there, it is right there, well
you know, yeah, it's it's tall because I wanted to

(24:08):
be able to look, you know, close to the horizon.
As an astronomer, we don't ever look to the horizon.
We always look at an angle that's high enough because
we don't want to have to go through what's called
air mass. The amount of air between us and the
distant stars rises dramatically when you're starting to take into
account you're looking through the curve of the Earth. As

(24:29):
you're looking in the distance, so near the horizon, and
things you're always flickering. They're never really quite focused. But
there are some objects that I'd like to show people
because I'm an outreach astronomer. I want to show people's
stuff in the night sky, as you know, you know this,
and so I want to be able to show them
the really cool stuff that's out there, even if it's

(24:51):
not the best focus. You know, stuff I know that's
right now. As an example, I was doing some testing.
Actually this is from a live stream. Okay, all right,
we'll break down the stream screen. Here on the left
you see two of the galaxies in the Constellation of Leo.

(25:12):
Look at all the detail in those galaxies.

Speaker 5 (25:15):
This is.

Speaker 1 (25:18):
Just a twenty five second photo, Okay. On the right,
I have another application just sitting up there right now.
Normally I would show the galaxies full screen so people
can see all the wonderful details, but this gives an
illustration of what's going on at all times. On the right,
that's a guiding program that we use, and those you

(25:39):
can see on the far right there there's a little
gray square with a white fuzzy thing in the middle.
That's a star image, and we're guiding on that star image,
and so we aren't the telescope as we have it
automatically guiding and it works very well, and so we
stack images right and so this image here that you

(26:03):
see in the image photo, that's twenty two images that
have been laid on top of each other. Okay, and
those images that are stacked like that, what happens is
when you stack images on top of each other, the
individual noise from each frame gets averaged out over many,
many stacks of images. And so we create these these

(26:26):
dynamic stacks, and then those are the pictures we make
available to folks. If they want a highly developed one,
a highly specialized one, one that really really literally looks good, well,
then you can join our patreon. Yeah, yeah, join our patreon. Yeah,

(26:48):
do it. No, And if you're at no, yeah, yeah.
So there's a lot going on now as far as
the other stuff that's up on that mountain. When I
showed you this picture here, Okay, to the left of
that dome, you can kind of see another building there. Okay,

(27:12):
it's a little bit to the left. It gets kind
of right. You can kind of see the top of
it kind of over there. You know, Okay that that
building has about thirty telescopes in it, and it's a
gigantic roll off roof thirty by thirty size, you know,
foot building, and the whole roof rolls right off, exposing

(27:34):
all these telescopes. But the telescopes are just you can't
even walk through there, it's so it's so cluttered. But
the telescopes are all facing you know, specific directions, and
they don't move. Now, what would be valuable? What would
be valuable about that? Okay? Well, the answer is actually

(27:58):
something that if you think about it, it'll make sense,
and that is that we have special types of satellites.
You know, we know about different types of satellites. We
have satellites at orbit. You can see them move through
the sky. Okay, every night at sunset you can see many,
many satellites, including the International Space Station. We also have

(28:21):
satellites that are stationary over one point on the Earth
at all times. Those are called geostationary satellites or geo
geosynchronous geostationary not quite the same thing, but they basically
mean that the the geostationaries are the ones that are

(28:42):
over one point on the Earth at all times. Okay,
And those are twenty two thousand and five hundred miles
up in altitude. That's where they are in their orbit.
Why that far out? Well, you look twenty two thousand miles.
The reason for that is when you look at a

(29:04):
satellite going over, you see it move right, and then
it fades out right, International Space Station bright yellow, Then
it fades out, okay, starlink Sometimes in trains of twenty
or thirty or more, Okay, then they fade out. Well.
The reason is because they're in lower orbits. And when

(29:24):
you're in a lower orbit of only a few hundred miles,
then you have to orbit faster to stay in that
perfect circle. Because an orbit is the exact combination of
just enough horizontal movement to counteract the pull of gravity
trying to pull you down. And if you do that
all the way around the planet, you can move in

(29:45):
a perfect circle around the planet. Okay, you're going this
way as quick as you're being pulled down by gravity,
so it balances you into a perfect circular orbit. So
the International Space Station is in a circular orbit, and
it's at an altitude of two hundred and fifty two
miles above our heads. Okay. Now, when the astronauts, or

(30:08):
when the astronauts Butching and Sunny were rescued the other day, okay,
it took the rescue ship seventeen hours to get to them.
Why they're only two hundred fifty two miles up. What's
that all about. Well, the problem is that once they
get into orbit, they have to reach the orbit of
the space station. Okay, then they have to start moving

(30:31):
toward the space station, and they do it slowly. So
the time it took to get up there was seventeen hours.
Can you imagine sitting in a chair for seventeen hours?

Speaker 4 (30:42):
Oh? Probably not no, but if you're in space, I
would do it.

Speaker 1 (30:46):
Ah, And what is it about space that would make
it less of a problem on your on your buns.

Speaker 4 (30:52):
There's no gravity.

Speaker 1 (30:53):
Yeah, you're not feeling you're not you're weightless, so to speak.
You're in micro gravity, so you don't you're just sort
of like, you know, that's probably. Hey, this is really enjoyable,
you know, so it's a little bit more fun and
not as stressful and taxing on the body and just
sitting still in a chair. So it's easier to sit

(31:14):
still in space, you know. In fact, they encourage you
to sit still. You know, when you sleep, people put
your hands run don't run, Well, yeah, they they don't
run in space, that's right, because you're gonna go like this. Uh,
but they put these elastic bands on you so you

(31:34):
can run like you're jogging on a treadmill, and as
you jump, they pull you back down and they simulate gravity.
So the astronauts have to do an hour a day
up in space to keep their muscles active. Otherwise when
they get back down here, they'll be blobs because being
out of gravity for a while makes you really weak.

Speaker 4 (31:56):
You know, their eight day mission and all the time,
how weak they must have been because it does not
be planned.

Speaker 1 (32:05):
No, they weren't planning nine months. Yeah. So the thing is,
you know, people say, well, why wouldn't they brought home earlier? Well,
here's the problem with that. They were part of the
Boeing Corporation's star Liner program. The Boeing star Liner system

(32:25):
has different types of space suits than the SpaceX Dragon
systems have. Why didn't they communicate? I don't know. I
think everybody's trying to carve out their own little piece
of space. Okay, But the bottom line is that they
couldn't just fly back in a Dragon capsule, which there's
one dock on the space station. Why couln't they just

(32:46):
get in and go home? Because they have to be
in space suits on the way back. They have to
plug in, they have to do all the things they
have to do. They couldn't do it in the Boeing,
I'm sorry, in the Dragon capsule because they didn't have
SpaceX spacesuits, which cost, by the way, custom made for
each astronaut twelve million dollars a piece. So this last

(33:11):
mission to the space station delivered Butch a SpaceX space suit,
and Sunita was able to wear one of the other
SpaceX suits because she managed to fit into it. Probably
not the most comfortable because it wasn't tailored to her exactly,
but she was close enough that it was okay for

(33:32):
the ride home. So technically she could have gone home earlier.
But Butch and Sunny repair and they were on the
same mission, so they went home together. So interestingly, so
when people say, wow, they could have come home any time, No,
they couldn't have. They couldn't have because they didn't have
the space suits to ride in the Dragon capsules. This

(33:54):
is a call for me to generalize and make a
uniform code of spacesuit constructions so that every everyone going
to space, Russians, Japanese, Israelis Okay, Indians, Americans all right,
and of course, anyone else will will have a spacesuit

(34:17):
that is the same type of generic construction instead of
having all these trademarked and copyrighted and patented, you know,
outlets and connectors and I'll never no, forget that, just
make it one generic thing.

Speaker 4 (34:33):
Well, then in the movies Mark normally they have like
five or six spacesuits just hanging right here in the closet.
I didn't know what the problem was.

Speaker 1 (34:41):
I know, at twelve million dollars apiece, they didn't have
a few, they didn't have that many extras. They had
one extra and that was for someone that was on
the station, but that person was going to be staying.
So the next Dragon mission will bring up yet another
one for that person. Twelve million dollars apiece, spunk, that's ridiculous, right,

(35:02):
that's a lot of money. So clearly, you know, so
now you get a little better picture, right, you know,
that's something that's something that's unfortunate. Right now, we'll standardize
at some point, I guarantee it, and then in fact,
this probably would, this incident probably will make it so

(35:23):
it happens. So that's pretty cool. So but from here
on earth, you know, we we can only look up
through the atmosphere, and it's interesting. You know. I used
to work with the late great Douglas Trumbull, Okay, the
guy that did Blade Runner, Star Trek, the motion picture
you know, Closing Concerts is the Third Kind two thousand

(35:48):
and one, a Space Odyssey, and Doug and I were
very good friends, and one of the things that he
wanted to do was create three D movies, and so
he started, you know, we actually put the other technology.
I worked with him, not as you know, I was
an underling, just doing yes, sir, whatever you need, sir
kind of thing. But he created this beautiful three D

(36:10):
video from on board the ISS, and when you look
at the screen and you see things within three D,
it's a very different understanding, a very different feel, a
very different visceral connection. Okay, So we're looking out of
the cupola on the ISS, which is that nice paneled

(36:31):
window setting. You look out and there's a soy Us
capsule hanging right nearby, and you can see it there,
and we're going in orbit around the Earth. The Earth
is going by going by. You see thunderstorms, you see auroras, Okay,
but you're seeing him in three D. You're seeing that
auroras aren't just flat light to the sky. They're billowing
bands that have depth and height. Oh, incredible stuff. And

(36:56):
this this is something that all astronauts feel when they
look down at the Earth from above like that. It's
called the overview effect. And for those of you watching
watch and look up the overview effect, you'll find Doug's
name in there because he took part in this. And
the overview effect is why when astronauts come back in

(37:18):
nearly all cases, they come back saying, what are we
fighting for? And why we have such differences? When you
see the Earth from space, there's no borders, there's no walls.
You know, it's really just a beautiful, impressive ball of blue,
you know, yeah, yeah, And then you look at the
height of the atmosphere is like one hundred miles maybe

(37:40):
getting just about. When the sun's very active, it gets
a little thicker. When it's not, it's get a little
less thick. But you know, up there, we look at
contrails in the sky from down here, right, but from
up in the space station, you're looking at contrails effectively
two hundred and fifty miles away. So there the tiniest
white line and you don't even see them, and then

(38:02):
they could be covering your skies. But from the space
station you can't really see them unless they broaden out
into clouds. Okay, over time, which happens. You know. It's
part of the contrail science that a lot of the
chemtrail people would rather not have to pay attention to.
It's an inconvenient truth for them. So it's just so

(38:25):
interesting how this all works. In the view fromp space.
When you look down from above, it changes your perspective,
you know. And even though I've never been up there,
I want to. Yes, they would do. Yeah, you go
too if I can think of, I'll save you a
seat on the Dragon capsule.

Speaker 4 (38:44):
Okay.

Speaker 1 (38:47):
The nice thing is, you know, if you think about
the genius of Elon Musk, he actually he's created a
fully automated system. When Sunita and Butch got in that
capsule to come home, it was automated. It came home
all by itself. They just said to sit there and go, wow,
look at the view. You know, if you remember the

(39:08):
Apollo era, the the button panels on the Apollos, all
these flip switches, push buttons, covered switches do not press
I mean, all these different things that could go wrong,
and a gimbal joystick that you could hold with the
gloves on. Oh, there's actually a game out there that

(39:28):
is you have to learn how to use that, and
it's sort of like a it's like a re entry
game where you actually re enter in the Apollo capsule
of that era. And it's like only someone who wants
to punish themselves trying to actually learn this stuff would
actually be successful at it. I'd burn up every time. Okay,

(39:49):
I haven't tried it, and I don't want to because
that's not interesting to me.

Speaker 4 (39:52):
Well, even if you sturvey, it looks like you burn up.
I saw how scorched that capsule was. That's correct.

Speaker 1 (40:00):
I remember they're going from there. They're going from seventeen thousand,
five hundred miles an hour. And what they do is
when they separate from the space station. Okay, they're going
seventeen thousand, five hundred miles an hour, they hit thrusters
okay to slow them down in their orbit, and they're
automatically going to start dropping. Okay, because at a different altitude,

(40:21):
your orbits are different speeds. So when I was talking
about the geostationary satellites. The farther out you go, the
slower the satellites have to go to stay in that circle. Okay,
because Grabby's a little weaker. So if you're nearer the Earth,
you got to go faster so that you know, for
all your horizontal motion, gravity's pulling down a little stronger.

(40:42):
You got to go faster to stay in that circle.
The station, with its very gossamer solar panels, is moving
over seventeen thousand miles an hour. Right, that's really fast
and people can't comprehend that sometimes still, right, because you're
moving at the same speed when you're up there. Yeah,
So as you undock, okay, if you do a burn

(41:04):
with your retros to slow down your forward motion, you're
just gonna start dropping because gravity's gonna start pulling you.
And now you're going to enter a gradual lower orbit.
Lower over the station's gonna be going away from you,
over your head, and you're eventually when they time it
just right, a certain amount of seconds, a certain attitude,
a certain amount of burns, a certain amount of another orientation,

(41:27):
and you'll end up coming back to Earth exactly where
you want on the planet Earth. And they calculate with
the selest mechanics, they calculate exactly where that is. So
they go around the Earth a few more times, getting
lower and lower, until finally, as they start to hit
more and more atmosphere, they started to they turn the
capsule backwards because the heat shields back here and it

(41:49):
can go backwards into the atmosphere and it blats, you know,
and it blades all that stuff, so that the capsule
is protected as it's coming back into the atmosphere. You
like that. That's kind of a great visual. This is
my flames, okay, and the capsule is protected, but it
has a heat shield on it, so it's protected. You know. Yeah,

(42:09):
I know that there have been accidents. The Soviets had
accidents where one of their Soyer's capsules h didn't come
back in, didn't orient right, and this this high temperature
of over thirty five hundred degrees fahrenheit, burned through the
capsule and killed the cosmonauts. Okay, now that's and it
landed fine, and when they opened it up they were

(42:30):
met with a horror scene. So that that happens one time,
and then you fixed that. You know. There was one
of the case where the capsule was compromised and all
the air was taken out way up in orbit, and
the single cosmonaut there was a h I don't remember.
I think it was a guy Kmarov. Okay, he ended

(42:54):
up getting killed and all that was left for him
was a little tiny, crispy critter unfortunately. Yeah, so heat
shield failure is a big, big thing. So obviously in
space is dangerous, and astronauts the most dangerous occupation there is,
you know, And there's there's a few things if people

(43:17):
want to try it. There's a few things people can
do to enjoy the potential for to enjoy the potential
for going to space. And we'll come back to the
subject matter in a minute. But just a little further aside,

(43:38):
there's an aircraft called the Vomit Comet. Now it's given
that name because it's an old aircraft and they've gutted
the interior, put padding the whole length of the tube
and you go in, you lay down on your back,
it takes off, goes up with this sky. It's climbing
like this, okay, for a long long time. Then as

(43:59):
it gets to us certain point, it goes over the
top of a parabola. You know, remember the geometry shape
of a parabola goes over the top. As it does that,
you rise up off the floor because now you're feeling
micro gravity for the first time. It's that feeling you
get when you go over the top of a roller
coaster hill just as you drop that oh your stomach.

(44:21):
That's how they feel all the time, and that's why
some astronauts can't can't acclimate to that. That's scary, isn't it.
So I give it a shot, a shot.

Speaker 4 (44:37):
I thought. Rides the zipper, you know, that'll ride the
zipper a few times. That'll get to set for space.

Speaker 1 (44:46):
Yeah. The vomit comet though, was cool because they do
that arc and it lasts about fourteen to twenty seconds
when they do that arc, so you're floating around. Oh
I'm weightless as well, okay, And in that moment you
feel like the astronauts do all the time. And then
they tell you, Okay, we're coming out of it, and

(45:07):
you're going to get back down to the ground and
lay back down, and then you feel the weight again.
You wait again as they come out of the bottom,
and then they turn they go do it again thirteen
or fourteen more times. So if you get sick on
the first one, you're out of luck for the rest
of the flight.

Speaker 4 (45:25):
With you.

Speaker 1 (45:27):
Yeah, there's about twenty five or so people that get
to go at a time, maybe fifteen, I forget the number.
But you're flying a whole jet for just fifteen or
so people. So it's not cheap. It literally costs you
between ten and eighteen thousand dollars to go for this ride.

(45:48):
So it's really only for the rich or for companies
that want to get rid of certain employees. You know,
i'd you know, I'm done. Yeah, it's pretty neat and yeah,
but so I did want to talk about the fact
that Sunny and Butcher made it back. Fine, you know

(46:10):
when you think about it, Okay, that fiery passes through
the atmosphere, you know, Okay, as they're coming back into
the atmosphere like that. Okay, that heat shield is what
protects them, as they said, but it's also that that
is air thicker and thicker and thicker atmosphere. So when
they're in the spacecraft, they go from being weightless to

(46:32):
now feeling you know, the ability of gravity to affect them.
And as they're getting closer and closer to the Earth
and going through this, they're slowing down. As they slow down,
gravity is getting stronger and stronger. So by the time
they're hanging under the drogue shoes, the ones that come
out initially they just kind of trail up above them
all are dropping. Okay, they're they're feeling gravity again. You know,

(46:57):
to some extent that when the full mains come out,
the main parachus is four big ones. They come out
and they stay kind of vertical for a while, and
that's called reefing. They have them reef because if they
opened up wide right away, they could be shattered, because
that's a problem with the They're still moving pretty fast, right,

(47:18):
so they reef like this for a while. Okay, catch
some air, and they're designed to open up more and
more and more as they slow down. So once they
slow down, all four of them come out, and now
the people in the in the in the seats in
there are going, holy cow, man, I'm happy again now
feeling the way. So it's pretty interesting how that works.

(47:40):
So you know, there's a lot. So that's the effort
it takes for us to get off the planet, right now,
you know, that's the effort. And I know that you
know we've We've got another hour in a bit here
to talk about the other main topic. But I did
want to put it up to see if you had

(48:01):
any questions about this as well, because I know we
also have people watching in the chat. I'd like to
find out if they've got anything they'd like to share.
Are any questions?

Speaker 4 (48:12):
I got a question on like the space thing, how
they first sanded up there. You know they mister can
for eight days. I know that there's a lot of
redundancy on space capsules or space ships and yems and stuff.
So what I mean, how do they plan for like

(48:32):
medical things, if someone had paike like pyroid neds every
day or something. Do they plan in advance in case
something like this happens? Or is it just the supply
mission you're just at the Mercy.

Speaker 1 (48:45):
Well that's the thing, Okay, resupply missions resupply some obviously
essentials food that they can't replace. Now, this is going
to turn off a few people, but when you go
to the bathroom on the space station number one, okay,
that's recycled and you drink it, yeah, oh yeah, And

(49:09):
that recycled urine is the best water on the whole
planet because it's so crisp and clear and clean. You know,
once you filter everything out of it and chill it,
you probably would think you're drinking a really nice bottle
of a very high quality water, you know. So yeah,

(49:31):
it's really uh yeah, a mountain stream, all right, it's
my altitude stream that becomes drinking water. And you know,
things like that you get over, I think, really quickly,
because you know, you realize that if you don't drink it,
you die, you know, so it's very important to do that,
you know. I know that that. That's one thing. Now

(49:56):
the other well, the bathrooms are very specialized up there,
but keep in mind that the astronauts travel in a
microgravity environment, so they just kind of float through. So
you can imagine that if you kind of went to
the bathroom, it's gonna go, you know. And when water
is set free up there, it tends to form little
globs round balls, okay, And it's really weird how it operates.

(50:22):
I remember watching one astronaut took a GoPro camera and
a big ball of water and he pushed the GoPro
into the water inside the spacecraft, inside one of the habitats,
and it just sat there floating, and the view from
inside is like you're looking through the water at him.

(50:42):
It was the coolest thing, but it pointed out how
water operates. Now, water operates and water molecules operate using
the surface tension. Okay, the minimal minimal area, yeah okay.
And so it means that the shape that would be

(51:05):
generated by a water drop in space would be the
least uh, it would require the least amount of energy
to maintain. And that's a sphere. That's why planets are spheres. Okay,
that's why Earth is a sphere and not flat. Okay,
you know it's not flat. Yeah, you know. We have

(51:27):
a break coming up, don't.

Speaker 4 (51:28):
We We have in six minutes.

Speaker 1 (51:31):
Oh good. Okay, So when we when we talk about
we talk about like water and space and everything. So
when you actually go to the bathroom in space, you
can't just like here, stand in front of a toilet
and go boom and aim it because those drops would
splash off of things and get airborne and just float around.
The go in your eye, the go in your ear.

(51:53):
It's just not any fun, right, Yeah. They do. They
have these special vacuum hoses and things, and you actually
use those for both ends. And there's special capabilities that
you you and special instruments that you use in order
to do that. On a space shuttle, it was a

(52:16):
I have a Space Shuttle manual here, and the number
of steps to use the Space Shuttle toilet. It's about
seventy five steps to go to the bathroom on the
By that time you've gone in your pants.

Speaker 4 (52:27):
I'm telling you ahead, that's the thing.

Speaker 1 (52:31):
Practice thanks, perfect practice practice. Yeah. I think I would
drink at all. It's like, oh, drink this all now. Yeah.
So that's the kind of thing that's fun, right about
the whole traveling through space. Now, I saw a few

(52:51):
questions out there. I know that somebody asked. I think
it was Donald Kunzer. Did he ask about in Mariann's
here too, by the way, Yeah, I think he asked
about radio telescopes. We don't have any radio telescopes out
in space. The James Web is looking at infrared energy, okay,

(53:14):
But radio waves are out in that far spectrum okay,
and the James Web see is far out there okay.
But radio waves we can use here on Earth because
we can capture the radio waves reaching us from space. Okay,
So we don't need to put a radio telescope out
in space. But in fact it was that large collection

(53:39):
of radio telescopes all over the planet Okay, as a
planet orbits and rotates, right as a planet revolves, we
had these telescopes at various points of the planet, all
looking at a particular location as the Earth was rotating.
And that particular location was the center of a galaxy

(54:00):
called Measure eighty seven. It was where they saw a
black hole in the center. And the thing is, it's
so far away that to have a telescope with the
kind of resolution you need to see something that small
from tens of millions of light years away means the
telescope has to be a big diameter. So what they

(54:22):
did was very cleverly used the diameter of the Earth okay,
eight thousand miles with telescopes at various places on the Earth,
including Antarctica down there out of the view, and they
looked at this object that's Earth rotated. As it's rotating,
they're seeing it as they're rotating. There they're watching the
same object the whole time, so they're catching all this imagery.

(54:43):
So now we have this one swath of data for
this latitude, one swath of data for this latitude, one
swath of the data for this latitude, et cetera, et cetera,
et cetera. Added together, we get a very rough eight
thousand mile diameter set of observas. Okay, repeat that often
enough and now you get a much higher data set

(55:06):
accuracy with higher resolution. And this is how we were
able to resolve seeing something forty plus million light years
away out in the middle of out in space. I
thought that was pretty cool. And they've done it with
the black hole the center of our own galaxy, which
is about thirty three thousand light years away. You know,

(55:29):
so clearly that kind of thing is something that is
really good for us to do, right, So we can
do that from the Earth. See, we can do that
radio stuff from the Earth, but from but if we
have to do anything else, we want to look with
telescopes like our sky tour telescopes or you know, earth

(55:52):
based telescopes. You'll notice they're all on high mountains, okay,
and the high mountains mean less atmosphere through Okay, the
atmosphere is about one hundred miles thick, but it gets
drastically thinner, and by the time you reach about twenty
five thousand feet you're above about half all the year
on the Earth, So if you get up to like

(56:14):
seven or thirteen thousand, you're actually making quite a stab there,
you know. So out at Monakea in Hawaii, they're at
thirteen thousand, seven hundred feet, Okay, people that go there
for the first time sometimes need supplemental oxygen. I rode
in an Army aircraft as a photographer for an air show.

(56:38):
I mean, I wasn't in the Army, but I could
ride with the team, the skydiving team, and We're at
twelve thousand feet and doing all these really white, wicked turns,
and of course I got air sick on the way down,
but I didn't do anything. It just got queasy. But
from that altitude, it was we're going two hundred and

(56:59):
thirty nine, you know, just so obviously pretty.

Speaker 4 (57:02):
Fast, fast and debris.

Speaker 1 (57:05):
Yeah, we're going fast. Yeah. But then the temperature where
I was sitting was like below zero because the wind chill,
but it was eighty five degrees in the ground. So yeah. Yeah.
So anyway, the point being that, you know, from that altitude, okay,
you the atmosphere was thinner, and I could feel myself

(57:27):
feeling lightheaded. Yeah, I think we have to pick this
up on the other side.

Speaker 4 (57:33):
Now, let's do it. I'm interested, so.

Speaker 1 (57:36):
Cool, Okay, all right, guys, Well we'll be right back, yeah,
right after well these words.

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Speaker 3 (59:23):
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Speaker 1 (01:01:17):
Hey, welcome back everybody. Yeah, so, yeah, I misunderstood a
question in the chat. I think the question was are
there any radio telescopes in Benson at that site? And
the answer is no, there's not. Yeah, it's yeah, yeah,

(01:01:39):
it's an optical observatory location, you know, but it's nice.
The altitude, by the way, is thirty six hundred feet,
which is double what we are in the Sonoran Desert
west of Phoenix. With sky through one that's like nineteen
hundred eighteen hundred feet or so. But you know, still

(01:02:02):
not bad. I've noticed some significant differences in the night
sky during the summer in Benson than in Wickenberg. It's
actually that extra bit of altitude, wow, a lot of
air below us, so at least enough so that you
can see more detail in the Milky Way than I've
ever seen. Yeah, yeah, yeah, yeah. So in any case,

(01:02:30):
I was going to take us on a path of
looking at planets around other stars and kind of get
an idea of the kind of things we've done with
all of our technology where we can barely leave the Earth.
But I wanted to do one last thing, and that
is to talk about a potential problem for us if

(01:02:50):
we put too many satellites into space. Now, yes, we
have Musk putting up the Starlink satellites, okay, but it's
sort of like a mixed bag for me because our
telescope out and the Sonora runs from starlink. We actually

(01:03:10):
have our Internet due to Starlink, And as it turns out,
our Benson location is probably gonna need Starlink too, because
when you have ten or twelve astronomers on the mountain
all using their stuff at the same time, the Internet
is slowed down and that's not good. So we may

(01:03:33):
put up a private Internet network up there through starlink.
I don't want to, but we might have to. And
I did want to answer this question from Karen. Does
the VLA Well, she means is the VLA still running
radio telescopes just a very large array, And the answer

(01:03:56):
is yes, yeah, and so yeah, that is that's something
that is going on now, there's something like twenty two
to twenty four radio dishes that are on the plane
out there, the Sant Augustine plane. I've been there.

Speaker 4 (01:04:15):
I was there.

Speaker 1 (01:04:18):
And with my producer Bill from our show, he was
previous producer. He's been there. And these are these big
eighty foot diameter radio dishes, but they're on tracks that
can be they can move and be moved around. So
if they move closer, they have a different resolution when
they moved farther apart, and so if you want to

(01:04:41):
see detailed things, you change the orientation of these dishes.
And so it's a variable radio telescope, which is kind
of cool, really neat variable, you know, so kind of neat.
So yeah, So the VLA is the of doing things

(01:05:02):
and so, uh, they there's a maintenance shed when you
first get there. Uh off the visitors center there's a
large shed and it's open at one end, and nine
times out of ten there's a satellite dictionary being maintained
and going through maintenance. And it's aferent diameter dish. So

(01:05:22):
you can imagine now, if you go for the tour,
you actually climb up the ladders and go onto one
of the dishes. So you can actually see, you know,
from that perspective what it's like, you know, really kind
of cool. But that make a cool photo, you know.

Speaker 5 (01:05:37):
Oh it sounds great? Yeah, great, exactly mm hmm next
next year, yeah.

Speaker 1 (01:05:49):
I So, I wanted to add something up here. This
is this is right. Here is an exo planet presentation
that I prepared for everybody. And we won't get through
all of it, but that's okay. I'm just trying to.
I want to point out some of the most important parts,
right and that the bottom line is if anyone has questions,

(01:06:12):
feel free. You know how I run skyter live stream, Well,
Skyter Radio is the same way. If you got a question,
put it up there and I will make sure that
we answer it. So and the same goes for you too,
down there, Terra, you could be up here too. You
don't have to be down there, you know. So yeah,
so we talk about extra planets. One of the things

(01:06:33):
that's important is, you know, why are we why do
we look for these extra planets? Right? Well, the idea
is that we want to find out if we're still
if we're alone, and you know, is there life beyond
us here? You know? And the most important thing is
we're searching for life that's carbon based, right, and that

(01:06:54):
means by definition, we're going to be finding earthlike worlds, right, okay,
because you know, the question is what might they look
like otherwise? And that's a question we'll answer a little while.
But think about this, we're carbon based life forms. Carbon

(01:07:15):
is the fourth most abundant element in the entire universe.
The third most abundant one oxygen, second helium, and the
most abundant one is hydrogen. Yeah, you got it. And
so with that abundance out there, it stands the reason
that the carbon, which is extremely flexible, I mean, carbon

(01:07:40):
can make bonds with and break bonds with more things,
millions upon millions of things, more than any other element
in the periodic table. So it stands the reason that
life is going to be based on carbon right now. Yeah,
it made the carbon bigot. I agree. Okay, So I

(01:08:01):
guess that means that being a carbon bigot, it just
recognizes the importance of carbon and the universe. Okay. Now,
when we look at the prospect of intelligent life finding us, well,
Stephen Hawking once said we should keep our heads down,
don't you know, stay below the radar, you know, over there,

(01:08:24):
stay down here, hide, okay, peak out once in a while. Okay,
that's what that's what you know, Stephen Hockey would like
to have us do. Remember this, we've already been out
there and we weren't given in control of it. Because
if you have a carbon based life form on a planet,

(01:08:44):
what's something that all carbon based life forms require.

Speaker 4 (01:08:49):
Water? Oxygen?

Speaker 1 (01:08:51):
Exactly that water and oxygen, and we have copious amounts
of both and have had for long before there was
life on our planet. Okay, that's nice to say intelligent
life on our planet. Right, So it was back oh gosh,
we're talking about two point four billion with a b

(01:09:14):
billion years ago, brillion years ago. Yes, that's when there
was something called the Great Oxidation Event, the GOE. That
meant that at that time, suddenly, and I do mean suddenly,
over a few several hundred thousand years, the amount of

(01:09:35):
oxygen in our atmosphere skyrocketed. Now that from an atmosphere
that was of a basement levels of methane, carbon monoxide
CO two, ammonia all right and so forth, and hydrogen. Okay,

(01:09:57):
that suddenly we had oxygen, diatomic oxygen two oxygen atoms
together the breathable kind that we used. And why is that? Well,
because early in our life here on Earth, I mean,
if you look at the picture here, what do you see.

(01:10:18):
Do you see a continent.

Speaker 4 (01:10:20):
Green primordial soup?

Speaker 1 (01:10:23):
Yeah, you see basically a greenish blue, right, you see
the clouds, and then you see what looks like ocean. Right,
So basically it was a water filled planet. And so
this water filled planet with the appearance of continents that
came later, was already starting to pump oxygen into the
atmosphere and we weren't even here yet, you know. So

(01:10:45):
there's a lot of things that happened at that time.
But one of the things that happened too was these
carbon based life forms that we have here depend on
a bunch of things. They depend on things like complex hydrocarbons,
carbon based compounds, and amino acids. Right, so we have

(01:11:09):
the basic building blocks of DNA, right site seeing guanine, thiamine,
and adnine. Okay, those are the four basic nucleotides. Okay,
well those were those were here. Some were delivered to
the Earth through comets and meteors, and as it turns out,
they're thinking that maybe comets weren't the primary provider of

(01:11:32):
water to the planet because they're made of ice, right,
so you figure out maybe a lot of them destruct
the Earth. Sure, No, Actually there was a lot of
asteroids to destruct the Earth too, that had, you know,
proportionally more water than tiny comets would. So the asteroids
actually probably did that job, you know what I mean.

(01:11:52):
Terror Yeah, yeah.

Speaker 4 (01:11:54):
Well there's so much water, I'm not in it all
the times it seems that there's more Earth. It's asteroids
that would It's incredible.

Speaker 1 (01:12:04):
Yeah, there had been a lot of asteroids struck and
and of course the Earth also made the building blocks
that we benefit from too, and that's what's interesting. So, okay,
this is all true. A lot of the building blocks
were delivered by other sources meteors, asteroids, comets, okay, and
the Earth made some of itself, and and so the

(01:12:24):
way the Earth made them. Just as an example of this
is Commet sixty seven p Tree mu Gersamenco, the Rosetta Mission.
That's a comet. That's what a comet looks like up close.
We landed on this comet, and the Rosetta Mission was
an orbiter that went around this comet took these photos. Okay,

(01:12:44):
the pile at landed. pH I l A E was
released from the orbiter went down and it was supposed
to latch onto you know, down here somewhere. It was
supposed to latch onto the ground where my cursor is
here you can see it, and had these little pins
that would fire into the ground to anchor it because
there's very little gravity on a comet, so if it

(01:13:06):
hit it would just go bring and bounce off, so
it had these little firing pins. Unfortunately, when it hit,
it fired the pins and that catapulted it off. So
it must have hit like a hard rock, you know,
underneath this icy mantle of stuff, and it sent it
bouncing up to fifteen times across the face of the
comet with very low gravity, totally out of control, and

(01:13:29):
it ended up landing in a fissure you and it
could be seen from the orbit of the Rosetta mission
a little bit, but not much. You know, it stuck
like in a fissure down there, you know, like down
in this region here it's sort of like a little
fissure which you can't really see. So maybe here kind
of like in this region a dark area, and so

(01:13:51):
you saw it in there briefly, but but Anyway, you
also noticed these things, these jets of gas right here.
See that that's two of them. Yes, there's actually several.
Notice that there's streams. Okay, yeah, and that's that's interesting
because what's happening is the comet sixty seven P was

(01:14:12):
getting closer to the sun. As it got closer to
the sun, it started to heat up. And when he
heated up, this this is dust on the comets surface,
acquired over billions and billions of years, Okay, because it's
been here for four point six billion years, and that's
this is how it looked, you know. And successive passages

(01:14:33):
by the sun melt melt the interior a bit, and
then there's gases trapped inside and it comes shooting out
in jets, which causes the comet to rotate it a
little funny sometimes, and so this trapped gas comes out.
Maybe there's carbon dioxide there, carbon monoxide, cyanogen, whatever, but

(01:14:54):
it was trapped in there, these molecules, and they come
shooting out at high speed and they can be photographed.

Speaker 4 (01:15:00):
You know, in that photograph, I see a horse's head.

Speaker 1 (01:15:06):
I see, Oh yeah, it's a whole body. In fact,
here's the horse's back end. Right here, and there's crows
sitting there pecking at his back end right here. Well
that's very good. Uh. And just for those that don't know,
she's an artist and the darn good one. Okay, so
you know she's she's the favorite go to artist for Skypter,

(01:15:31):
you know, as well as everything else does, which is phenomenal.
That does look like a horse, as you mentioned, does. Wow,
until you said that, I didn't even notice, right, you know, we.

Speaker 4 (01:15:43):
All see differently, and you know, yeah.

Speaker 1 (01:15:49):
So this being the closest view of a comment we've
really ever had. And more than half of this comment
is made up of carbon based molecules, organic molecules. So
you can see why comics delivering material to the Earth
was very important in our early formation. Okay. And then
meteorites also are very important. This one here is called

(01:16:13):
the Murchison meteorite. This one meteor it's one meteorite that
fell brought ninety different amino acids to this planet.

Speaker 4 (01:16:21):
Wow.

Speaker 1 (01:16:22):
Amino acids are the building blocks of life, Spock. They
are the building block. We have to bring these to
our planet, right, so's it, Mark, I don't know.

Speaker 4 (01:16:35):
Okay, amino acids.

Speaker 1 (01:16:38):
Yeah, yeah, yeah, So within some of these some of
these confines, there were ninety amino acids. Incredible, incredible. Now,
the Earth itself also was able to create these building
blocks of life as well. The whole point, if you
see where this is going, the building blocks of life

(01:17:00):
are brought to us from all over the universe for
many different means. And then the planet itself provided it's
in that not too hot, not too cold zone known
as the habitable zone, the Goldilock zone. Okay, we'll also provide.
And on our planet we had the luxury of having
liquid water on the surface. Now, liquid water can exist

(01:17:24):
on the Martian surface for a short time. As soon
as you pour it out of your jug, it'll go
down to the ground and go and in short order
it'll evaporate away and it'll actually supplimate away and go
directly from water to the vapor. Okay. The reason it

(01:17:46):
has to do with the pressure of the atmosphere. Okay,
Mars is sort of self regulating. Its pressure is just
below the pressure required to have liquid water on the surface.
And that's for another I've talked about this before, how
the pressure run Mars self regulates the state just below
that and it's not magic it's not some kind of conspiracy.

(01:18:10):
It's actually just the way the universe works. And it
has to do with something called a triple point of water.
All right, But back on Earth, Earth being more massive,
with enough of a substantial atmosphere, it was able to
retain the pressure with its gravity. It retained the atmosphere,

(01:18:32):
meaning the pressure of the atmosphere was high enough that
liquid water could exist in the surface. It wasn't always
the pressure we have now, which is fourteen point seven
pounds per square inch every square inch in your body.
You're getting fourteen point seven pounds of atmosphere all over
your head, all the way to space, pressing down on
that one square inch, and then you just add it

(01:18:54):
all up, so we have a lot of pressure. You
go into the ocean and you dive down to you know,
thirteen thousand feet like the depth of the Titanic, and
you're talking about six and six and a half tons
per square inch body. See, now, that's not just the
way to the water. That's the way of the atmosphere

(01:19:15):
over your head all the way to space as well,
plus the way to the water in that tiny little
square inch all the way down to the bottom. Okay,
added up your whole body and you're gonna get squished
out of existence right now, Actually, that's sort of not true.
Your body is mostly water, and water is effectively not compressible,

(01:19:39):
meaning that your eyes won't go and go away because
they're filled with water. The pressure is the same, right,
so the ocean water will be pressing on them, right,
and your eyes are used to pushing out at fourteen
point seven pounds per square inch. So with that kind
of pressure on your body, water's not compressible. So it's

(01:20:01):
not going to push the eye balls in, okay. But
what it will do is penetrate your sinuses and go
all the way and go in your ears, go probably
go past the ear drums into all the air filled spaces,
especially your lungs. Okay. So the Navy had the bright
idea of experimenting some years ago with a highly saturated

(01:20:23):
oxygen solution, and divers that tested it would have to
inhale this liquid, in other words, drown allow themselves to
be drowned, knowing full well that they're going to be
able to breathe on the other side of that, and
they would pump this high saturated liquid through their bodies

(01:20:45):
and that highly saturated liquid in their bodies would actually
allow them to gain the oxygen they require, and that's
the one stumbling block to diving deep in the ocean
as human beings. Right, So we could dive routinely, we'd
be able to dive to like three thousand feet by
breathing a solution and go open our air canals and

(01:21:08):
our ears and all that. And it was a program
that actually kind of worked. You've seen the movie The
Abyss where they dropped a little rat, yeah in that liquid, Well,
that was really done, and that was this highly saturated material.
So he didn't die, okay, because he was actually able
to breathe. But your diaframatic muscle that controls that can

(01:21:31):
breathe the air in and out, but it can't breathe
the liquid in and out, so it has to be assisted.
So they would have to pump it through, so they
had these big pumps. They tried it, and it worked,
but the only trouble was that divers that tried this
you can expect that not all the liquids are going
to come out of their lungs, So these divers would

(01:21:53):
end up, for the sake of the experiment, getting a
severe case of pneumonia, you know, fluid in a lunge
ungs and so they have to go through lengthy recoveries
if they survived at all. There's not a whole lot
of information on this out there, but it was something
that was done. So anyway, So pressure on the Earth

(01:22:14):
at the surface is fourteen point seven pounds per square inch,
and then the ocean, of course is deeper. But that's
that forty point seven pounds more than enough to have
liquid water on the surface. So what happened is and
the primordial Earth, we actually ended up with this incredible
little petri dish here on our planet. And it was

(01:22:37):
exactly it was a giant b burner, okay, and it
was it was the equivalent of this experiment we see
right here. This is the Milli array experiment on in
nineteen fifty two. And the mili array experiment was an
experimental set of it looks just like you see a
glass ball that had water in it. It had ammonia
in it NH three, it had methane H four, it

(01:23:00):
had diatomic hydrogen H two, and carbon monoxide COO. That
was the primordial atmosphere of the Earth, as we thought,
and still think it is probably likely. Right, There's been
changes in the formula here and there, but the bottom
line is that's that's kind of what it is. And
so on the right there, you see there's a heat source. Well,

(01:23:23):
think of that as simulating the water cycle on the planet.
The water's heated, it's turned into water, vapor goes all
the way up that right side, comes over the top
and drops down into this flask. Okay, and in that
flask there's a spark gap. So what's that simulating on

(01:23:44):
our planet? Thunder and lightning, Yes, exactly. Yeah, So this
was to test the Miliary experiment was meant to test
whether the Earth itself could create the building blocks of life.
And the result after a week was this brown sludge
on the bottom of that flask you see there at

(01:24:04):
the left. And that brown sludge turned out to be
a incredible amount of amino acids. Okay, building blocks of
life formed just through lightning action, as you see here
in this diagram. So when Stanley Miller died in two

(01:24:26):
thousand and seven, they found twenty more amino acids that
they never detected the first time.

Speaker 4 (01:24:33):
You know, are you seeing that original sealed bile?

Speaker 1 (01:24:37):
Yeah, that's right. They had the original sealed vials and
when they examined them again with better techniques, they had
missed twenty amino acids, so there was a lot. So
in other words, Earth creates its own amino acids required
as building blocks of life as well. And that's really
kind of cool, you know. I thought that was really
a neat thing. Now. Another odd of tea which I

(01:25:00):
think is interesting, is how we're constructed as carbon based creatures.
Think about it. Bilateral symmetry. Who knows what that is
out there? I think all of you do. Uh, were
the same on the right as the left for the
most part. Okay, And bilateral symmetry is potentially a product

(01:25:22):
of how DNA replicates. Now, we won't go into DNA replication.
I don't want to go through the biology with you
because I I guess that's not what this is about.
This has to stay fun. But but you know, you
know how DNA replicates because you're you're you're smart about
this too. Yeah, that's right. One half on zips and

(01:25:43):
another complementary symmetrical side zips in to form the new molecule. Well,
at the micro level, that's what's happening. At the macro level.
The body has imitated that too. So we have two eyes,
we have two are We are symmetrical left and right,
and it's possibly due to the way the base life

(01:26:05):
form that we are was created. Right now, that's that's
the thought process. Now, this is true in all higher
life forms. Now it's not true for every life form
because we also have radial symmetry. Okay, the internal arrangement
could be different. But the way the creature works with

(01:26:27):
the environment is through a symmetric mechanism. Okay, we have
one set of intestines, we have one heart. Okay, but
externally we interact through symmetry with our environment. Clever, clever design. Now,
But as I said, there is more than that. We

(01:26:48):
have radial symmetry. Consider a tulip or daisy, right, lots
of little petals all the way around. Okay. And starfish
are interesting. They are pentamerus. They are they're they're a
five sided I kind of I kind of dermata is
the name of them. And they're bilaterally symmetric as larmie
when they're when they're first born, and they look kind

(01:27:10):
of weird. They don't look like starfish at all. They
look like little suction cups. Okay, but then as time
moves on, they they become, uh, this this radially symmetric,
five sided creature, you know. So it's pentamerous panamerism. So
so bilateral symmetry is built into the nature of how

(01:27:34):
we were formed. That's really cool. So now the question is, Okay,
let's suppose there's life elsewhere. We all believe there is.
I do I actually think it made it here? What
does earth like mean? What does that mean? Well, obviously,

(01:27:56):
like I was an oxygen breathing creature, carbon based feature,
maybe bilaterally symmetric, right, something like that, right, yeah, yeah,
I would think. So, Okay, well, we know that for
earth like creatures to exist, they need to be in
the habitable zone of their star, the one I mentioned before,

(01:28:17):
where you're just far enough from the star that the
water isn't boiled off the surface like on Venus maybe
in its past, or frozen into hard as granite material
as on Mars right now, which is just at the
far end way out there, so kind of in that
not too hot, not too cold here, that's where we are, Okay,
that's the habitable zone, and liquid water has to be

(01:28:40):
able to form and stay on there. Why do we
say that because in all of our studies it looks
like life began in the water. We come from the water.
You know, how do you know you've come from the water.
There's a simple reason. We know that we were born
in the ocean.

Speaker 4 (01:29:01):
I guess is it our salinity? Is it our salt? Yes?

Speaker 1 (01:29:06):
Yeah, it's our salt content. Now, our salinity and our
skin is not nearly as high as the ocean. I
think we're like what three percent or something and the
ocean's higher. Well, the bottom line is that that salinity
is a vestige of vestigial remains, actually a vestigial remnant
of our salt, you know, dependence over the years. Now

(01:29:31):
why salt? There's a big reason for that, and I'll
tell you in a moment. But consider this. When we
finally climbed out of the water, we had to take
a shell of salt with us. Salt water, right, like
a turtle shell. So our skin is like a turtle
shell's it's made mostly of water, and it has a
salinity of a certain amount, like we talk, and so

(01:29:55):
we carry this vestigial remnant with us at all times
so we can exist out of the water. Oddly enough,
we've evolved so far out of the water that now
the water can kill us if we try to if
we go into that's all right, thanks a lot water. Okay, yeah,
So so the solidity is interesting, and our dependence on sodium,

(01:30:18):
which is worth the sodium chloride. A sodium atom and
a chlorine atom together make salt table salt NA sodium
cl chlorine. Okay, yes, I know sodium is doesn't it's
not enable. That's that's the elemental formula an A so
capital N LITTLEA and cl. All right, sodium chloride. Now,

(01:30:42):
why is that? Well, why is the water salty? As
a matter of fact, Now, that's that's a very interesting dependency.
We had. For the longest time, our atmosphere was ninety
times thicker than it is now. Venus atmosphere is ninety
times thicker than ours right now, but ours is much

(01:31:03):
thinner now. And the reason is because we're in that
habitable zone. So what could happen is we had a
rocky surface that had hardened early on, and it was
molten for a long time, and then it became hard
and rocky, and then because we're in we had a
thicker atmosphere here, unlike Venus, it could rain, and when

(01:31:26):
it started to rain, water would hit the land and
then run in little rivulets and make rivers, and finally
large rivers and gushing water falls and so forth into
low lying areas. Over time, over millions of years, that
became oceans. The thing that's interesting is when water runs
over rock, several things happen. First of all, sodium atoms

(01:31:49):
are easily dislodged from the rock strata, and so were
chlorine atoms. And the thing that's interesting is one of
the atoms has an extra electron, and the atoms needs
an electron. So when those sodium chlorine atoms get into
the water, they go boop and they connect to each other. Okay,

(01:32:10):
and that's sodium chloride, sodium chlorideventin, Hey, sodium chloride, and
now that sodium chloride now, and certain salinities, and there's
different types of salts as well. Based on the compounds
is what causes the oceans to be salty. And all

(01:32:31):
life forms in the ocean depend on sodium as a result,
and so do we. So our vest harvestigial sodium that
we have in our bodies is something that was a
holdover from our evolution out of the oceans. You know,
my shirt says, so I'm just kidding, right, So liquid
water was very very important. As they said, the other

(01:32:52):
thing that was really important is that the star isn't crazy,
that the star is not some wildcat that starts shooting
all kinds stuff as you know. Yeah, like ultraviolet radiation
to go, okay, you're all sterile, now, Okay, Ultraviolet radiation
does a number on water molecules in the atmosphere. Just

(01:33:13):
look at Mars. Okay, our magnetic field, which is another
fortunate you know, I say, contribution of the formation of
the Earth is that we have a molten a molten
outer core and a solid innercore. Well, they rotate against
each other and generate electric currents of very very high amounts.

(01:33:34):
Those electric currents in turn make magnetic fields, and we
have a magnetosphere, a giant magnetic field around our planet
as a result of that core down below. Now, Mars
also had one of these. Okay, Mars also had water
like we have, right, Mars had a thicker atmosphere. However,

(01:33:59):
Mars is a little small, and the electrical charge being
generated in its core waned over time because the Martian dynamo,
that is that that creates these electrical charges wasn't as
powerful as the Earth's, and over time it was able
to wane and go away. So when that happened, the

(01:34:22):
ultraviolet radiation from the Sun was no longer trapped out
by the atmosphere. Okay, the ultraviolet radiation was actually, you know,
able to penetrate the Martian atmosphere and the water vapor
molecules H two O molecules, and the atmosphere would be
struck by this ultraviolet radiation pow, and the hydrogen would

(01:34:44):
be separated from the oxygen. Okay. So you have two
hydrogen atoms free to go to space, oxygen atoms fall
down to the planet. Okay, And now you have this
disassociation of all the water molecules in the Martian atmosphere okay,
again far into the habitable zone there. And so now

(01:35:07):
with that disassociation of the molecules, they became H two
and zero. Right. So fast forward a billion years and
all the water on Mars is now evaporating and there's
no water cycle anymore. It doesn't rain back out, So
the water evaporates and goes away, evaporates and goes away.

(01:35:27):
Eventually you're left with a bone dry, sterile surface like
Mars is today. Surface. Notice I said surface, right, Okay,
so that's why. And the Martian top soil is irradiated
by ultraviolet radiation and it's just you know, there's nothing
that can grow there right now. But underneath the surface
dust layer is the water that froze. Because Mars had

(01:35:52):
copious water still does, okay, And the surface of the
surface water froze and got covered by dust. And once
that happened, as the Martian atmosphere thinned out, all right,
the pressure dropped, a lot of water sublimated, went away,
and much of it as it got colder, the water froze.
And now the water on Mars is as hard as granite. Okay.

(01:36:16):
There was a probe that landed in the northern plains
of Mars, and when it took a downward looking shot
where it was landed, the jet of the exhaust of
the landing landing jet displaced a lot of the soil.
And guess what you're looking at a twilight white ice

(01:36:37):
right below this lander. Yeah, very very cold, and so
you can see so Mars has a lot of water.

Speaker 4 (01:36:45):
Is it salty?

Speaker 1 (01:36:47):
Yes. As a matter of fact, the Martian water will
be salty for the same reason ours was. Okay, And
the thing that's interesting is it's a south pole of Mars,
like a kilometer below the surface, a surface I'm sorry,
an orbiting probe. I think it was Malan space sidence
systems of the Mars orbital camera. No, it was a

(01:37:08):
radar was able to detect water beneath the south pole
cap of Mars. Why water, I thought water wasn't there?
Mark what's going on? Because the weight of the strata
on top increases the pressure down below enough for liquid
water to exist deep underground. Yeah, an underwater reservoir or

(01:37:30):
aquifer or lake. Yeah. And that water down below is
miles long, and it most likely, as you just pointed out,
is very briny salty. See. So liquid water exists on
Mars too. It's just that it's locked up in a
different way right now. Because the Martian atmosphere thinned out.

(01:37:54):
Earth's atmosphere didn't thin out until it started raining, and
then it reached a level of equal liver where it
is now right, Venus was too hot, the water could
never form rain clouds and rain out, so it never
rained out. Okay, however it did because of the sulfur

(01:38:14):
content and so forth, it did go into making a
lot of sulfuric acid, and the clouds are riddled with it,
all right, So obviously habitable zone, liquid water, habitables, you know,
stable star system. Okay, our early sun was pretty energetic,
but it's sort of stabilized downbo. Actually it's really not

(01:38:35):
as kind to us. I know, where what we call
a habitable planet. I guess what, we're not super habitable.
There are planets out there that'll be much better for
us than this one, believe it or not. This one's
always trying to kill us. Volcanic eruptions, tornadoes, hurricanes, play tectonics,
making earthquakes. You know, Oh we're all gonna die. I

(01:38:58):
mean that kind of thing happening too.

Speaker 4 (01:39:01):
What did we expect that on a melt.

Speaker 1 (01:39:05):
Not necessarily a super habitable planet might not have the
same type of tectonic activity we have, and so it
might have a lot of water with a lot of
land masses, and they might be static, you know. And
there's actually some planets that seem to look like they
may be more super habitable. They're a little bigger than
the Earth, but so what you know, you think about

(01:39:28):
you know, planets that are like twice the size of
the Earth, and they call them super Earth. So it
doesn't mean they're actually large earths. That means they're just
just twice the size of the Earth. So they're kind
of a supersized earth like or rocky planet. It could
all be rocky, but if it looks like the Earth,
you might say, well, if that's twice the size, then
gravity can be pretty strong. How could those things survive?

(01:39:50):
How can anything survive? Go to our deep ocean. Right
on the bottom of the deepest parts of the ocean.
You got little fish swimming around right the sand. They're
down there, thirty thousand feet deep at the bottom where
Titanic is. It's not a dead zone. There's creatures down
there living in the deep sea, always in the perpetual darkness.

(01:40:12):
Bring them ups, bring them up to the surface, and
what happens to them?

Speaker 4 (01:40:17):
Don't they go inside out or something? I mean bodies
like distorted and stuff.

Speaker 1 (01:40:22):
Yeah. The if you bring them up and you bring
them up in a container that's like an open top
on it, okay, you actually find that they just go
and they just burst, And that's really terrible. So to
get a good sample, you got to keep them at
the same pressure down there, and to do that you

(01:40:44):
need a specialized set of containers. And so to do that,
the deep submercibals have these titanium canisters that can withstand
that pressure and it just fills with water, okay, under
the pressure that it's under, and it sucks up the
little creatures and when it gets to the surface, those

(01:41:05):
creatures are still intact. You know. Now if they opened
it and pour it out, it will do that, you know,
and that wouldn't be any fun. But so, you know,
other words, what I'm getting at is that creatures can
live in all different pressures. Even us. There's creatures that
might say, you have like almost fifteen pounds per square

(01:41:26):
inch in your body, how can you live well? Because
we're evolved that way and those creatures down there evolve
that way too. So that's how that works. You know,
if we get to Europa around Jupiter, right, you have
Io Europa, ganimating Calisto, the four you know, primary what
they call the Galilean moons of Jupiter. In our sky

(01:41:47):
tower telloscopes who always see Io Ganymede. I'm sorry, Io
Europa ganimede Chlysto. We always see those. Well, Europa has
this big ice sheath many tens of miles thick, and
then inside because of the constant gravitational you know, kneading
as in kinneating like kneading bread, okay, and squeezing and tugging,

(01:42:10):
the interior is very warm and all that ice is
melted and it's probably very briny salty. However, it turns
out also that that stuff in the middle right, it's
actually the two thousand mile diameter moon. So they're thinking,

(01:42:31):
holy cow, there might be life under that ice. I mean,
we have life in the dark here, don't we, right,
event yeah, that the geothermal events. In fact, finding life
for the geothermal events is why we started to think
that maybe there's life on Europa and even on Saturn's

(01:42:52):
three hundred mile diameter moon. Enceladness, which is a similar
situation in Seladness, actually has active geothe events that we
can see. So that's pretty cool, right, So does it
mean that life is guaranteed you No, of course, not
doesn't mean that it's possible. Absolutely, So even in our
solar system we might find extremophile life compared to us.

(01:43:15):
You know, life at the extreme, and that could be
us to another life form that's here from another star.
These human things are extremophiles. They live under this big,
thick atmosphere and not in not in space like us.
Oh how do they do it? Right? So a lot

(01:43:36):
of things, you know. So I've told you about the
habitable zone, and I told you about the liquid water,
and I told you about the stable star. You know.
So that's pretty cool, you know. Now, it's interesting to
notice that, you know, there's many different types of stars
out there. Right when I showed you before, I showed
you this one image for a couple images in a

(01:44:00):
our media here, and you saw the different spectra of
the different stars here. Okay, each star has different elements.
Those black lines mean different elements. And just out of curiosity,
you notice the third line down and says Alpha Lira.
That's Vega, the star Vega twenty six light years from us,

(01:44:22):
and it's an A zero and the V means that
it's a normal fusion hydrogen fusion star like our son.
Look at how thick those black lines are to the
left and heading out towards the center right of Alpha Era. Okay,
those it's well known that A type. Stars have the

(01:44:45):
brightest or the deepest. They call it lines of hydrogen.
That's the hydrogen Bamber series b A L M E R.
You have to remember that won't be on the test. Okay,
so the Bomber series, those bright lines are actually those
big lines. They A zero stars have the fattest lines,
and that's kind of important. And then we have as

(01:45:09):
you see next, you have Zeta Era that's in A four,
and that one actually has thinner lines. But notice that
it has more lines near the middle there in the
green right and then the red. Now what that means
is this star has more elements in its outer atmosphere

(01:45:30):
that are absorbing energy, right and and Vega. Well, it
doesn't have to mean that. It means that the star
was made with more elements when it was made that
were in the stellar nebula from which it was made,
and all those elements aren't doing fusion. The only thing

(01:45:54):
doing fusion is in the core, and we don't see
what that's doing. We only see what's in the out
an envelope of a star. The core is just it's
it's burning hydrogen into helium. Then if it gets hot enough,
it'll do helium into carbon, carbon into oxygen, oxygen into magnesium,
and and and more, and then finally it gets the

(01:46:15):
iron where it stops. But that's only for very very
massive stars. Okay. So the farther down this table, you
go from the O stars down to the M stars. Okay,
the cooler the star is, all right, the stars that
are really hot, And I guess I said it's this one.

(01:46:36):
This chart starts with a B star. But we did
look at you know, we did look at these guys here,
which shows the the O stars up there, okay, And
it goes right through bes of the different types and
you can see the literally this the lines. And if
you look at the A zero right here, Okay, that

(01:46:57):
A zero shows those really big dark line and you
see that those dominate the spectrum of those A stars. Okay,
so that's pretty cool. All right. So all that all
that stuff means is that there are certain stars that
are more conducive to life. Okay. So when we ask
the question if can they all support life? The answer

(01:47:18):
is no. Okay. On that upper left, that's the O
stars we talked about, brightest and bluest. Okay. Now there's
a snaky line. This this snaky line right here, see
my little cursor snaky line going right down there. This
is called the main sequence. You notice the sun is

(01:47:39):
in here too, right here, this main sequence, this is
the star. These are the stars that are actually all
they're doing in their cores for converting hydrogen into helium.
That's the main fusual, that's all they do right now. Okay,
all right, But when this o star stops fusing yogen

(01:48:00):
into helium, it may extend, it may expand, and if
it expands, it could end up expanding into a red
super giant. These are the post main sequence, that is,
the post hydrogen into helium burning phases for these stars,
so they can become giants based on what's happening. Stars

(01:48:24):
that are like this they're born that way, and when
they get born that way, they only live a few
million years and they go boom. So stars like that, okay,
and I mean boom super nova. Stars like that can't
support life, right And the reason is because they don't
live long enough. They don't last long enough. All right.

(01:48:45):
So you see there's that relationship between you know, the
color and the temperature of these stars, hottest and bluest, coolest,
the redst right now. It's also true that we can
kind of alkolate the brightest light that comes from a
star through this thing called Ween's law, and this is

(01:49:08):
you know, I won't get into Ween's law, but it
just means that we can calculate what we expect coming
from these stars, and what we'll find sometimes is that
much of the light from these blue stars comes from
the ultra violet side of the spectrum. What that means
is like with Mars, sterility, baby, Okay, those if there's

(01:49:31):
any planets at all, they are probably going to be
sterile rocks. Okay, so that's what's important there. Now. The
consensus is that stars from about A here to m
can possibly support planets. We are a G. We're a G,
and then not just a G, but a G two,

(01:49:53):
So G number two and then Roman numeral five because
that's the V is where they belong on this diagram.
The V says if they're here, like if they're in
this doing hydrogen and helium, they're they're V, which means
they're just they're called dwarfs, believe it or not. And
if they are here, actually up here, they're one a

(01:50:18):
Roman numeral one A. Okay, so that means super giants. Okay,
and we have regular giants here, which are types two, three,
and four Roman numerals. All right, and all these stars exist,
but stars up here are not going to be able
to have life bearing capabilities. It's the main sequence stars. Okay,

(01:50:41):
these are short lived. These are long lived. Do you
know down here these M stars, of the coolest m
stars there are terra. Do you know that not a
single one has actually died in the universe yet since
it's been born. They last three years. Yeah, they last
billions of years. Yeah, So there you see it. I mean,

(01:51:04):
this is kind of the bottom line is this is
the kind of thing where when we look at different
stars in the universe, we see that only certain ones
can support life like us. We also see that the
building blocks of life, if you're in the habitable zone,
come from asteroids and comets and meteors and from the
planets themselves. Okay, Now, I was watching as one of

(01:51:29):
the last things I'll mention, I was watching when the
curiosity rover on Mars was doing a grind. Okay, they
have a tool called the rat rock abrasion tool. And
by the way, I just have to say, there's a
scientist at JPL that got me started in jefferd Potion Lab,
that got me into astronomy. His name was Bert Lee

(01:51:52):
Bert and is nickname Gentry Lee, and he's the head
of all outer space robotic missions. He's the head engineer.
And I set my space station planned to him as
a nine year old, not knowing he was. I had
no idea who he was. He was a NASA scientist

(01:52:13):
at the time. And he wrote back and he sent
me a big box full of pamphlets and mission patches
and models and books and said, guy, an incredible guy.
Gentrily Yeah. And I actually talked to forty years later
and I said, you know, Gentry, you got me into astronomy.

(01:52:36):
And I told him the whole story about the my
space box. I used to revere that box had full
of all these things. And I said, thanks to you,
I got very interested in astronomy and I became an astronomer.
And he goes, I don't remember, but that's exactly the
kind of thing that I used to like to do,
because I felt that children were very important to foster that.
He's absolutely right, and that's why I do public outreach

(01:53:00):
astronomy today, probably because of that one man, because I
want to I want to foster the science and get
that curiosity going in the minds of people and folks.
I don't get paid for this. Well neither do you,
I guess, right, so a little bit. Yeah, yeah, I

(01:53:27):
did want to see I know, I had a question. Cha, yeah,
I know. We're getting down to it. Here it is,
here we go. I think. Now, when you're interested in
doing astronautical outreach, one of the things you look for
is what are called measure objects. Okay, Charles Messier in
the sixteen hundred and seventeen hundreds put together a list

(01:53:50):
of over one hundred different objects, one hundred and ten
different objects that were really cool. And he was doing
it not because of that. He was doing because he
was category rising what not to look at if you're
looking for comets, which I thought was hilarious. Yeah. So anyway,
Charles Messier categorizes objects as objects to avoid if you're

(01:54:13):
looking for comets, and it turned out they're the most
interesting objects we like to look at every day. Now,
it's really cool. The other nebula of their clusters, they're
globular clusters. There's special things the galaxies really neat, but
skypcher Life fan wants to know about doing a mecha marathon,
which is something people do. The best method is there's

(01:54:35):
a couple of times a year when it's best to
do that because all the mestry objects are all over
the sky. But there's only a couple of times a
year when you can actually look at the first one
and the last one and do them all in order.
A couple of times a year. You gotta wait for
you know, you gotta wait. You know it's an all nighter,
you're doing an all nighter. But yeah, so I will

(01:54:59):
ask even though you spell my name wrong there, Okay,
it's an m R C. Okay, but even even so,
I'll do this. I will. I'll help you with the
messia marathon. I'll get the dates that are best to
start looking all right, that's pretty cool. So I guess
I have to say, you know you guys. I want

(01:55:20):
to thank you guys for watching. This is our new spot.
Like I said, eight to ten on Wednesdays, and we'll
build a lot more live shows. Because of the fact
that it's not the weekend. I was killing us on
the weekend, you know. So that said, I'm going to
hang up here with you guys and with Tara. Isn't

(01:55:41):
she great? Give her around? You know?

Speaker 2 (01:55:44):
Yeah?

Speaker 4 (01:55:45):
Great? Great? Questions is just fun.

Speaker 1 (01:55:49):
Great, yeah, yeah. And it's always a pleasure having you
on with us, Tarah and listening to everybody in the chat,
and the questions are always good questions. I know I
missed some of your questions, and I'm sorry about that,
but I will I will get I will get to
answer them in our next sky to live stream when
we actually open the telescopes, you know. Uh. And so

(01:56:13):
I'm gonna open Benson tonight, but not publicly. I'm doing
it because I'm troubleshooting a little camera problem. You know.
Well the alternative is a fifteen hundred dollars fix. Yeah,
I'm gonna fix this so I can. Oh, I'll try right, Yeah.

(01:56:34):
I don't want to send you out to Benson's too
long a drive. You know. We have someone out there
that can go out there. We have two people now
that can go out there. We have a wonderful guy,
David from Starizona, who goes out there to help us,

(01:56:54):
and we also have another guy out there named Glenn
who will come out and he's only six minutes away.

Speaker 4 (01:57:00):
That's great. Yeah, a lot of support from everybody.

Speaker 1 (01:57:03):
Yeah, yeah, and so. And the thing that's important is
that astronomy is for everyone, Scientists for everyone. Sometimes you
just need to explained in the way that you need
to hear it. And that's what I do with shirt.
It's like this, well, thank you, I'm on the back,

(01:57:27):
you know. Oh well what's on the back is more
of the same, And they're all different equations. And like
I said, I've used many of these trigonometric identities in
the past, and I still use some of them, but
not not all of them. You know, that era, that
era was kind of fun right there. Just so it's

(01:57:49):
time to go. All right, guys, we'll have a good
time and we'll see you again on the next Skyter
live stream and Skyter Radio. Get it all.

Speaker 4 (01:57:57):
Hi everybody, Thank you. Beli