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Episode Transcript
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Speaker 1 (00:00):
Hi everyone, and welcome back to the morning round. But
we are alive once again. Those that want to join
me on the chat, you're most definitely welcome to do so.
Speaker 2 (00:07):
So let's get started here now where we love off yesterday.
Speaker 1 (00:12):
It is Tuesday, September seventeenth, and where we are with
the math and where it has taken us and where
we're most definitely headed regarding this and what's on the
table now, what's on the table is like minuscule as
opposed to what's on the board here, and so let's
look at this now.
Speaker 2 (00:33):
We're gonna look at this start again, and we're talking about.
Speaker 1 (00:35):
A low mass black hole and the radiation density that
we have to calculate. So we're gonna use the we
we're using an HO calculation. We're gonna talk about where
it takes us next. So we're talking about the we
talked of yesterday about where we're.
Speaker 2 (00:52):
Talking about the time of the age.
Speaker 1 (00:56):
Excuse me of cause we're talking about slow down in
time and we're also talking about time curvature, which are
two separate things and gotten there by two different calculations.
And the ingredients that gets us their regarding the particles
and what each element is made of and where each
element is coming from within space, so and it corresponds
(01:17):
with its own space time. And that's where we're headed
regarding the replica star, neutron star or two dwarft stars.
We're talking about the potential of the two draft stars
here also, but let's talk about this first here.
Speaker 2 (01:34):
So if we if we talk about this star and.
Speaker 1 (01:41):
The obviously the their mass.
Speaker 3 (01:46):
Loss to evaporation.
Speaker 1 (01:47):
With this, determine how many bes of years it takes
the star, the black hole specifically to die.
Speaker 2 (01:56):
Now so, and it meant.
Speaker 1 (02:00):
Due to the core heating up because we're focused on
the core. It goes on what is admitted into the
atmosphere around around the start itself. Because remember we're speaking
of spectification because of the strong tide of forces that
low mass black holes have.
Speaker 2 (02:15):
And what that change is what that change.
Speaker 1 (02:20):
Emmits because we're speaking of speak pulling the the particles
back into the core. So we are where we're with
the math here now is we're speaking about the predominantly radiation, gas,
gravity and dust.
Speaker 2 (02:37):
So now so we do we look.
Speaker 1 (02:39):
At listen, it takes us back and looking at the
star itself now and looking at its core before the
loss of mass was began. So we're talking about early
space times and the radiation calculated radiation of matter, the
dark energy, because it's the majority of dark energy in
(03:00):
the over our density. So we're talking about quantum radiation,
feel absorption.
Speaker 2 (03:05):
We're no, we know we're talking to the field that we're.
Speaker 1 (03:07):
Speaking of is the radiation fiel because we're speaking of
gamma rays and radiation electromagnetic field. So we're speaking of
explosion now regarding this star, but we're speaking of explosion
regarding something else, and we need that to happen because remember,
we're needing a particle so that we can really dissect
(03:29):
and look at what is being pulled into the core
of the star and what changes that that would denote.
But after spogification has happened, so and now, so when
we do that, when with the ho calculations regarding the
start itself, it takes us where do you all?
Speaker 3 (03:47):
Where did you all get that?
Speaker 1 (03:48):
It takes us? Where did you all get that? It
takes us? Well, it takes us to the supernova. Now,
we spoke yesterday that the super nova, the type of
super nova that it is, is lax and that can
go along.
Speaker 2 (04:09):
With you all that may have with your.
Speaker 1 (04:12):
Own calculations, may have stated, well, it would be with
it being a draft star. Now, but remember with the
supernova calculations, it takes us to what is it dust?
So we're dealing with dust and dust particles majority with
this super nova it would just be dust and we
(04:33):
need those particle ingredients.
Speaker 2 (04:35):
But with that dust, it does.
Speaker 3 (04:37):
Take us to white draft star.
Speaker 2 (04:40):
And yesterday we stated that, well, I stated two draft stars.
Speaker 1 (04:45):
Now, so with this dust, because we're dealing with radiation
majority gas, gravity and dust with what's on the table,
that's what we're dealing with now.
Speaker 2 (04:55):
So with this dust, it takes us.
Speaker 1 (04:58):
Now, this carried dust here because remember with the start
itself and where with.
Speaker 2 (05:03):
The HO calculations, it takes us to age.
Speaker 1 (05:08):
Beginning star evolution and the what it was within the
particles of that and that is calculating what emmits through.
Speaker 2 (05:17):
The explosion of the type of energy release.
Speaker 1 (05:21):
And we already stated that that was I stated yesterday
that we were talking about radiation feel and your manity
rigid radiation and the material that's released in the atmosphere
now that stays around.
Speaker 2 (05:34):
This black hole.
Speaker 1 (05:35):
Even though we know that black holes are weak as
it relates to pulling in towards them.
Speaker 2 (05:40):
But they have the high the strong title.
Speaker 1 (05:45):
Forces and that's the specification that that goes along with
the time curvature. But we'll get into that in a
minute because that's the exciting part and dies what's going
to give more information now. So now, so if we
talk about the so so we have the supernova being
(06:06):
just it's just dust and the dust particles that we're
needing cause we're needing to get down to the to root,
to the root of it. We're need to get into
the particles and we have to to formulate the age
of the particles, and we do that by formulating the
age of the star itself and whatever values you will
all put in. Also we're speaking and where do you
get the values from? Whereby what's on the table and
(06:28):
the potential of replica star neutron star are two drass
stars being the uh spotification of spocification of what the
stars core can pull into it.
Speaker 2 (06:42):
And we're working primarily with gravity.
Speaker 1 (06:45):
Because we know that we're working primarily with gravity because
of where the next calculations take us.
Speaker 3 (06:52):
It takes us straight to this spoglification.
Speaker 2 (06:55):
Now, and let's talk.
Speaker 1 (06:57):
About steps out of the spagification for a bit in
the time curvature, most specifically, because yesterday I stated that, well,
we obviously know that there is a massive object in orbit,
(07:19):
and then I stated that there could be two. One
would be Sun or Sun similar. Now, how do we
get the calculations that it would be Sun or Son similar?
The value calculations that it will be Sun and so
Sun similar, Because we're talking about majority radiation, gas and gravity,
(07:39):
and we're speaking about the explosion core and what the
particles that are are are are emitted into the atmosphere
released in the atmosphere.
Speaker 2 (07:50):
And what the material is that it carries.
Speaker 1 (07:53):
Now so, and we noticed by the calculations of the HO,
the HO calculations of the starts off the black hole
itself and what it is primarily made of the core
the center that that notes what it would be emitting
into the atmosphere material and energy released.
Speaker 3 (08:17):
Now so, if we look.
Speaker 1 (08:20):
At time curvature, and as I stated yesterday that the
secondary massive object.
Speaker 3 (08:36):
State that it.
Speaker 2 (08:37):
Did not have to be in orbit.
Speaker 1 (08:38):
Because we talked about distance, we have to talk why
do we have to talk about distance? Well, we have
to talk about distance because we're talking about the slowing
down of time, and also we're talking in that in
the the So because we're speaking of the slowing down
of time, also that density can be calculated by well,
the disity can be calculated by factor okay, because we're.
Speaker 2 (09:02):
Gonna slow it down of time.
Speaker 1 (09:03):
So that lets us know that the secondary massive object
does not have to be in orbit, and that took
us to cluster galaxies. But also the calculations of the
specification took us to looking at the volume of the
cluster galaxies. Now, so let's talk about specification first and
(09:24):
then we're good to the custer galaxies. We'll get to
this other massive object that is not in orbits, but
is massive enough to have a well, because we're talking
about spogification, is massive enough to have an effect in
time curvature, which is eaque with the spotification in this
(09:46):
instance at distance and what the massive object is constructive of.
Speaker 3 (09:53):
So we're talking about particles.
Speaker 1 (09:55):
Particles released in the energy of those particles now, so
the type of energy within those particles. So let's look
at spotification now because of what we're working with and
we're what are we working with, Well, we're working with
replica Star, Neutron Star are two draw stars, two white
(10:20):
Draft stars. Now we're talking about dealing with a lot
of dark matter, especially with the we're especially with the secondary.
Speaker 2 (10:32):
Massive. It could be.
Speaker 1 (10:36):
Super massive here with this, we're gonna do the calculation
that lets us know if it can be super massive
and still be within the range of white white Draft
star too, specifically Replica Star a neutron star. But it
is massive now and it could be the the Their
massiveness could be equal to that of the prime very
(11:00):
object that is within orbit, and we've already calculated that
as being the sign. So when we look at spetification
and strong strong tidal forces, we look at the the
the what is creating a part of the creation of
(11:21):
the time curvature as stretched out and not actually curve.
It will be stretched out and not actually curve. And
so how do we know it would be stretched out
and not actually curve, Well, because we're the field equations
that we're dealing with and we're.
Speaker 2 (11:39):
Dealing with their radiation film. So it will be stretched out.
Speaker 1 (11:43):
The spotification will be stretched out, not actually curve.
Speaker 3 (11:47):
Or bent, and that would take us too.
Speaker 1 (11:56):
Now, the massive object that is in orbit in the
cluster Gallay season.
Speaker 2 (12:00):
That's what we left out yesterday.
Speaker 3 (12:01):
So this is the most important, This.
Speaker 1 (12:03):
Is very this is the most not the most this
is the most important part, but this is a very
informative part. This is where we're gonna be looking at
a lot of different particles. We're gonna be looking at
multulee of gravitational fields.
Speaker 3 (12:19):
We're gonna be looking at a multitude of.
Speaker 1 (12:24):
Space times and a multitude of potential meaning meaning the
actual physics within the galaxies. Because with custer galaxries, we're
(12:48):
speaking of a we're not talking to we're not speaking
of elliptical galaxies.
Speaker 2 (12:54):
We're speaking of irregular cluster galaxies.
Speaker 1 (12:56):
So we're talking about a multitude of variety of galaxies.
So that's why we're gonna have different space times, different particles,
different stars, much to the stars, a motude of explosion,
because we're talking about stars within stars that we're talking
(13:18):
about we're talking about dark energy. So in volume and mass,
and it is massive, and it could be equally massive
to the Sun, the primary orbiting closer orbit object in orbit,
it could be equal in mass to that. But this
will also come along with volume, not but it takes
(13:46):
us to the slow down in time. Also when we
get onto the cluster galaxies, it takes us into the
slowdown of time also obviously with the with the curvature,
the space time curvature, but it takes us to the
looking that this slow down in time.
Speaker 2 (14:01):
So we'll talk about time.
Speaker 1 (14:02):
Dolation is what it would be, and the radiation that
electromagnetic feel that we're speaking of speed cause we're talking
about distance in this in in our star, our lower
mass black hole, in the weakness of being able to
(14:24):
pull towards it. Lets us know the power gravitational power
of the two massive objects orbiting around it. Well the
secondary massive massive object orbited that isn't in its orbit
in what it consists of with these cluster galaxies and
(14:53):
the gravity. So this is the most the the these
galaxies are the most important here in their volume cause
we're talking about hot gas, so we're talking about explosions
(15:15):
and what they're emitting also, and what they've admitted is
what's being is what's I was a part of the
ingredients in the spot of the spot gification and what's
around our star, our black hole, the massive black hole
then lower mass black hole, excuse me, and what's being
pulled back into this core and the gravitational ability for
(15:40):
it to be pulled into is where things get pretty
interesting because even it be because looking at their irregular
clusters w w W. Because we're not talking about electrical galaxies.
(16:03):
We're talking about irregular galaxy clusters. So we have spirals
there no specified shape, but spirals. Why spirals because the
spotification is stretched out and because of the type of
(16:23):
emissions our from the lower mass black hole, because of
the type of mission and was released into the atmosphere,
the material and the energy released to the atmosphere within
the atmosphere, that particle collision, not growing in size, particle
collision we spoke of yesterday, but the type of galaxy clusters,
(16:45):
the type of our second that the type of massive
the type of massive object that is not a part
of the orbits, but most definitely influencing what is being
pulled in gravitationally into the core.
Speaker 2 (17:07):
Of our of our start and remember I'll start not
being able to admit light and doesn't emit.
Speaker 1 (17:20):
Light, but being able to pull in why, well, because
of this spoglification and the massive.
Speaker 3 (17:30):
Object within its.
Speaker 1 (17:34):
Not even within its not even within its orbit. As
I stated, yesterday, not even within its orbit. And that's
the complexity of it. It's very it's very complex, but
it's very understandably applicable. And why what makes it understand
(17:54):
to be applical what because of the custom galaxies. And
this is where the real work comes in, because this
is where we're looking at what type of emissions, what
type of particles, where they consist of the age other particles,
what type of galaxies, what the opposite, what type of stars,
(18:14):
what type of matter?
Speaker 3 (18:16):
What would know?
Speaker 4 (18:17):
What we did in primary with dark matter, even with
the same even with the.
Speaker 1 (18:33):
Time dilation, is it would be close to the speed
of light, not at the speed of light. And we
in the calculation of what makes that soul, it's gonna
be within the within the type of clusters galaxies, their
(18:55):
ho calculations, age.
Speaker 2 (19:00):
Space time, probability of.
Speaker 1 (19:08):
What can be achieved laws of physics corresponding with their
space time. So this is where we get into the
heavier application of the calculations that will allow the gravity
to be pulled into the core of what is left
(19:31):
of our star. So at this point we've broken it
down to knowing that we're dealing with primary radiation gas gravity, dust.
Speaker 2 (19:56):
And all of this is due to particle collisions and explosions.
Speaker 1 (20:10):
Because even when we're looking at but before we before
we introduce.
Speaker 2 (20:15):
The secondary massive.
Speaker 1 (20:17):
Object that is not in rigit orbit, but which are
the galaxy clusters, Before we introduced that, we were already
looking at the conversion of gravity of gravitational energy in
the particles. Okay, and what we were the energies that
work was the gravitational particles. Well, they are from the
(20:38):
emission of the star, the energy released and the material.
Speaker 2 (20:48):
And that's where the time curvature comes from.
Speaker 1 (20:50):
The time curvature comes from the black hole itself, and
it's ho calculations letting us know that age and letting
us know its laws of physics and space time, also
(21:13):
letting us know the potential of its continued because remember
we're working with the core still even though there has
been mass laws and that's what was needed. That's what's
needed cause we're talking about creating now. So we're talking
about the pulling, the pulling in. We have two draw
(21:39):
star fats. We have it from the dust of the supernova.
It's just dust. It's just dust.
Speaker 3 (21:48):
We in this application of what we're doing, is it.
Speaker 1 (21:50):
Does so, and we also have it from the custom galaxies.
That's why the that's why what is introduced is the
replicast neutrons start two draws stars. That's why I introduce
that as the calculations of what would be formulated after
the the material is pulled into the core. The probability
(22:13):
of what could be formulated into the materials. Where is
pulling this star as it as as it sits on
the table without depth calculations, you know, without dept calculations,
it would be pulling more towards.
Speaker 2 (22:31):
Two draws stars, replica star.
Speaker 1 (22:42):
It's still neutron star courer, just now getting into the
depth calculations with the Clustre galaxies and with Custer galaxies
(23:04):
and and spotification. It brings us to c to slicing.
It brings us to slicing because we will go into neutrinos.
(23:32):
So because we're looking at the w W, we're we're looking.
Speaker 2 (23:40):
At the particles, but looking at the particles as they're.
Speaker 3 (23:51):
Gravitationally pulled.
Speaker 1 (23:55):
Towards the spotification and what happens to them, because remember
we're pulling into the core and the spotification is a
part of what is creating the change. It's a part
of what is is creating the the change. What is
pulling particles together, the magnetic force of pulling them to
(24:18):
do gravitational force excuse me, of pulling them together, and
they're pulling them into the core of what is left
of our star and in w having to ha having
(24:47):
it take us to slicing because because of the dust
particles that.
Speaker 2 (24:52):
We're dealing with.
Speaker 1 (24:57):
And the age and the laws of physics that would
determine their capacity.
Speaker 3 (25:10):
Now, so to do what is associated with.
Speaker 1 (25:14):
Having to be done or be what is associated excuse me,
what what has to be? We're to create the replica star,
neutrons star of the two Draws stars. So now that
we're dealing with the particles itself, the part of the
(25:36):
particles themselves, and obviously with the particles of their mission,
but the now dealing with the the particles of the
gap cluster galaxies and now able to do those calculations,
we could see what the potential of outcome White Drawt Star,
two Neutron star or replical star and their potential of
(25:59):
coming into the core. And they're being light the type
(26:27):
of gas that these galaxies are meant their their h
the ho calculations for for the coastal galaxies are gonna
be very important and very telling. I'll say their volume.
The volume calculations are gonna be very important, very telling.
(27:02):
That also aligns itself with the time dilations and our
in the weakness of the gravitficational pull of our star
is also associated with the time dilation could be calculated
any time dilation alongside the quantum fluctuations uh the well
(27:30):
that would be the similar the qu quantum function fluctuations
of the secondary object, which would be the massive galaxies
in the the massive cluster galaxies.
Speaker 2 (27:40):
It's like a lot of calculations there of potential.
Speaker 1 (27:44):
So this is a lot of information, a lot of
information nowadays y as of yesterday we introduced.
Speaker 2 (27:49):
The cluster galaxies into the equation.
Speaker 3 (27:52):
A lot of information help.
Speaker 1 (28:03):
Could because even within this information we're talking about different
types of gravity and all this is lying up wellness all.
Speaker 2 (28:13):
Necessary to pull into the core of our start.
Speaker 1 (28:15):
Because remember the the the the gravitational pull.
Speaker 3 (28:18):
With the is a weakeed.
Speaker 1 (28:24):
Is a weakened because the mass is all to evaporation evaporation,
so that would content that would contain any type of gravitational.
Speaker 3 (28:32):
Pull towards.
Speaker 2 (28:37):
Already not emitting any type of light.
Speaker 1 (28:45):
So where things stand is that where we are now
dealing with the particles from the explosions, and we have
it coming from which we have the uh starts self
there and then we also have it with relax with
(29:07):
as it does. Then we have with the custom Well,
we have to calculate the disclosion with the customer galaxies
because it start dependent and that's gonna come from the
from the HO calculations.
Speaker 2 (29:19):
They have to give a lot of information.
Speaker 1 (29:22):
So we're differently dealing with as a stated radiation, that's
the field we're dealing with, that's the quantum field. We're
dealing with radiation, gravity, different types of gravity.
Speaker 2 (29:35):
Gas does particles, and we're dealing with.
Speaker 3 (29:47):
Space time curvature.
Speaker 1 (29:48):
Space also slow down slowed down in time, so we're
dealing with time dilations and we're dealing with much of
the space times because.
Speaker 3 (29:57):
Of the custom galaxies. We're dealing with a mu altitude of.
Speaker 1 (30:02):
Laws of physics because we're speaking of the Customer galaxies
and that's depending on the H calculations, and we're dealing
with spirals, we're dealing with irregular galaxies. We're dealing with spiles,
so that's gonna be incorporated in the calculations. Also because
it holds the spiral holds a high potential for their
to formulate new stars. Also just like the dust, because
(30:28):
we're speaking of type laps and it's obviously just like
this spotification. So these are the ingredients and the ingredients
of what we were looking for. It's like we need
the particles after the explosion has occurred, so we're dealing
with now we're dealing with the with the actual particles
and time and space time. We're talking about curvature and
(30:48):
time dilations that we're talking about pulling into our star,
into the core of our star, and the potential of.
Speaker 2 (30:55):
The ingredients of what makes that necessary.
Speaker 3 (31:00):
Okay from wanted till next time. We'll continue this tomorrow.
Speaker 2 (31:02):
Thanks for listening. See what the calculation the math takes
us by
Hi everyone, and welcome back to the morning round. But
we are alive once again. Those that want to join
me on the chat, you're most definitely welcome to do so.
Speaker 2 (00:07):
So let's get started here now where we love off yesterday.
Speaker 1 (00:12):
It is Tuesday, September seventeenth, and where we are with
the math and where it has taken us and where
we're most definitely headed regarding this and what's on the
table now, what's on the table is like minuscule as
opposed to what's on the board here, and so let's
look at this now.
Speaker 2 (00:33):
We're gonna look at this start again, and we're talking about.
Speaker 1 (00:35):
A low mass black hole and the radiation density that
we have to calculate. So we're gonna use the we
we're using an HO calculation. We're gonna talk about where
it takes us next. So we're talking about the we
talked of yesterday about where we're.
Speaker 2 (00:52):
Talking about the time of the age.
Speaker 1 (00:56):
Excuse me of cause we're talking about slow down in
time and we're also talking about time curvature, which are
two separate things and gotten there by two different calculations.
And the ingredients that gets us their regarding the particles
and what each element is made of and where each
element is coming from within space, so and it corresponds
(01:17):
with its own space time. And that's where we're headed
regarding the replica star, neutron star or two dwarft stars.
We're talking about the potential of the two draft stars
here also, but let's talk about this first here.
Speaker 2 (01:34):
So if we if we talk about this star and.
Speaker 1 (01:41):
The obviously the their mass.
Speaker 3 (01:46):
Loss to evaporation.
Speaker 1 (01:47):
With this, determine how many bes of years it takes
the star, the black hole specifically to die.
Speaker 2 (01:56):
Now so, and it meant.
Speaker 1 (02:00):
Due to the core heating up because we're focused on
the core. It goes on what is admitted into the
atmosphere around around the start itself. Because remember we're speaking
of spectification because of the strong tide of forces that
low mass black holes have.
Speaker 2 (02:15):
And what that change is what that change.
Speaker 1 (02:20):
Emmits because we're speaking of speak pulling the the particles
back into the core. So we are where we're with
the math here now is we're speaking about the predominantly radiation, gas,
gravity and dust.
Speaker 2 (02:37):
So now so we do we look.
Speaker 1 (02:39):
At listen, it takes us back and looking at the
star itself now and looking at its core before the
loss of mass was began. So we're talking about early
space times and the radiation calculated radiation of matter, the
dark energy, because it's the majority of dark energy in
(03:00):
the over our density. So we're talking about quantum radiation,
feel absorption.
Speaker 2 (03:05):
We're no, we know we're talking to the field that we're.
Speaker 1 (03:07):
Speaking of is the radiation fiel because we're speaking of
gamma rays and radiation electromagnetic field. So we're speaking of
explosion now regarding this star, but we're speaking of explosion
regarding something else, and we need that to happen because remember,
we're needing a particle so that we can really dissect
(03:29):
and look at what is being pulled into the core
of the star and what changes that that would denote.
But after spogification has happened, so and now, so when
we do that, when with the ho calculations regarding the
start itself, it takes us where do you all?
Speaker 3 (03:47):
Where did you all get that?
Speaker 1 (03:48):
It takes us? Where did you all get that? It
takes us? Well, it takes us to the supernova. Now,
we spoke yesterday that the super nova, the type of
super nova that it is, is lax and that can
go along.
Speaker 2 (04:09):
With you all that may have with your.
Speaker 1 (04:12):
Own calculations, may have stated, well, it would be with
it being a draft star. Now, but remember with the
supernova calculations, it takes us to what is it dust?
So we're dealing with dust and dust particles majority with
this super nova it would just be dust and we
(04:33):
need those particle ingredients.
Speaker 2 (04:35):
But with that dust, it does.
Speaker 3 (04:37):
Take us to white draft star.
Speaker 2 (04:40):
And yesterday we stated that, well, I stated two draft stars.
Speaker 1 (04:45):
Now, so with this dust, because we're dealing with radiation
majority gas, gravity and dust with what's on the table,
that's what we're dealing with now.
Speaker 2 (04:55):
So with this dust, it takes us.
Speaker 1 (04:58):
Now, this carried dust here because remember with the start
itself and where with.
Speaker 2 (05:03):
The HO calculations, it takes us to age.
Speaker 1 (05:08):
Beginning star evolution and the what it was within the
particles of that and that is calculating what emmits through.
Speaker 2 (05:17):
The explosion of the type of energy release.
Speaker 1 (05:21):
And we already stated that that was I stated yesterday
that we were talking about radiation feel and your manity
rigid radiation and the material that's released in the atmosphere
now that stays around.
Speaker 2 (05:34):
This black hole.
Speaker 1 (05:35):
Even though we know that black holes are weak as
it relates to pulling in towards them.
Speaker 2 (05:40):
But they have the high the strong title.
Speaker 1 (05:45):
Forces and that's the specification that that goes along with
the time curvature. But we'll get into that in a
minute because that's the exciting part and dies what's going
to give more information now. So now, so if we
talk about the so so we have the supernova being
(06:06):
just it's just dust and the dust particles that we're
needing cause we're needing to get down to the to root,
to the root of it. We're need to get into
the particles and we have to to formulate the age
of the particles, and we do that by formulating the
age of the star itself and whatever values you will
all put in. Also we're speaking and where do you
get the values from? Whereby what's on the table and
(06:28):
the potential of replica star neutron star are two drass
stars being the uh spotification of spocification of what the
stars core can pull into it.
Speaker 2 (06:42):
And we're working primarily with gravity.
Speaker 1 (06:45):
Because we know that we're working primarily with gravity because
of where the next calculations take us.
Speaker 3 (06:52):
It takes us straight to this spoglification.
Speaker 2 (06:55):
Now, and let's talk.
Speaker 1 (06:57):
About steps out of the spagification for a bit in
the time curvature, most specifically, because yesterday I stated that, well,
we obviously know that there is a massive object in orbit,
(07:19):
and then I stated that there could be two. One
would be Sun or Sun similar. Now, how do we
get the calculations that it would be Sun or Son similar?
The value calculations that it will be Sun and so
Sun similar, Because we're talking about majority radiation, gas and gravity,
(07:39):
and we're speaking about the explosion core and what the
particles that are are are are emitted into the atmosphere
released in the atmosphere.
Speaker 2 (07:50):
And what the material is that it carries.
Speaker 1 (07:53):
Now so, and we noticed by the calculations of the HO,
the HO calculations of the starts off the black hole
itself and what it is primarily made of the core
the center that that notes what it would be emitting
into the atmosphere material and energy released.
Speaker 3 (08:17):
Now so, if we look.
Speaker 1 (08:20):
At time curvature, and as I stated yesterday that the
secondary massive object.
Speaker 3 (08:36):
State that it.
Speaker 2 (08:37):
Did not have to be in orbit.
Speaker 1 (08:38):
Because we talked about distance, we have to talk why
do we have to talk about distance? Well, we have
to talk about distance because we're talking about the slowing
down of time, and also we're talking in that in
the the So because we're speaking of the slowing down
of time, also that density can be calculated by well,
the disity can be calculated by factor okay, because we're.
Speaker 2 (09:02):
Gonna slow it down of time.
Speaker 1 (09:03):
So that lets us know that the secondary massive object
does not have to be in orbit, and that took
us to cluster galaxies. But also the calculations of the
specification took us to looking at the volume of the
cluster galaxies. Now, so let's talk about specification first and
(09:24):
then we're good to the custer galaxies. We'll get to
this other massive object that is not in orbits, but
is massive enough to have a well, because we're talking
about spogification, is massive enough to have an effect in
time curvature, which is eaque with the spotification in this
(09:46):
instance at distance and what the massive object is constructive of.
Speaker 3 (09:53):
So we're talking about particles.
Speaker 1 (09:55):
Particles released in the energy of those particles now, so
the type of energy within those particles. So let's look
at spotification now because of what we're working with and
we're what are we working with, Well, we're working with
replica Star, Neutron Star are two draw stars, two white
(10:20):
Draft stars. Now we're talking about dealing with a lot
of dark matter, especially with the we're especially with the secondary.
Speaker 2 (10:32):
Massive. It could be.
Speaker 1 (10:36):
Super massive here with this, we're gonna do the calculation
that lets us know if it can be super massive
and still be within the range of white white Draft
star too, specifically Replica Star a neutron star. But it
is massive now and it could be the the Their
massiveness could be equal to that of the prime very
(11:00):
object that is within orbit, and we've already calculated that
as being the sign. So when we look at spetification
and strong strong tidal forces, we look at the the
the what is creating a part of the creation of
(11:21):
the time curvature as stretched out and not actually curve.
It will be stretched out and not actually curve. And
so how do we know it would be stretched out
and not actually curve, Well, because we're the field equations
that we're dealing with and we're.
Speaker 2 (11:39):
Dealing with their radiation film. So it will be stretched out.
Speaker 1 (11:43):
The spotification will be stretched out, not actually curve.
Speaker 3 (11:47):
Or bent, and that would take us too.
Speaker 1 (11:56):
Now, the massive object that is in orbit in the
cluster Gallay season.
Speaker 2 (12:00):
That's what we left out yesterday.
Speaker 3 (12:01):
So this is the most important, This.
Speaker 1 (12:03):
Is very this is the most not the most this
is the most important part, but this is a very
informative part. This is where we're gonna be looking at
a lot of different particles. We're gonna be looking at
multulee of gravitational fields.
Speaker 3 (12:19):
We're gonna be looking at a multitude of.
Speaker 1 (12:24):
Space times and a multitude of potential meaning meaning the
actual physics within the galaxies. Because with custer galaxries, we're
(12:48):
speaking of a we're not talking to we're not speaking
of elliptical galaxies.
Speaker 2 (12:54):
We're speaking of irregular cluster galaxies.
Speaker 1 (12:56):
So we're talking about a multitude of variety of galaxies.
So that's why we're gonna have different space times, different particles,
different stars, much to the stars, a motude of explosion,
because we're talking about stars within stars that we're talking
(13:18):
about we're talking about dark energy. So in volume and mass,
and it is massive, and it could be equally massive
to the Sun, the primary orbiting closer orbit object in orbit,
it could be equal in mass to that. But this
will also come along with volume, not but it takes
(13:46):
us to the slow down in time. Also when we
get onto the cluster galaxies, it takes us into the
slowdown of time also obviously with the with the curvature,
the space time curvature, but it takes us to the
looking that this slow down in time.
Speaker 2 (14:01):
So we'll talk about time.
Speaker 1 (14:02):
Dolation is what it would be, and the radiation that
electromagnetic feel that we're speaking of speed cause we're talking
about distance in this in in our star, our lower
mass black hole, in the weakness of being able to
(14:24):
pull towards it. Lets us know the power gravitational power
of the two massive objects orbiting around it. Well the
secondary massive massive object orbited that isn't in its orbit
in what it consists of with these cluster galaxies and
(14:53):
the gravity. So this is the most the the these
galaxies are the most important here in their volume cause
we're talking about hot gas, so we're talking about explosions
(15:15):
and what they're emitting also, and what they've admitted is
what's being is what's I was a part of the
ingredients in the spot of the spot gification and what's
around our star, our black hole, the massive black hole
then lower mass black hole, excuse me, and what's being
pulled back into this core and the gravitational ability for
(15:40):
it to be pulled into is where things get pretty
interesting because even it be because looking at their irregular
clusters w w W. Because we're not talking about electrical galaxies.
(16:03):
We're talking about irregular galaxy clusters. So we have spirals
there no specified shape, but spirals. Why spirals because the
spotification is stretched out and because of the type of
(16:23):
emissions our from the lower mass black hole, because of
the type of mission and was released into the atmosphere,
the material and the energy released to the atmosphere within
the atmosphere, that particle collision, not growing in size, particle
collision we spoke of yesterday, but the type of galaxy clusters,
(16:45):
the type of our second that the type of massive
the type of massive object that is not a part
of the orbits, but most definitely influencing what is being
pulled in gravitationally into the core.
Speaker 2 (17:07):
Of our of our start and remember I'll start not
being able to admit light and doesn't emit.
Speaker 1 (17:20):
Light, but being able to pull in why, well, because
of this spoglification and the massive.
Speaker 3 (17:30):
Object within its.
Speaker 1 (17:34):
Not even within its not even within its orbit. As
I stated, yesterday, not even within its orbit. And that's
the complexity of it. It's very it's very complex, but
it's very understandably applicable. And why what makes it understand
(17:54):
to be applical what because of the custom galaxies. And
this is where the real work comes in, because this
is where we're looking at what type of emissions, what
type of particles, where they consist of the age other particles,
what type of galaxies, what the opposite, what type of stars,
(18:14):
what type of matter?
Speaker 3 (18:16):
What would know?
Speaker 4 (18:17):
What we did in primary with dark matter, even with
the same even with the.
Speaker 1 (18:33):
Time dilation, is it would be close to the speed
of light, not at the speed of light. And we
in the calculation of what makes that soul, it's gonna
be within the within the type of clusters galaxies, their
(18:55):
ho calculations, age.
Speaker 2 (19:00):
Space time, probability of.
Speaker 1 (19:08):
What can be achieved laws of physics corresponding with their
space time. So this is where we get into the
heavier application of the calculations that will allow the gravity
to be pulled into the core of what is left
(19:31):
of our star. So at this point we've broken it
down to knowing that we're dealing with primary radiation gas gravity, dust.
Speaker 2 (19:56):
And all of this is due to particle collisions and explosions.
Speaker 1 (20:10):
Because even when we're looking at but before we before
we introduce.
Speaker 2 (20:15):
The secondary massive.
Speaker 1 (20:17):
Object that is not in rigit orbit, but which are
the galaxy clusters, Before we introduced that, we were already
looking at the conversion of gravity of gravitational energy in
the particles. Okay, and what we were the energies that
work was the gravitational particles. Well, they are from the
(20:38):
emission of the star, the energy released and the material.
Speaker 2 (20:48):
And that's where the time curvature comes from.
Speaker 1 (20:50):
The time curvature comes from the black hole itself, and
it's ho calculations letting us know that age and letting
us know its laws of physics and space time, also
(21:13):
letting us know the potential of its continued because remember
we're working with the core still even though there has
been mass laws and that's what was needed. That's what's
needed cause we're talking about creating now. So we're talking
about the pulling, the pulling in. We have two draw
(21:39):
star fats. We have it from the dust of the supernova.
It's just dust. It's just dust.
Speaker 3 (21:48):
We in this application of what we're doing, is it.
Speaker 1 (21:50):
Does so, and we also have it from the custom galaxies.
That's why the that's why what is introduced is the
replicast neutrons start two draws stars. That's why I introduce
that as the calculations of what would be formulated after
the the material is pulled into the core. The probability
(22:13):
of what could be formulated into the materials. Where is
pulling this star as it as as it sits on
the table without depth calculations, you know, without dept calculations,
it would be pulling more towards.
Speaker 2 (22:31):
Two draws stars, replica star.
Speaker 1 (22:42):
It's still neutron star courer, just now getting into the
depth calculations with the Clustre galaxies and with Custer galaxies
(23:04):
and and spotification. It brings us to c to slicing.
It brings us to slicing because we will go into neutrinos.
(23:32):
So because we're looking at the w W, we're we're looking.
Speaker 2 (23:40):
At the particles, but looking at the particles as they're.
Speaker 3 (23:51):
Gravitationally pulled.
Speaker 1 (23:55):
Towards the spotification and what happens to them, because remember
we're pulling into the core and the spotification is a
part of what is creating the change. It's a part
of what is is creating the the change. What is
pulling particles together, the magnetic force of pulling them to
(24:18):
do gravitational force excuse me, of pulling them together, and
they're pulling them into the core of what is left
of our star and in w having to ha having
(24:47):
it take us to slicing because because of the dust
particles that.
Speaker 2 (24:52):
We're dealing with.
Speaker 1 (24:57):
And the age and the laws of physics that would
determine their capacity.
Speaker 3 (25:10):
Now, so to do what is associated with.
Speaker 1 (25:14):
Having to be done or be what is associated excuse me,
what what has to be? We're to create the replica star,
neutrons star of the two Draws stars. So now that
we're dealing with the particles itself, the part of the
(25:36):
particles themselves, and obviously with the particles of their mission,
but the now dealing with the the particles of the
gap cluster galaxies and now able to do those calculations,
we could see what the potential of outcome White Drawt Star,
two Neutron star or replical star and their potential of
(25:59):
coming into the core. And they're being light the type
(26:27):
of gas that these galaxies are meant their their h
the ho calculations for for the coastal galaxies are gonna
be very important and very telling. I'll say their volume.
The volume calculations are gonna be very important, very telling.
(27:02):
That also aligns itself with the time dilations and our
in the weakness of the gravitficational pull of our star
is also associated with the time dilation could be calculated
any time dilation alongside the quantum fluctuations uh the well
(27:30):
that would be the similar the qu quantum function fluctuations
of the secondary object, which would be the massive galaxies
in the the massive cluster galaxies.
Speaker 2 (27:40):
It's like a lot of calculations there of potential.
Speaker 1 (27:44):
So this is a lot of information, a lot of
information nowadays y as of yesterday we introduced.
Speaker 2 (27:49):
The cluster galaxies into the equation.
Speaker 3 (27:52):
A lot of information help.
Speaker 1 (28:03):
Could because even within this information we're talking about different
types of gravity and all this is lying up wellness all.
Speaker 2 (28:13):
Necessary to pull into the core of our start.
Speaker 1 (28:15):
Because remember the the the the gravitational pull.
Speaker 3 (28:18):
With the is a weakeed.
Speaker 1 (28:24):
Is a weakened because the mass is all to evaporation evaporation,
so that would content that would contain any type of gravitational.
Speaker 3 (28:32):
Pull towards.
Speaker 2 (28:37):
Already not emitting any type of light.
Speaker 1 (28:45):
So where things stand is that where we are now
dealing with the particles from the explosions, and we have
it coming from which we have the uh starts self
there and then we also have it with relax with
(29:07):
as it does. Then we have with the custom Well,
we have to calculate the disclosion with the customer galaxies
because it start dependent and that's gonna come from the
from the HO calculations.
Speaker 2 (29:19):
They have to give a lot of information.
Speaker 1 (29:22):
So we're differently dealing with as a stated radiation, that's
the field we're dealing with, that's the quantum field. We're
dealing with radiation, gravity, different types of gravity.
Speaker 2 (29:35):
Gas does particles, and we're dealing with.
Speaker 3 (29:47):
Space time curvature.
Speaker 1 (29:48):
Space also slow down slowed down in time, so we're
dealing with time dilations and we're dealing with much of
the space times because.
Speaker 3 (29:57):
Of the custom galaxies. We're dealing with a mu altitude of.
Speaker 1 (30:02):
Laws of physics because we're speaking of the Customer galaxies
and that's depending on the H calculations, and we're dealing
with spirals, we're dealing with irregular galaxies. We're dealing with spiles,
so that's gonna be incorporated in the calculations. Also because
it holds the spiral holds a high potential for their
to formulate new stars. Also just like the dust, because
(30:28):
we're speaking of type laps and it's obviously just like
this spotification. So these are the ingredients and the ingredients
of what we were looking for. It's like we need
the particles after the explosion has occurred, so we're dealing
with now we're dealing with the with the actual particles
and time and space time. We're talking about curvature and
(30:48):
time dilations that we're talking about pulling into our star,
into the core of our star, and the potential of.
Speaker 2 (30:55):
The ingredients of what makes that necessary.
Speaker 3 (31:00):
Okay from wanted till next time. We'll continue this tomorrow.
Speaker 2 (31:02):
Thanks for listening. See what the calculation the math takes
us by
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