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Episode Transcript
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Speaker 1 (00:01):
Happy one and welcome back to the morning ground. But
we are alive once again. It is Monday, September sixteenth.
Those that want to join in with me on the chat,
you're most welcome to do. So let's see what we're
speaking about this week later material on the table. Midweek,
we'll look at our math and see where that takes us,
cause it will be most definitely informative, and we'll see
(00:21):
what things what things evolve into. So we're looking at
lower mass black holes and remember what lower mass black
holes and you all follow along. Also, the title force
around the black holes are very high, so we're talking
about spiglification, which is gonna be very important w to
(00:43):
where we're trying to get to. We're speaking about time
curvature this week. We're also speaking about it's slowing down
of time, and we all know that the density of
what we're speaking about in the what in the space
environment can be calculated by that fact that it's slowing
down uptime. So this is a lot now, so let's
(01:07):
look at this specific star and what we need it
to be so that the outcome could be what we're
looking out.
Speaker 2 (01:18):
Well, well, the calculation the outcome.
Speaker 1 (01:19):
Would be of three things we'll have end up, and
we're gonna do the calculations of each one and what
would bring us there and what that would mean and
how it would have to happen. So we're gonna look
at each one of these now where the ending point
is that it is, because we're talking about lower mass
black holes, it is in two dwarf stars or one
(01:45):
neutron star or a replica star.
Speaker 2 (01:48):
Now.
Speaker 1 (01:49):
So and I know a lot of people are like, well,
that's gonna be quite chaotic. It might be or it
might not be, but we'll be able to do the
math and determine what will cause it to be and
most importantly, what would cause it not to be in
the probability of it not being, and what would cause
that probability.
Speaker 2 (02:06):
So let's go ahead and get started here. So when
were talking about.
Speaker 1 (02:13):
Lower mass black holes, you have to look at the
start itself, specifically and the loss of the outer layers,
because we're trying to get to the core now, because
we're trying to calculate what happens after the obviously more
mass being lost through the stars of evaporation, now, which
(02:34):
would cause it to be.
Speaker 2 (02:36):
A black hole.
Speaker 1 (02:38):
Now we know that with lower mass black holes, the
evacuation process is faster than with high mass black holes.
And I would be obvious, but we know that there
are different degrees of meaning sizes of lower mass black holes,
just like there are different sizes of high mass black holes.
You have to calculate the time that it would take
(02:59):
for that reparation. And also what is around the start
in orbit opposed from just the sign, because what we're
speaking about specifically, it would be there would be core.
Is talking about time curvature. There will obviously be a
massive object in orbit, and we're gonna see how we
got there to that, to that notation of that potentially
(03:23):
being the case.
Speaker 2 (03:25):
Now.
Speaker 1 (03:25):
So first of because we're gonna have to look at particles.
Why well, because we're talking about the loss of the
out of layers of the of the star and getting
down into this core, and because of the tidal forces
around low mass black holes and spotification and what that hapened,
(03:46):
what that creates and the gravitational pull back towards the
core of the start and what that's going to create.
And we stated that the potentials are the two draft
stars or a neutron star or replica start. I'm gonna
state what I mean with replica star, but after the
math is ended. Okay, so that'll be midweek now, because
(04:06):
replica start at CAD. That's gonna be the value dependent
meaning what type of calculations that are gonna be used,
and that could be a replica star can mean whatever
in anything. Now, remember this, this spotification is the most important.
So that's the tidal ways that are already around the start,
(04:26):
and we have to talk about the Obviously we're talking
we're talking about particles in black holes. You're talking about
calculations of well what one would think of as beginnings,
(04:52):
but we were talking about the infinite universe.
Speaker 2 (04:55):
We know that there really.
Speaker 1 (04:56):
Is no beginning, so you at the beginning as what
can be calculated is known for that specific universe or
what obviously we were talking about with the universe that
as we're doing it, we for what fourteen billion years,
but there are many universes. So well, let's talk about
the the law the loss of the outer layers first,
because we want to keep traveling these particles, especially.
Speaker 2 (05:18):
Well we we whatever we're speaking of.
Speaker 1 (05:20):
We're talking about particles here now, and what the particles
consist of their time period, their time period and what
they've graphic gravitation you put towards them that have created
them into something.
Speaker 2 (05:35):
Different.
Speaker 1 (05:36):
So obviously we're talking about the loss of the outer
layers in the in the the through what heat and
that's degree dependent.
Speaker 2 (05:44):
And what is the degree degree dependent on?
Speaker 1 (05:46):
Well, it's degree dependent on the mass of the start
and also the speed of the start. Now it being
a black hole, so it would that would be temperature
dependent and the officers that would have to be calculated also. Now,
so what would that cause where we're talking about supernovas now?
But what type of supernova? Were speaking about LAT supernovas
(06:08):
and we'll get into why well, we'll go ahead and
talk about now while we're talking about LAT supernova's. But
because we remember the outcomes and the numerical values that
we're gonna put here, it's gonna be Well's, it's just
gonna be there, the numerical values, it's gonna be depending
it will be outcome as too supernova type lasts. It
(06:28):
would be two draft stars with this one specifically, why
too well, because as I stated, with the time curvage,
you there's a would be a massive object in orbit
other than the site.
Speaker 2 (06:42):
So this.
Speaker 1 (06:44):
The loss of the out layers in the in the
core heating up, we're talking about supernovas and the energy
being pulled but through spotification, not just gravitational energy be
put being pulled back to the core of the black hole.
We were talking about spotification. So as we comes in
differently and quite warp and that's why we're talking about
(07:06):
the time curvature.
Speaker 2 (07:07):
We're also simply talking about.
Speaker 1 (07:09):
Slowing down in time as an external observational from an
external observational view, but also well we'll wait for that now.
So so let's talk about when when the with the
heating up of the core and what that amits. Now
(07:30):
we're into super and ova where we're talking about lacks
supernova and what they consist of the type of energy
obviously we're talking about. The energy that we're talking about
is about is radiation now, and gamma ray radiation is
what we're speaking of.
Speaker 2 (07:45):
So is.
Speaker 1 (07:48):
The energy that is released into space after the core
heats up. Now, the energy what the energy and the
material that is released in this space after the core
heats up. The energy that will be released in this
the type of energy that will be released in the
space will be gamma ray radiation, will be released in
(08:11):
this space.
Speaker 2 (08:12):
Now.
Speaker 1 (08:12):
That's highly important now in the type of material that
will be released in the space will be dependent upon
the type of start that we're talking about now, and
we calculate the type of stuff story you're talking about,
we'll have to calculate the mass obviously or their lower
mass start lower mass black holes, so we're talking about
(08:33):
talking about calculating colwer mask and just different degrees of
lower mass. Also, the density will have to be calculated.
And also we'll be looking at whatever it is time
coded within the particles which we're gonna be a part
of the material that's released out into the.
Speaker 2 (08:50):
That will be released out in this space now.
Speaker 1 (08:53):
And remember this material that's released out out into into space,
it is gonna be changed, and that's their most important
part of it is gonna be changed. But it's gonna
be changed through spogification, which is very important because we're talking.
Speaker 2 (09:06):
About the gravitational pull back into the core of the.
Speaker 1 (09:08):
Black hole now, knowing and we know that black holes
don't emit light, but we're gonna see that how that
could potentially be, how they could potentially.
Speaker 2 (09:27):
Take in light and admit.
Speaker 1 (09:29):
It because of the type of supernova we're speaking of
the type of spogification they will be going through, and
that's the that they will be going through after their
material and the images released out into space. And it's
gonna orbit be within the orbit of the UH, be
(09:49):
within the orbit of the black hole. And also it's
gonna be dependent because there are there's a massive object
that it could be equal to the Sun, but we
that has to be calculated also. Or it could be
equal to the Sun, that would be or in orbit
equal to its sign that would be an orbit.
Speaker 2 (10:13):
Or similar.
Speaker 1 (10:16):
To its sun coast over there. It's gonna have to
be this distance that is calculated.
Speaker 2 (10:23):
For that also. So listen, So we talked about the
type of.
Speaker 1 (10:27):
Energy that will be released. Now we're talking about gamma
gamma ray radiation here and the type of material, the
type of material is gonna be the what the type
of material is gonna be dependent on and how can
(10:50):
we come in with this figure.
Speaker 2 (10:52):
Well, but this is how we can come in with
the figure with the outcome.
Speaker 1 (10:56):
Now with the outcome of it being two draw stars,
one star or neutribe, okay, and then we always we
could calculate the material that will be released into space
along with the the the energy in that orbit around
(11:16):
the around the black hole, around the start in that spotification.
So that could tell a lot about the type of
material that was released through the core.
Speaker 2 (11:27):
Heating up.
Speaker 1 (11:30):
And losing is the loss of its is of layers.
But remember during the process the loss of the ISLA layers,
the mass is also lost also, so it kind of
changes the particles that are released. And also they go
through a significant change once they're released, they go through spotification,
so that's if it changes them. And staying within orbit
(11:53):
as obviously staying within orbit because of whatever the time
curve that you're here, and this some type of massive
object would be in orbit that would change it. So
there would be some type of emitting of some type
(12:15):
of other energy other than gamma ray is what I'm
getting here. So we'll have to calculate what that energy is,
what that energy would consist of, and it would be
coming from the massive object that will be in orbit.
Speaker 2 (12:38):
We will be able to calculate that by the outcome. Still,
it's like everything just goes by.
Speaker 1 (12:46):
Well, the three outcomes here as I say, the two
draw star, neutron star, or a replica start. Because even
with w even when we when when we're speaking of
the energy released and the material which is the material
(13:08):
is a big question mark here you put a value there,
put a put a but put a value there where
material could be that would take you to the I
the outcome two drawing stars, a neutron star or a
repl the start because we're talking about uh, the the.
Speaker 2 (13:24):
The the black hole that start becoming.
Speaker 1 (13:27):
Auh, a star that emits lights, but it's through the gravity,
potional pull or being able to pull like in due
to spotification that.
Speaker 2 (13:35):
It goes through by what is or in around it.
Speaker 1 (13:39):
Now, So if we if if we talk about particle
collision and because obviously that's what would be happening while
wa why would particle collision be happening, Well, part of
the collision collision would be happening because, as you are
well know, because of because the start when as it
start itself loses its.
Speaker 2 (13:56):
Core, loss of the outer layers.
Speaker 1 (14:01):
In releasing energy and material into the into the into
space it orbiting around it. Because spotification has to happen
because with low mass stars, as we more low mass
black holes, as we will know that there's that strong
title force is title force is stronger than that that
it is with with high mass black holes, so there
(14:25):
will be that particle collision there. So with that type
of particle colision, take it into account the time curvature,
which is due to what whatever uh large object massive
object will be in orbit. Also, while I I D
particilarly be two the Sun and one at a distance
(14:49):
that is close enough to have its it's something where
a particle range could be here because it's gonna take
us into quantum fluctuations, so we'll be converted there to
(15:12):
be a conversion of energy into particles. Because remember we're
pulling part we're pulling particle back into the core.
Speaker 2 (15:20):
Of the black hoble.
Speaker 1 (15:22):
After the after mass has been lost and the and
the loss of the ODO lader are there, and enough
has the enough time that has passed, and you calculating
time also of this start here, enough time has passed
whereas it's lost enough of the out of layer so
that it's obviously it would not be heaven to being
(15:43):
able to bring in light or emit light. But because
of spotification, the potential of that and the and also
because they've been becoming a supernova lapse now, so it
would be the potential of what it could bring into it.
(16:06):
And this the the spin factor here. There's a spin
factor here, so so this will be heat dependent. It
(16:39):
would be heat dependent because the as did as did
as the mass is being lost through evaporation and there's
a spin. There's a spin now speed of spink. It's
(17:02):
shrinking to what is to what they wouldn't need to
shrink and then there would be a spin enough mass
would need to be lost to be able to pull
(17:29):
towards it. What the what the particle has changed into
doing spotification, So that's what we will that's where the
(17:56):
this type of.
Speaker 2 (17:59):
Phenomenal would become like it would be like what one
would it expect.
Speaker 1 (18:05):
It was a big like chaotic, but not really because
the the because it would be but not really, but
it would be obviously shift and change. It would be
it would be shifting change, but that would be a
given with the spotification. It would but it would be.
Speaker 2 (18:34):
It's it, but it's.
Speaker 1 (18:35):
Mass and density dependent of the what one would look
at as chaos, and also it would be dependent upon
the start self, the black hole itself and its age
(19:04):
and also the type of material and with what it
released in this space.
Speaker 2 (19:14):
And it's it's not.
Speaker 1 (19:18):
And then what is already orbited around it does it
does not this type of part of polition.
Speaker 2 (19:24):
It doesn't grow in size, it changes, it bends, it
(19:46):
would bend.
Speaker 1 (19:55):
And when whenever we're talking about time curvature it is
that does then a type of cast. But that type
of chaos is dependent upon is mass and density dependent
is the obviously the laws of gravity depending on what
type of what universe for speaking of the laws of physics,
(20:16):
excuse me, depending on what universe we're speaking of, and
also depending on whatever is in orbit that is massive.
Speaker 2 (20:24):
That it will also be drawing particle and energy from.
Speaker 1 (20:30):
What that particle would consist of, but their energy will
consist of what this spogification creates, which will be uniform
with the curvature, with the time curvature and the stars mass.
Speaker 2 (20:44):
Now after it's.
Speaker 1 (20:45):
Become a supernova, and it's because we know that the
lord mass Black holds they don't have a strong gravitational pull,
but when they go through spoglification, it doesn't need to
be strong. With this case, especially with the outcomets being well,
the two draws stars or a new charge star or
replica star that obviously doesn't give off light.
Speaker 2 (21:05):
It can't doesn't admit light or can't receive it.
Speaker 1 (21:08):
But we're through spot spotification as a sensue that it
can't and through a type of rotational spinning and dependent
upon the the massive object that.
Speaker 2 (21:18):
Is in the orbit around and there could petentially be
two with this case because.
Speaker 1 (21:22):
World War two, because of whatever the conversion of particles
are with these types of with this type of fluctuation here.
Speaker 2 (21:56):
It would be.
Speaker 1 (21:57):
It would be all dependent upon that because even if
we talk about maybe sometimes what could be and then
(22:18):
the this would have to be calculated by the w
W what materials in the atmosphere and how will we
work knewn what value would you put in there numerically?
Well the outcome okay now it w and why how
the outcome can be drawn neutron store to dry stores
rep star unless you know about.
Speaker 2 (22:33):
Material that's orbiting around now it is the.
Speaker 1 (22:38):
The So sometimes the massive object in orbit could be
it could be as well, it could be.
Speaker 2 (22:50):
Cluster galaxies and know why that that those are h
it's a high likelihood where you're talking about uh talking
when you're.
Speaker 1 (23:06):
Speaking of lower massive black holes. Wise, the high likelihood
of cl couster galaxies because the the lower mass black holes,
they have a low or weak they have a very
weak gravitational pull because.
Speaker 2 (23:20):
The density is very low.
Speaker 1 (23:21):
So but there's usually around there, there's a there are
there are massive objects around them, and it's more highly
unlikely that they would there the obviously the MA there
w W, one massive object will around them would have
a high grational uh g gravitational pull, so it could
pull coastal galaxies around. And you're you're already talking about
(23:43):
material that is already attracted to dis orbit, but would
be attracted to whatever the massive objects are that are
in orbit, but closer enough, and because we're talking, we
(24:09):
know we're gonna talk about distance close enough in distance
to pull in emissions, pull in emissions.
Speaker 2 (24:28):
Of the loss of the outer layer, and also to.
Speaker 1 (24:37):
Be part of the spotification, because these title forces are
very strong around these around lord density black holes, lord
mass black holes. And and then and then that would
(24:58):
be this would be the highly likely the outcome of
replica star neutron start in two or two draw stars
in the in the the they're drawn in light after
spotification has happened. Because with this spotification and what that
(25:19):
would consist of, and we talked about it, it would
be the particles in orbit and and also their material
and the energy release from the start from the black
hole here and then this this massive object in orbit.
It would be highly inclusive that galaxy clusters are within
the orbit.
Speaker 2 (25:36):
But then would they could be at where if we're
talking about.
Speaker 1 (25:40):
Distance, well, this is what we capitulated based on the
type of outcomes it would be. Also everything is depending
on the outcome.
Speaker 2 (25:52):
Here now is if if we're talking about galaxy clusters
and light.
Speaker 1 (26:03):
And we're talking.
Speaker 2 (26:04):
About this here.
Speaker 1 (26:07):
Lower mass black holes not emitting like or not taking
in light, but we're talking about spotification and warped change
and curvature time curvature.
Speaker 2 (26:24):
Here the a super cluster of galaxies.
Speaker 1 (26:34):
Would and then they and you're talking about distance, they
if we're speaking about distance, it it doesn't have to
be well, would you distance had to be calculating, cause
(26:54):
we could say something is.
Speaker 2 (26:55):
Near, but it could be l light years away. It
could it could when we're talking about instance, it doesn't
have to be.
Speaker 1 (27:10):
In orbit. When we're speaking of super clusses and in
light and in in spocification, cause it's it's gonna pull it,
it's gonna pull it in. Now, it's gonna pulls it
(27:32):
towards the the the the lower mass black hole and
it and it creates the the the replica star neutron
star in two draws stars. It can would be highly
likely that.
Speaker 2 (27:46):
That would have to.
Speaker 1 (27:50):
Be applied here. But even with that type of particle collision,
it w it would not the this the start itself
would not grow in sauce. That's why the outcome would
(28:10):
be that would be there's a value here, figure number value.
Speaker 2 (28:17):
The numerical value would be that would that as the.
Speaker 1 (28:20):
Outcome would be the likely two draw stars cause they're
growing in sauce.
Speaker 2 (28:24):
It would happen even with the collision.
Speaker 1 (28:25):
Replica start, newtra store because the stratifications it changes and
warps it. It changes and warps it. And that's what
the the chaos with this type of that's where the
chaos where this type of theory comes in, because that's
what it would create. It would create a type of.
Speaker 2 (28:47):
It.
Speaker 1 (28:47):
It's u U not even it would it even be
a chaos which would be expected and thought of with
this type of theory, but it would it would be
also created. It's just a du a different type of phenomenon.
There is what it is, okay. But when we're gonna
get deeper into this during the week, we'll see where
our numbers take us, cause it obviously it will.
Speaker 2 (29:05):
Evolve there the it w it would evolve us on
the table here.
Speaker 1 (29:12):
And I'll be also including this in my in my
writings and expanding on it's okay if one of the
next kind of things for listening, that's the Morning Round
with for Monday, September sixteenth by
Happy one and welcome back to the morning ground. But
we are alive once again. It is Monday, September sixteenth.
Those that want to join in with me on the chat,
you're most welcome to do. So let's see what we're
speaking about this week later material on the table. Midweek,
we'll look at our math and see where that takes us,
cause it will be most definitely informative, and we'll see
(00:21):
what things what things evolve into. So we're looking at
lower mass black holes and remember what lower mass black
holes and you all follow along. Also, the title force
around the black holes are very high, so we're talking
about spiglification, which is gonna be very important w to
(00:43):
where we're trying to get to. We're speaking about time
curvature this week. We're also speaking about it's slowing down
of time, and we all know that the density of
what we're speaking about in the what in the space
environment can be calculated by that fact that it's slowing
down uptime. So this is a lot now, so let's
(01:07):
look at this specific star and what we need it
to be so that the outcome could be what we're
looking out.
Speaker 2 (01:18):
Well, well, the calculation the outcome.
Speaker 1 (01:19):
Would be of three things we'll have end up, and
we're gonna do the calculations of each one and what
would bring us there and what that would mean and
how it would have to happen. So we're gonna look
at each one of these now where the ending point
is that it is, because we're talking about lower mass
black holes, it is in two dwarf stars or one
(01:45):
neutron star or a replica star.
Speaker 2 (01:48):
Now.
Speaker 1 (01:49):
So and I know a lot of people are like, well,
that's gonna be quite chaotic. It might be or it
might not be, but we'll be able to do the
math and determine what will cause it to be and
most importantly, what would cause it not to be in
the probability of it not being, and what would cause
that probability.
Speaker 2 (02:06):
So let's go ahead and get started here. So when
were talking about.
Speaker 1 (02:13):
Lower mass black holes, you have to look at the
start itself, specifically and the loss of the outer layers,
because we're trying to get to the core now, because
we're trying to calculate what happens after the obviously more
mass being lost through the stars of evaporation, now, which
(02:34):
would cause it to be.
Speaker 2 (02:36):
A black hole.
Speaker 1 (02:38):
Now we know that with lower mass black holes, the
evacuation process is faster than with high mass black holes.
And I would be obvious, but we know that there
are different degrees of meaning sizes of lower mass black holes,
just like there are different sizes of high mass black holes.
You have to calculate the time that it would take
(02:59):
for that reparation. And also what is around the start
in orbit opposed from just the sign, because what we're
speaking about specifically, it would be there would be core.
Is talking about time curvature. There will obviously be a
massive object in orbit, and we're gonna see how we
got there to that, to that notation of that potentially
(03:23):
being the case.
Speaker 2 (03:25):
Now.
Speaker 1 (03:25):
So first of because we're gonna have to look at particles.
Why well, because we're talking about the loss of the
out of layers of the of the star and getting
down into this core, and because of the tidal forces
around low mass black holes and spotification and what that hapened,
(03:46):
what that creates and the gravitational pull back towards the
core of the start and what that's going to create.
And we stated that the potentials are the two draft
stars or a neutron star or replica start. I'm gonna
state what I mean with replica star, but after the
math is ended. Okay, so that'll be midweek now, because
(04:06):
replica start at CAD. That's gonna be the value dependent
meaning what type of calculations that are gonna be used,
and that could be a replica star can mean whatever
in anything. Now, remember this, this spotification is the most important.
So that's the tidal ways that are already around the start,
(04:26):
and we have to talk about the Obviously we're talking
we're talking about particles in black holes. You're talking about
calculations of well what one would think of as beginnings,
(04:52):
but we were talking about the infinite universe.
Speaker 2 (04:55):
We know that there really.
Speaker 1 (04:56):
Is no beginning, so you at the beginning as what
can be calculated is known for that specific universe or
what obviously we were talking about with the universe that
as we're doing it, we for what fourteen billion years,
but there are many universes. So well, let's talk about
the the law the loss of the outer layers first,
because we want to keep traveling these particles, especially.
Speaker 2 (05:18):
Well we we whatever we're speaking of.
Speaker 1 (05:20):
We're talking about particles here now, and what the particles
consist of their time period, their time period and what
they've graphic gravitation you put towards them that have created
them into something.
Speaker 2 (05:35):
Different.
Speaker 1 (05:36):
So obviously we're talking about the loss of the outer
layers in the in the the through what heat and
that's degree dependent.
Speaker 2 (05:44):
And what is the degree degree dependent on?
Speaker 1 (05:46):
Well, it's degree dependent on the mass of the start
and also the speed of the start. Now it being
a black hole, so it would that would be temperature
dependent and the officers that would have to be calculated also. Now,
so what would that cause where we're talking about supernovas now?
But what type of supernova? Were speaking about LAT supernovas
(06:08):
and we'll get into why well, we'll go ahead and
talk about now while we're talking about LAT supernova's. But
because we remember the outcomes and the numerical values that
we're gonna put here, it's gonna be Well's, it's just
gonna be there, the numerical values, it's gonna be depending
it will be outcome as too supernova type lasts. It
(06:28):
would be two draft stars with this one specifically, why
too well, because as I stated, with the time curvage,
you there's a would be a massive object in orbit
other than the site.
Speaker 2 (06:42):
So this.
Speaker 1 (06:44):
The loss of the out layers in the in the
core heating up, we're talking about supernovas and the energy
being pulled but through spotification, not just gravitational energy be
put being pulled back to the core of the black hole.
We were talking about spotification. So as we comes in
differently and quite warp and that's why we're talking about
(07:06):
the time curvature.
Speaker 2 (07:07):
We're also simply talking about.
Speaker 1 (07:09):
Slowing down in time as an external observational from an
external observational view, but also well we'll wait for that now.
So so let's talk about when when the with the
heating up of the core and what that amits. Now
(07:30):
we're into super and ova where we're talking about lacks
supernova and what they consist of the type of energy
obviously we're talking about. The energy that we're talking about
is about is radiation now, and gamma ray radiation is
what we're speaking of.
Speaker 2 (07:45):
So is.
Speaker 1 (07:48):
The energy that is released into space after the core
heats up. Now, the energy what the energy and the
material that is released in this space after the core
heats up. The energy that will be released in this
the type of energy that will be released in the
space will be gamma ray radiation, will be released in
(08:11):
this space.
Speaker 2 (08:12):
Now.
Speaker 1 (08:12):
That's highly important now in the type of material that
will be released in the space will be dependent upon
the type of start that we're talking about now, and
we calculate the type of stuff story you're talking about,
we'll have to calculate the mass obviously or their lower
mass start lower mass black holes, so we're talking about
(08:33):
talking about calculating colwer mask and just different degrees of
lower mass. Also, the density will have to be calculated.
And also we'll be looking at whatever it is time
coded within the particles which we're gonna be a part
of the material that's released out into the.
Speaker 2 (08:50):
That will be released out in this space now.
Speaker 1 (08:53):
And remember this material that's released out out into into space,
it is gonna be changed, and that's their most important
part of it is gonna be changed. But it's gonna
be changed through spogification, which is very important because we're talking.
Speaker 2 (09:06):
About the gravitational pull back into the core of the.
Speaker 1 (09:08):
Black hole now, knowing and we know that black holes
don't emit light, but we're gonna see that how that
could potentially be, how they could potentially.
Speaker 2 (09:27):
Take in light and admit.
Speaker 1 (09:29):
It because of the type of supernova we're speaking of
the type of spogification they will be going through, and
that's the that they will be going through after their
material and the images released out into space. And it's
gonna orbit be within the orbit of the UH, be
(09:49):
within the orbit of the black hole. And also it's
gonna be dependent because there are there's a massive object
that it could be equal to the Sun, but we
that has to be calculated also. Or it could be
equal to the Sun, that would be or in orbit
equal to its sign that would be an orbit.
Speaker 2 (10:13):
Or similar.
Speaker 1 (10:16):
To its sun coast over there. It's gonna have to
be this distance that is calculated.
Speaker 2 (10:23):
For that also. So listen, So we talked about the
type of.
Speaker 1 (10:27):
Energy that will be released. Now we're talking about gamma
gamma ray radiation here and the type of material, the
type of material is gonna be the what the type
of material is gonna be dependent on and how can
(10:50):
we come in with this figure.
Speaker 2 (10:52):
Well, but this is how we can come in with
the figure with the outcome.
Speaker 1 (10:56):
Now with the outcome of it being two draw stars,
one star or neutribe, okay, and then we always we
could calculate the material that will be released into space
along with the the the energy in that orbit around
(11:16):
the around the black hole, around the start in that spotification.
So that could tell a lot about the type of
material that was released through the core.
Speaker 2 (11:27):
Heating up.
Speaker 1 (11:30):
And losing is the loss of its is of layers.
But remember during the process the loss of the ISLA layers,
the mass is also lost also, so it kind of
changes the particles that are released. And also they go
through a significant change once they're released, they go through spotification,
so that's if it changes them. And staying within orbit
(11:53):
as obviously staying within orbit because of whatever the time
curve that you're here, and this some type of massive
object would be in orbit that would change it. So
there would be some type of emitting of some type
(12:15):
of other energy other than gamma ray is what I'm
getting here. So we'll have to calculate what that energy is,
what that energy would consist of, and it would be
coming from the massive object that will be in orbit.
Speaker 2 (12:38):
We will be able to calculate that by the outcome. Still,
it's like everything just goes by.
Speaker 1 (12:46):
Well, the three outcomes here as I say, the two
draw star, neutron star, or a replica start. Because even
with w even when we when when we're speaking of
the energy released and the material which is the material
(13:08):
is a big question mark here you put a value there,
put a put a but put a value there where
material could be that would take you to the I
the outcome two drawing stars, a neutron star or a
repl the start because we're talking about uh, the the.
Speaker 2 (13:24):
The the black hole that start becoming.
Speaker 1 (13:27):
Auh, a star that emits lights, but it's through the gravity,
potional pull or being able to pull like in due
to spotification that.
Speaker 2 (13:35):
It goes through by what is or in around it.
Speaker 1 (13:39):
Now, So if we if if we talk about particle
collision and because obviously that's what would be happening while
wa why would particle collision be happening, Well, part of
the collision collision would be happening because, as you are
well know, because of because the start when as it
start itself loses its.
Speaker 2 (13:56):
Core, loss of the outer layers.
Speaker 1 (14:01):
In releasing energy and material into the into the into
space it orbiting around it. Because spotification has to happen
because with low mass stars, as we more low mass
black holes, as we will know that there's that strong
title force is title force is stronger than that that
it is with with high mass black holes, so there
(14:25):
will be that particle collision there. So with that type
of particle colision, take it into account the time curvature,
which is due to what whatever uh large object massive
object will be in orbit. Also, while I I D
particilarly be two the Sun and one at a distance
(14:49):
that is close enough to have its it's something where
a particle range could be here because it's gonna take
us into quantum fluctuations, so we'll be converted there to
(15:12):
be a conversion of energy into particles. Because remember we're
pulling part we're pulling particle back into the core.
Speaker 2 (15:20):
Of the black hoble.
Speaker 1 (15:22):
After the after mass has been lost and the and
the loss of the ODO lader are there, and enough
has the enough time that has passed, and you calculating
time also of this start here, enough time has passed
whereas it's lost enough of the out of layer so
that it's obviously it would not be heaven to being
(15:43):
able to bring in light or emit light. But because
of spotification, the potential of that and the and also
because they've been becoming a supernova lapse now, so it
would be the potential of what it could bring into it.
(16:06):
And this the the spin factor here. There's a spin
factor here, so so this will be heat dependent. It
(16:39):
would be heat dependent because the as did as did
as the mass is being lost through evaporation and there's
a spin. There's a spin now speed of spink. It's
(17:02):
shrinking to what is to what they wouldn't need to
shrink and then there would be a spin enough mass
would need to be lost to be able to pull
(17:29):
towards it. What the what the particle has changed into
doing spotification, So that's what we will that's where the
(17:56):
this type of.
Speaker 2 (17:59):
Phenomenal would become like it would be like what one
would it expect.
Speaker 1 (18:05):
It was a big like chaotic, but not really because
the the because it would be but not really, but
it would be obviously shift and change. It would be
it would be shifting change, but that would be a
given with the spotification. It would but it would be.
Speaker 2 (18:34):
It's it, but it's.
Speaker 1 (18:35):
Mass and density dependent of the what one would look
at as chaos, and also it would be dependent upon
the start self, the black hole itself and its age
(19:04):
and also the type of material and with what it
released in this space.
Speaker 2 (19:14):
And it's it's not.
Speaker 1 (19:18):
And then what is already orbited around it does it
does not this type of part of polition.
Speaker 2 (19:24):
It doesn't grow in size, it changes, it bends, it
(19:46):
would bend.
Speaker 1 (19:55):
And when whenever we're talking about time curvature it is
that does then a type of cast. But that type
of chaos is dependent upon is mass and density dependent
is the obviously the laws of gravity depending on what
type of what universe for speaking of the laws of physics,
(20:16):
excuse me, depending on what universe we're speaking of, and
also depending on whatever is in orbit that is massive.
Speaker 2 (20:24):
That it will also be drawing particle and energy from.
Speaker 1 (20:30):
What that particle would consist of, but their energy will
consist of what this spogification creates, which will be uniform
with the curvature, with the time curvature and the stars mass.
Speaker 2 (20:44):
Now after it's.
Speaker 1 (20:45):
Become a supernova, and it's because we know that the
lord mass Black holds they don't have a strong gravitational pull,
but when they go through spoglification, it doesn't need to
be strong. With this case, especially with the outcomets being well,
the two draws stars or a new charge star or
replica star that obviously doesn't give off light.
Speaker 2 (21:05):
It can't doesn't admit light or can't receive it.
Speaker 1 (21:08):
But we're through spot spotification as a sensue that it
can't and through a type of rotational spinning and dependent
upon the the massive object that.
Speaker 2 (21:18):
Is in the orbit around and there could petentially be
two with this case because.
Speaker 1 (21:22):
World War two, because of whatever the conversion of particles
are with these types of with this type of fluctuation here.
Speaker 2 (21:56):
It would be.
Speaker 1 (21:57):
It would be all dependent upon that because even if
we talk about maybe sometimes what could be and then
(22:18):
the this would have to be calculated by the w
W what materials in the atmosphere and how will we
work knewn what value would you put in there numerically?
Well the outcome okay now it w and why how
the outcome can be drawn neutron store to dry stores
rep star unless you know about.
Speaker 2 (22:33):
Material that's orbiting around now it is the.
Speaker 1 (22:38):
The So sometimes the massive object in orbit could be
it could be as well, it could be.
Speaker 2 (22:50):
Cluster galaxies and know why that that those are h
it's a high likelihood where you're talking about uh talking
when you're.
Speaker 1 (23:06):
Speaking of lower massive black holes. Wise, the high likelihood
of cl couster galaxies because the the lower mass black holes,
they have a low or weak they have a very
weak gravitational pull because.
Speaker 2 (23:20):
The density is very low.
Speaker 1 (23:21):
So but there's usually around there, there's a there are
there are massive objects around them, and it's more highly
unlikely that they would there the obviously the MA there
w W, one massive object will around them would have
a high grational uh g gravitational pull, so it could
pull coastal galaxies around. And you're you're already talking about
(23:43):
material that is already attracted to dis orbit, but would
be attracted to whatever the massive objects are that are
in orbit, but closer enough, and because we're talking, we
(24:09):
know we're gonna talk about distance close enough in distance
to pull in emissions, pull in emissions.
Speaker 2 (24:28):
Of the loss of the outer layer, and also to.
Speaker 1 (24:37):
Be part of the spotification, because these title forces are
very strong around these around lord density black holes, lord
mass black holes. And and then and then that would
(24:58):
be this would be the highly likely the outcome of
replica star neutron start in two or two draw stars
in the in the the they're drawn in light after
spotification has happened. Because with this spotification and what that
(25:19):
would consist of, and we talked about it, it would
be the particles in orbit and and also their material
and the energy release from the start from the black
hole here and then this this massive object in orbit.
It would be highly inclusive that galaxy clusters are within
the orbit.
Speaker 2 (25:36):
But then would they could be at where if we're
talking about.
Speaker 1 (25:40):
Distance, well, this is what we capitulated based on the
type of outcomes it would be. Also everything is depending
on the outcome.
Speaker 2 (25:52):
Here now is if if we're talking about galaxy clusters
and light.
Speaker 1 (26:03):
And we're talking.
Speaker 2 (26:04):
About this here.
Speaker 1 (26:07):
Lower mass black holes not emitting like or not taking
in light, but we're talking about spotification and warped change
and curvature time curvature.
Speaker 2 (26:24):
Here the a super cluster of galaxies.
Speaker 1 (26:34):
Would and then they and you're talking about distance, they
if we're speaking about distance, it it doesn't have to
be well, would you distance had to be calculating, cause
(26:54):
we could say something is.
Speaker 2 (26:55):
Near, but it could be l light years away. It
could it could when we're talking about instance, it doesn't
have to be.
Speaker 1 (27:10):
In orbit. When we're speaking of super clusses and in
light and in in spocification, cause it's it's gonna pull it,
it's gonna pull it in. Now, it's gonna pulls it
(27:32):
towards the the the the lower mass black hole and
it and it creates the the the replica star neutron
star in two draws stars. It can would be highly
likely that.
Speaker 2 (27:46):
That would have to.
Speaker 1 (27:50):
Be applied here. But even with that type of particle collision,
it w it would not the this the start itself
would not grow in sauce. That's why the outcome would
(28:10):
be that would be there's a value here, figure number value.
Speaker 2 (28:17):
The numerical value would be that would that as the.
Speaker 1 (28:20):
Outcome would be the likely two draw stars cause they're
growing in sauce.
Speaker 2 (28:24):
It would happen even with the collision.
Speaker 1 (28:25):
Replica start, newtra store because the stratifications it changes and
warps it. It changes and warps it. And that's what
the the chaos with this type of that's where the
chaos where this type of theory comes in, because that's
what it would create. It would create a type of.
Speaker 2 (28:47):
It.
Speaker 1 (28:47):
It's u U not even it would it even be
a chaos which would be expected and thought of with
this type of theory, but it would it would be
also created. It's just a du a different type of phenomenon.
There is what it is, okay. But when we're gonna
get deeper into this during the week, we'll see where
our numbers take us, cause it obviously it will.
Speaker 2 (29:05):
Evolve there the it w it would evolve us on
the table here.
Speaker 1 (29:12):
And I'll be also including this in my in my
writings and expanding on it's okay if one of the
next kind of things for listening, that's the Morning Round
with for Monday, September sixteenth by
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