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8/13/2019 Linear Coasting
1/39
8/13/2019 Linear Coasting
2/39
Figure:Half-Knowledge- the right of a PhD student!
Rohin Kumar Alternative Models of Cosmology
http://find/8/13/2019 Linear Coasting
3/39
All izz not well with CDM
Background
Well! not really if u dont think
Dark Matter(decel)
Dark Energy (accel)
Inflation (accel)
Age problem
Rohin Kumar Alternative Models of Cosmology
http://find/8/13/2019 Linear Coasting
4/39
All izz not well with CDM
Background
Well! not really if u dont think
Dark Matter(decel)
Dark Energy (accel)
Inflation (accel)
Age problem
Rohin Kumar Alternative Models of Cosmology
http://find/http://goback/8/13/2019 Linear Coasting
5/39
All i t ll ith CDM
8/13/2019 Linear Coasting
6/39
All izz not well with CDM
Background
Well! not really if u dont think
Dark Matter(decel)
Dark Energy (accel)
Inflation (accel)
Age problem
Rohin Kumar Alternative Models of Cosmology
All i t ll ith CDM
http://find/8/13/2019 Linear Coasting
7/39
All izz not well with CDM
Background
Well! not really if u dont think
Dark Matter(decel)
Dark Energy (accel)
Inflation (accel)
Age problem
Rohin Kumar Alternative Models of Cosmology
All i t ll ith CDM
http://find/8/13/2019 Linear Coasting
8/39
All izz not well with CDM
Background
Well! not really if u dont think
Dark Matter(decel)
Dark Energy (accel)
Inflation (accel)
Age problem
Rohin Kumar Alternative Models of Cosmology
Recipes Assumptions
http://find/8/13/2019 Linear Coasting
9/39
Recipes-Assumptions
a(t) =tandk= 1 in FRW metric implies flat space-timeand open space.
Empirical - Power Law solutiona tn
Dirac-Milne Model
Antimatter has negative active gravitational mass.Matter and antimatter are separated in domains (ob)No inflation - but what about Radiation?
Large scale gravity?
We dont know
Rohin Kumar Alternative Models of Cosmology
http://find/8/13/2019 Linear Coasting
10/39
Recipes Assumptions
8/13/2019 Linear Coasting
11/39
Recipes-Assumptions
a(t) =tandk= 1 in FRW metric implies flat space-timeand open space.
Empirical - Power Law solutiona tn
Dirac-Milne Model
Antimatter has negative active gravitational mass.Matter and antimatter are separated in domains (ob)No inflation - but what about Radiation?
Large scale gravity?
We dont know
Rohin Kumar Alternative Models of Cosmology
http://goforward/http://find/http://goback/8/13/2019 Linear Coasting
12/39
Recipes Assumptions
8/13/2019 Linear Coasting
13/39
Recipes-Assumptions
a(t) =tandk= 1 in FRW metric implies flat space-timeand open space.
Empirical - Power Law solutiona tn
Dirac-Milne Model
Antimatter has negative active gravitational mass.Matter and antimatter are separated in domains (ob)No inflation - but what about Radiation?
Large scale gravity?
We dont know
Rohin Kumar Alternative Models of Cosmology
Recipes-Assumptions
http://find/8/13/2019 Linear Coasting
14/39
Recipes-Assumptions
a(t) =tandk= 1 in FRW metric implies flat space-timeand open space.
Empirical - Power Law solutiona tn
Dirac-Milne Model
Antimatter has negative active gravitational mass.Matter and antimatter are separated in domains (ob)No inflation - but what about Radiation?
Large scale gravity?
We dont know
Rohin Kumar Alternative Models of Cosmology
Recipes-Assumptions
http://goforward/http://find/http://goback/8/13/2019 Linear Coasting
15/39
Recipes-Assumptions
a(t) =tandk= 1 in FRW metric implies flat space-timeand open space.
Empirical - Power Law solutiona tn
Dirac-Milne Model
Antimatter has negative active gravitational mass.Matter and antimatter are separated in domains (ob)No inflation - but what about Radiation?
Large scale gravity?
We dont know
Rohin Kumar Alternative Models of Cosmology
http://goforward/http://find/http://goback/8/13/2019 Linear Coasting
16/39
Supernovae Data
8/13/2019 Linear Coasting
17/39
Supernovae Data
There is a remarkable agreement of data with linear model
Figure:Has better2 fit too :)
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/8/13/2019 Linear Coasting
18/39
Nucleosynthesis
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of
4
Heand
7
LiGives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/8/13/2019 Linear Coasting
19/39
Nucleosynthesis
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of
4
Heand
7
LiGives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/http://goback/8/13/2019 Linear Coasting
20/39
Nucleosynthesis
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of
4
Heand
7
LiGives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/8/13/2019 Linear Coasting
21/39
Nucleosynthesis
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of 4Heand 7Li
Gives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/8/13/2019 Linear Coasting
22/39
Nucleosynthesis
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of 4Heand 7Li
Gives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/8/13/2019 Linear Coasting
23/39
y
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of 4Heand 7Li
Gives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
Nucleosynthesis
http://find/8/13/2019 Linear Coasting
24/39
y
time-Temperature relationship is differentt= 1H0
T0T
1MeV 3.3yrs (1 Sec in SBBN)
Weak interaction decoupling happens at 90keV
Slower production of 4Heand 7Li
Gives correct 9 109 values to eliminate needs for
non-baryonic matter such as Dark Matter
Dand 3Heare produced by photodisintegration of 4He
induced by annihilation photons (in D-M model)
Electron screening effects in plain linear coasting
Rohin Kumar Alternative Models of Cosmology
CMB
http://find/http://goback/8/13/2019 Linear Coasting
25/39
Not the same initial conditions (no inflation)
No Dark Matter
Linear Scale factor
Recombination process is almost unchanged (z 1020)but age would be 14 106yrs. instead of 380000 yrs.
Random fluctuations in Pressure and density (local)
Matter-antimatter collisons in D-M model
Rohin Kumar Alternative Models of Cosmology
CMB
http://goforward/http://find/http://goback/8/13/2019 Linear Coasting
26/39
Not the same initial conditions (no inflation)
No Dark Matter
Linear Scale factor
Recombination process is almost unchanged (z 1020)but age would be 14 106yrs. instead of 380000 yrs.
Random fluctuations in Pressure and density (local)
Matter-antimatter collisons in D-M model
Rohin Kumar Alternative Models of Cosmology
CMB
http://goforward/http://find/http://goback/8/13/2019 Linear Coasting
27/39
Not the same initial conditions (no inflation)
No Dark Matter
Linear Scale factor
Recombination process is almost unchanged (z 1020)but age would be 14 106yrs. instead of 380000 yrs.
Random fluctuations in Pressure and density (local)
Matter-antimatter collisons in D-M model
Rohin Kumar Alternative Models of Cosmology
http://find/8/13/2019 Linear Coasting
28/39
CMB
8/13/2019 Linear Coasting
29/39
Not the same initial conditions (no inflation)
No Dark Matter
Linear Scale factor
Recombination process is almost unchanged (z 1020)but age would be 14 106yrs. instead of 380000 yrs.
Random fluctuations in Pressure and density (local)
Matter-antimatter collisons in D-M model
Rohin Kumar Alternative Models of Cosmology
CMB
http://find/8/13/2019 Linear Coasting
30/39
Not the same initial conditions (no inflation)
No Dark Matter
Linear Scale factor
Recombination process is almost unchanged (z 1020)but age would be 14 106yrs. instead of 380000 yrs.
Random fluctuations in Pressure and density (local)
Matter-antimatter collisons in D-M model
Rohin Kumar Alternative Models of Cosmology
http://find/8/13/2019 Linear Coasting
31/39
CMB Contd...
8/13/2019 Linear Coasting
32/39
Angular scale of the first peak corresponds to the angle
under which is seen sound horizon at decoupling
dDM
A (z)
dCDMA (z) 169
=S(z)
dA(z)
RememberS= t
0 cs
dt
a(t) wherecs=
c3(1 +R)
Matter anti-matter collisons(?)
epoch during QGP transition ofT 170MeVAcoustic
waves then propagate in the plasma as long as matter and
antimatter are in contact, i.e. until the gravitational
decouplingz 3 104
With these values, the comoving sound horizon is found to
be 42Gpc
with these values First acoustic peak would be at l 200
which means 10
Rohin Kumar Alternative Models of Cosmology
CMB Contd...
http://find/8/13/2019 Linear Coasting
33/39
Angular scale of the first peak corresponds to the angle
under which is seen sound horizon at decoupling
dDM
A (z)
dCDMA (z) 169
=S(z)
dA(z)
RememberS= t
0 cs
dt
a(t) wherecs=
c3(1 +R)
Matter anti-matter collisons(?)
epoch during QGP transition ofT 170MeVAcoustic
waves then propagate in the plasma as long as matter and
antimatter are in contact, i.e. until the gravitational
decouplingz 3 104
With these values, the comoving sound horizon is found to
be 42Gpc
with these values First acoustic peak would be at l 200
which means 10
Rohin Kumar Alternative Models of Cosmology
http://find/8/13/2019 Linear Coasting
34/39
CMB Contd...
8/13/2019 Linear Coasting
35/39
Angular scale of the first peak corresponds to the angle
under which is seen sound horizon at decoupling
dDM
A (z)
dCDMA (z) 169
=S(z)
dA(z)
RememberS= t
0 cs
dt
a(t) wherecs=
c3(1 +R)
Matter anti-matter collisons(?)
epoch during QGP transition ofT 170MeVAcoustic
waves then propagate in the plasma as long as matter and
antimatter are in contact, i.e. until the gravitational
decouplingz 3 104
With these values, the comoving sound horizon is found to
be 42Gpc
with these values First acoustic peak would be at l 200
which means 10
Rohin Kumar Alternative Models of Cosmology
CMB Contd...
http://find/8/13/2019 Linear Coasting
36/39
Angular scale of the first peak corresponds to the angle
under which is seen sound horizon at decoupling
dDM
A
(z)
dCDMA (z) 169
=S(z)
dA(z)
RememberS=
t
0
cs
dt
a(t)wherec
s=
c3(1 +R)
Matter anti-matter collisons(?)
epoch during QGP transition ofT 170MeVAcoustic
waves then propagate in the plasma as long as matter and
antimatter are in contact, i.e. until the gravitational
decouplingz 3 104
With these values, the comoving sound horizon is found to
be 42Gpc
with these values First acoustic peak would be at l 200
which means
10
Rohin Kumar Alternative Models of Cosmology
CMB Contd...
http://find/8/13/2019 Linear Coasting
37/39
Angular scale of the first peak corresponds to the angle
under which is seen sound horizon at decoupling
dDM
A
(z)
dCDMA (z) 169
=S(z)
dA(z)
RememberS=
t
0
cs
dt
a(t)wherec
s=
c3(1 +R)
Matter anti-matter collisons(?)
epoch during QGP transition ofT 170MeVAcoustic
waves then propagate in the plasma as long as matter and
antimatter are in contact, i.e. until the gravitational
decouplingz 3 104
With these values, the comoving sound horizon is found to
be 42Gpc
with these values First acoustic peak would be at l 200
which means
10
Rohin Kumar Alternative Models of Cosmology
CMB Contd...
http://find/8/13/2019 Linear Coasting
38/39
Angular scale of the first peak corresponds to the angle
under which is seen sound horizon at decoupling
dDM
A
(z)
dCDMA (z) 169
=S(z)
dA(z)
RememberS
= t
0
cs
dt
a(t)wherec
s=
c3(1 +R)
Matter anti-matter collisons(?)
epoch during QGP transition ofT 170MeVAcoustic
waves then propagate in the plasma as long as matter and
antimatter are in contact, i.e. until the gravitational
decouplingz 3 104
With these values, the comoving sound horizon is found to
be 42Gpc
with these values First acoustic peak would be at l 200
which means
10
Rohin Kumar Alternative Models of Cosmology
So now what?
http://find/8/13/2019 Linear Coasting
39/39
I
dont know!
Rohin Kumar Alternative Models of Cosmology
http://find/