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Lecture 6: EDS, Milne and other Universes
1. Omega Notation 2. Time in simple Universes
– The Einstein de Sitter Universe (flat, matter only) – The Milne Universe (empty) – A Radiation Universe (flat, radiation only) – Dark Energy Universe (flat, dark energy only)
3. The Anthropic Principle 4. Distances:
– Einstein de Sitter – Matter and curvature
5. The LOT Universe: - Time - Distances
Course Text: Chapter 4 Wikipedia: Einstein de Sitter, Milne, Dark Matter, Large Scale
Structure
Omega Notation !M =
!M ,o
!crit= !M ,o
8"G3Ho
2
!R =!R,o
!crit= !R,o
8"G3Ho
2
!" =!"!crit
= !"8"G3Ho
2 ="
3Ho2
!K = #kc2
Ro2Ho
2
! =!M +!R +!"
!K =1#!1=!M +!R +!" +!K = FRIEDMANN EQUATION TODAY
!crit =3H0
2
8"G
! >1, implies a high-density Universe!=1, implies a flat Universe!<1, implies a low-density Universe
qo = !!!RR!R2
"
#$
%
&'o
= !!!R!R
"
#$
%
&'o
1Ho
Deceleration parameter, defn: Not used much these days.
Reminder:
Einstein de Sitter Universe • ΩM=1, ΩR=0, ΩΛ=0, i.e., flat (k=0), matter only Universe
• Universe will expand at a decreasing rate forever.
!RR!
"#
$
%&
2
=8!G"
3, and " = "o
RoR
'
()*
+,
3
- !R2 =8!G"oRo
3
31R
Lets try: R. tq - t2q/2 . t/q
Above only valid if: 2q-2=-q, or q=23
i.e., RRo
=tto
'
()
*
+,
23
differentiate to get: !R = 2Ro3to
23t
13
set to today's values and rearrange to get:
to =2
3Ho
0 9Gyrs
• ΩM=0, ΩR=0, ΩΛ=0, i.e., empty, open (k=-1) Universe or Special Relativity case (no mass)
• Universe will expand at a constant rate forever.
– i.e., Infinite size after infinite time.
Milne Universe
!RR!
"#
$
%&
2
=c2
R2
' !R2 = c2
Integrate w.r.t t' R = ±ct i.e., scale factor proprtional to time.
to =1Ho
(13Gyrs
• ΩM>1, ΩR=0, ΩΛ=0, i.e., closed (k=+1), matter only Universe
• Universe will expand to a constant size and then re-collapse
Over-dense Universe
!RR!
"#
$
%&
2
=8!G"
3+c2
R2 , and " = "oRoR
'
()*
+,
3
- !R2 =8!G"oRo
3
31R. c2
i.e., !R = 0 when Rc =8!G"oRo
3
3c2
Radiation only Universe • ΩM=0, ΩR=1, ΩΛ=0, i.e., flat (k=0), radiation only Universe
• Universe will expand at a decreasing rate forever. [Note this was the relation we adopted in Lec 2.]
!RR!
"#
$
%&
2
=8!G"
3, and " = "o
RoR
'
()*
+,
4
- !R2 =8!G"oRo
4
31R2
Lets try: R. tq - t2q/2 . t/2q
Above only valid if: 2q-2=-2q, or q= 12
i.e., RRo
=tto
'
()
*
+,
12
differentiate to get: !R = 1Ro2to
12t
12
set to today's values and rearrange to get:
to =1
2Ho
0 6Gyrs
• ΩM=0, ΩR=0, ΩΛ=1, i.e., flat (k=0), dark energy only Universe
• Universe will expand at an exponential rate forever!
Dark Energy only Universe
!RR!
"#
$
%&
2
=8!G"
3, and " =Constant
' !R2 (R2
i.e., R( et
With Λ
Anthropic Principle • So what is the value of Ω?
‒ ΩΜ+ΩR∼0.01 - 1.0 (e.g., counting mass of galaxies in a volume) – Why so close to 1?
• Anthropic Principle – Weak
Only in a Universe with Ω~1 can life come about to ask the question why Ω~1, hence its no coincidence. ‒ Ω<<1 Universe too diffuse and expanding too fast for
stars/galaxies to form. ‒ Ω>>1 Universe re-collapses before life can evolve.
– Strong Only Universe with Ω~1 are allowed by some as yet undiscovered physics.
– E.g., Inflation (see Lec 8).
Weak Anthropic principle Lots of Universes possible each with very different physics with the laws universal within each bubble. Only those Universe which can support life will puzzle over their good fortune…
Image: James Schombert
Strong Anthropic principle Only one Universe possible, physics to be determined:
Image: James Schombert
Distance in an EdS Universe • ΩM=1, ΩR=0, ΩΛ=0, i.e., flat (k=0), matter only Universe
• What we want is an expression for, dp the proper distance
• To get this we now need to combine R(t) with the metric
!!RR= !
4!G"3
, !RR"
#$
%
&'
2
=8!G"
3, " = "o
RoR
"
#$
%
&'
3
, RRo
=tto
"
#$
%
&'
23
Set t = to, get:
qoHo2 =
4!G"o3
,Ho2 =
8!G"o3
, qo =(M
2= 0.5
Distance in an EdS Universe
0 = c2dt2 ! R2dr2
R2dr2 = c2dt2
dr0
r1
" = c dtRt1
to
"
Consider a photon travelling from some point towards us . RWM reduced to:
Photon starts at r=0 and gets to r1 today
Photon leaves at time t1 and arrives at time to
(dp = Ror1)
R = Rotto
!
"#
$
%&
23
(to =23Ho
)
! r1 =cRoto23 1
t23t1
to
" dt
Distance in an EdS Universe Ror1 = cto
23 1
t2
3t1
to
! dt = cto2
3 3t1
3"#$
%&'t1
to
Ror1 = 3cto2
3 to1
3 ( t11
3"#$
%&'
Ror1 = 3cto 1( t1to
)
*+
,
-.
13"
#
$$
%
&
''
But: to =2
3Ho& t1
to
)
*+
,
-.
2 3
=R1
Ro=
11+ z
/ dp = Ror1 =2cHo
1( 1(1+ z)
12
"
#$$
%
&''
This is the standard EdS solution which most astronomers used to calculate distances for most of the last century (pre-Λ) Remember also:
dl = (1+ z)dp, da =dp
(1+ z)
Distance in an open matter dominated Universe
• From 1990s onwards it was clear ΩM<1 this implied the possibility of an open Universe and we needed, in brief:
!RR!
"#
$
%&
2
=8!G"
3'kc2
R2
At to
Ho2 =
8!G"o3
'kc2
Ro2
1=(M 'kc2
Ho2Ro
2
kc2 = Ho2Ro
2[(M '1]
Subs for kc2into above replace "="oRoR
!
"#
$
%&
3
& divide by Ho2 (Ro R)2
) !R = RoHo[(MRoR'(M +1]
12
dr
[1' kr2 ]1
20
r1
* =cdtRt1
to
* =cRr1
ro
* dR!R
as !R = dR dt
Sub x = RRo
=1
(1+ z)
!dr
[1" kr2 ]1
20
r1
# =cHo1
(1+z)
1
# [$M
x"$M +1]"
12 x"1dx
“It is straightforward to show that…” Cosmology, Weinberg
Translation:
After 20 years of sporadic effort it was shown that:
valid for all k
dp = Ror1 =2cHo
[!Mz+ (!M " 2)( (1+!Mz) "1)!M2 (1+ z)
]
Mattig’s Formulae (1958)
The Lot Universe • In the late 1990s the data favoured a non-zero Λ • The full-monty has no analytic solution but we can
derive the integral following the same route:
1. Start with Friedmann Equation 2. Set variables to todays values 3. Substitute for qo, Ho, ΩM, ΩR, ΩΛ
4. Rearrange to get kc2 5. Sub back into F.E. 6. Express variables in terms of Ro/R 7. Substitute for Ωs 8. Rearrange and tidy to get dR/dt 9. Put into RWM
• Step1: Write down Friedmann equation:
• Step 2: Set to todays values:
• Step 3: Substitute for Ho & Ωs
• Step 4: Rearrange to get kc2
• Step 5: Substitute back into FE
!RR!
"#
$
%&
2
=8!G"3
+'3(kc2
R2
!RR!
"#
$
%&o
2
=8!G"o3
+'3(kc2
Ro2
1=)M +)' (kc2
Ro2Ho
2
kc2 = Ro2Ho
2[)M +)R +)' (1]
!RR!
"#
$
%&
2
=8!G"3
+'3(Ro2Ho
2[)M +)R +)' (1]R2
• Step 6: Express all variables as Ro/R
• Step 7: x by R2/(Ro2Ho
2 ) & sub for Ωs
• Step 8: Rearrange to get dR/dt
• Age of Universe:
• No analytic solution known, good approx =
!RR!
"#
$
%&
2
=8!G"M ,o
3(RoR)3 + 8!G"R,o
3(RoR)4 + '
3(Ro2Ho
2[)M +)R +)' (1]R2
!R2
Ro2Ho
2 =)M ,oRoR+)R,o(
RoR)2 +)' (
RRo)2 ()M ,o ()R,o ()' +1
!R = RoHo[)M ,oRoR+)R,o(
RoR)2 +)' (
RRo)2 ()M ,o ()R,o ()' +1]
12
tage = dt0
t0
! =dR!R0
R0
!
tage =1Ho0
1
! ["M (1+ z)+"R (1+ z)2 +"# (1+ z)
$2 +"k ]$12d 1
(1+ z)
tage =23Ho
[0.7!M + 0.3" 0.3!# ]"0.3 =13Gyrs
Distance R2dr2
1! kr2 = c2dt2
dr
[1! kr2 ]1
2o
r1
" = c dtRt1
to
" = c 1RdR!RR
Ro
"
dr
[1! kr2 ]1
2o
r1
" =c
RoHo
1R
[#M ,oRoR+#R,o(
RoR
)2 +#$ ( RRo
)2 !#M ,o !#R,o !#$ +1]!1
2 dRR1
Ro
"
Rodr
[1! kr2 ]1
2o
r1
" =cHo
(1+ z)!1
1(1+z)
1
" [#M ,o(1+ z)+#R,o(1+ z)2 +#$ (1+ z)!2 +#k ]
!12d 1
(1+ z)
Rodr
[1! kr2 ]1
2o
r1
" =cHo
1[#M ,o(1+ z)
3 +#R,o(1+ z)4 +#$ +#k (1+ z)
2 ]1(1+z)
1
" d 1(1+ z)
Where: dp = Ror1
Messy, but easy to evaluate on a computer. This is the expression we all use today, made a little easier because k=0
Distances in cosmology
Luminosity distance Angular diameter distance