In General > s.a. astronomy; early
universe; matter.
* 1995: The dogma is
b
0.05,
dm
0.95,
cc =
0.
* 1998: M Turner & D
Schramm predict 5% ordinary matter, based on deuterium abundance.
* 1999: "Matter" consists
of ordinary matter/radiation (
0.2),
dark matter, and dark energy (possibly a cosmological constant).
* 2000: Cold dark matter
from new cmb data; Favored values
m
0.4
0.1,
b
= 0.02 h–2, 0.001 <
nu < 0.1,
cc
0.7.
* 2001: New DASI and Boomerang cmb data; Favored values
b
= 0.05,
dm =
0.30,
de
= 0.65 (p < 0).
* 2002: 2dF galaxy redshift survey and cmb,
m =
1 –
cc =
0.30; Using KamLAND data,
nu
0.070 h–2.
* 2003: WMAP data give
b
= 0.04,
dm =
0.23,
de =
0.73; SDSS data,
b
= 0.05,
dm
= 0.25,
de
= 0.70.
* 2003:
CDM
provides best fit to data, with
tot =
1.02
0.02.
* Critical density: At the present time,
crit =
6 H atoms/m3 = 10–26 kg/m3;
Notice that
cc =
c2/3H02.
* Entropy: The entropy of the universe is low but increasing.
@ Matter content: Melott PRP(90);
Persic & Salucci MNRAS(92)ap/05 [baryons];
Bahcall ap/96 [large-scale
structure]; White ap/96-in
[large z];
Dolgov ap/02-in, ap/02-in
[antimatter]; Krauss & Scherrer PRD(07)ap [radiation
cannot become dominant again].
@ Density: Coles & Ellis Nat(94)aug,
97; Bahcall & Fan PNAS(98)ap;
Krauss
hp/98-in [cosmological constant];
Bahcall PS(00)ap/99-in
[galaxy clusters]; Roos & Harun-or-Rashid ap/00, ap/00 [flatness];
Turner ApJL(02)ap/01;
Schindler ap/01-in
[
m];
Waterhouse & Zibin a0804 [variation of
].
Magnetic Fields > s.a. astronomical
phenomena.
* Theoretically: A universal
magnetic field has been proposed as a way of avoiding the initial singularity
in some cases; It also favors formation
of structure in the universe.
* And observation: There
seem to be Mpc-scale, 10–7–10–5-G
magnetic fields in all galaxies and clusters, possibly arising from differential
rotation
and helical turbulence, but their origin is not totally clear; Search
for a universal magnetic field so far has been inconclusive,
and it
does not seem to be favorred by many.
@ General: Enqvist IJMPD(98)ap,
Carroll & Field ap/98-in,
Field & Carroll PRD(00)ap/98 [primordial];
Hogan ap/00 [from
recombination]; Gasperini PRD(01)ap/00 [seeds,
theory]; Tsagas gq/01-in
[coupling to geometry]; Clarkson et al CQG(03)ap/02 [from
cmb]; Shukla PS(05)
[origin]; de Gouveia Dal Pino ap/06-in.
@ Galactic and intergalactic: Anchordoqui & Goldberg PRD(02)hp/01 [extragalactic,
local]; Kronberg PT(02)dec;
Giovannini IJMPD(04)ap/03 [th,
review]; Dar & De Rújula PRD(05)ap [theory]; > s.a. astronomical
objects.
@ Early universe: Davidson PLB(96); Grasso & Rubinstein PRP(01).
@ UMF: in Olivo-Melchiorri & Melchiorri RNC(85) & refs.
Types of Matter > s.a. dark
matter; electroweak
theory;
inflationary scenarios; quantum
field theory in curved spacetime; topological
defects.
* Components: Ordinary "baryonic" matter, dark matter, "dark
energy" (possibly
a cosmological constant).
* Cosmic IR background:
One motivation to study it is to learn more about population III stars, whole
light is now mostly IR.
@ Reviews: Dine ht/01-in;
Durrer ap/02-in;
Fukugita & Peebles ApJ(04)ap [energy
inventory].
@ Repulsive matter: Cornish & Starkman ap/98; > s.a. dark
energy.
@ Mirror matter: Foot PLB(99)ap [stars?],
PLB(99)ap [planets?];
Mohapatra & Teplitz
PLB(99)ap [MACHOs?];
Foot & Mitra
APP(03)ap/02 [Solar
System]; Foot & Silagadze IJMPD(05)
[supernovas and GRB's]; Ciarcelluti IJMPD(05), IJMPD(05).
@ Cosmic IR background: news pn(98)jan;
Biller et al PRL(98)
[limits]; Kashlinsky PRP(05)ap/04;
Fernandez & Komatsu ApJ(06)ap/05
[near IR]; Lagache et al ap/05-in
[sources]; Kashlinsky et al ApJL(07)ap/06
[sources].
@ Cosmic 21-cm background: Cooray PRD(06)
[and e scattering]; Kleban et al JCAP(07)ht,
Wyithe & Loeb a0708-MNRAS
[fluctuations];
Loeb JCAP(08)-a0801 [validity
of classical treatment]; Metcalf a0801-in
[gravitational lensing]; Pritchard & Loeb a0802-PRD
[evolution]; Pen et al a0802-MNRAS
[detection of structure]; > s.a. observational
cosmology;
perturbations.
@ Other diffuse background: Henry ap/99;
Lagache et al ASS(99)ap [sub-mm]; > s.a. cmb; gamma
rays; gravitons; neutrinos.
Matter Distribution > s.a. galaxy
distribution; perturbations;
relativistic cosmology;
quantum cosmology.
* Idea: Luminous matter has a roughly fractal distribution up to 15–20
Mpc, while radiation is much more homogeneous and isotropic; They are distributed
approximately the same way at galaxy cluster scales, and are possibly
homogeneous
on larger, super-horizon scales; We don't know why.
* Fluctuations: There is a spectrum of density fluctuations (Zel'dovich
spectrum?); No consensus on origin.
@ Clustering, large-scale stucture: Governato et al Nat(98)ap [seeds];
Guzzo ap/99-in;
Einasto ap/00-in;
Sylos Labini & Pietronero ap/01-in
[complexity]; Gott et al ApJ(05)ap/03 [complete
map]; Hwang & Noh ap/05 [validity
of Newtonian modeling].
@ Homogeneity: Gaite et al ApJL(99)ap/98 [matter,
vs fractal]; Dautcourt ap/99 [constraints];
Lahav ap/99-in, ap/00-in;
Trodden & Vachaspati
MPLA(99)gq [problem].
@ Case against homogeneity: Clarkson & Barrett CQG(99)ap,
Barrett & Clarkson CQG(00)ap/99;
Clarkson
ap/00-PhD.
@ Statistical methods: Kerscher ap/99-in;
Shandarin ap/04-in;
Gabrielli et al 05; > s.a. cmb.
@ Skewness: Amendola & Quercellini PRL(04)ap [and
the equivalence principle].
@ Related topics: Durrer & Sylos Labini ap/98/A&AL,
Gawiser ap/00-PhD
[and cmb]; > s.a. fractals.
Observational Missions
* Past: COBE (Cosmic Background Explorer), launched in 1989, reported
the first anisotropy in 1992.
* Present and future:
WMAP (Wilkinson Microwave Anisotropy Probe) launched in 2001, reported results
in 2003 and 2006; ESA's Planck, scheduled for
launch in
2009.
Main page – Abbreviations – Journals – Comments – Other
sites – Acknowledgements
Send feedback and suggestions to bombelli at olemiss.edu – Modified
25 jun 2008