In General > s.a. astronomy; early-universe
cosmology; 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]; Holder et al a0907/ApJ
[baryon-dark matter ratio fluctuations]; Ferreira & Starkmann Sci-a0911 [dark
fields vs modified gravity].
@ 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 references: 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 AIP-ap/06.
@ 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);
Brown PhD(06)-a0812
[primordial].
@ 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).
* 2008: Recent experiments,
including PAMELA, ATIC, WMAP, and EGRET, have revealed unusually high electron-positron
production in the cosmos, more so
than can be explained by mechanisms such as supernova explosions or cosmic-ray
collisions; This discrepancy is leading some researchers to speculate that
dark matter may play a part [@ news pt(08)nov].
* 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 GRBs]; 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,
Fernandez et al a0906/ApJ [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 NCB(07)-a0801-in
[gravitational lensing]; Pritchard & Loeb PRD(08)-a0802
[evolution]; Pen et al a0802/MNRAS
[detection of structure]; Peterson et al a0902-rp
[mapping]; Khatri & Wandelt a0910-in
[and fundamental physics]; > s.a. observational
cosmology;
perturbations.
@ Other diffuse background: Henry ap/99;
Lagache et al ASS(99)ap [sub-mm];
Zhao et al PLB(09) [free-streaming gas in radiation-dominated era]; > s.a. cmb; gamma
rays; gravitons; neutrinos.
Matter Distribution > s.a. galaxy
distribution [including cosmic web]; 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.
* Galactic vs cosmic abundances: The Milky Way and all other galaxies are missing
most of their baryons in that the ratio of the known baryonic mass to the gravitating
mass (within the virial radius), is several times less than the cosmic ratio
determined from WMAP.
* 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]; Bregman a0906 [galactic vs cosmic].
@ 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 PhD(99)ap/00.
@ Local void scenarios: Alexander et al a0710 [supernova and cmb data]; > s.a.
theory of cosmological acceleration.
@ 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 A&AL-ap/98,
Gawiser PhD(99)ap/00
[and cmb]; > s.a. fractals in physics.
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 8
nov 2009