Matter Content of the Universe| Matter Content of the Universe |
In General > s.a. astronomy; cosmological
parameters; early-universe cosmology, baryogenesis
and nucleosynthesis; matter distribution.
* 1995: The dogma is that
Ωb ≈ 0.05, Ωdm
≈ 0.95, Ωcc = 0.
* 1998: M Turner &
D Schramm predict 5% ordinary matter, based on deuterium abundance.
* 1999: "Matter"
consists of ordinary matter/radiation (Ω ≈ 0.2), dark matter,
and dark energy (possibly a cosmological constant).
* 2000: Cold dark matter
from new cmb data; Favored values Ωm
≈ 0.4 ± 0.1, Ωb
= 0.02 h−2,
0.001 < Ων < 0.1,
Ωcc ≈ 0.7.
* 2001: New DASI and Boomerang cmb data; Favored
values Ωb = 0.05, Ωdm
= 0.30, Ωde = 0.65 (p < 0).
* 2002: 2dF galaxy redshift survey and cmb,
Ωm = 1 − Ωcc
= 0.30; Using KamLAND data, Ων
≤ 0.070 h−2.
* 2003:
WMAP data give Ωb
= 0.04, Ωdm
= 0.23, Ωde
= 0.73; SDSS data, Ωb
= 0.05, Ωdm
= 0.25, Ωde = 0.70.
* 2003: The ΛCDM model provides the
best fit to the data, with Ωtot = 1.02 ± 0.02.
* 2013: GRBs as standard candles give
Ωm = 0.30, Ωde
= 0.70; WMAP 5-year data Ωm = 0.27,
Ωde = 0.73; Planck mission Ωm
= 0.317, Ωde = 0.683.
* 2015: Planck mission data
give Ωm = 0.308 ± 0.012.
* Critical density: At the present time,
ρcrit = 6 H atoms/m3
= 10−26 kg/m3;
Notice that Ωcc = Λ
c2/3H02.
* Entropy: The entropy of the universe is low but increasing.
@ General references: Melott PRP(90);
Persic & Salucci MNRAS(92)ap/05 [baryons];
Bahcall ap/96 [large-scale structure];
White ap/96-conf [large z];
Dolgov NPPS(02)ap,
hp/02-proc [antimatter];
Krauss & Scherrer PRD(07)ap [radiation cannot become dominant again];
Holder et al ApJ(10)-a0907 [baryon-dark matter ratio fluctuations];
Ferreira & Starkmann Sci(09)nov-a0911 [dark fields vs modified gravity].
@ Density: Coles & Ellis Nat(94)aug,
97;
Bahcall & Fan PNAS(98)ap;
Krauss AIP(98)hp [cosmological constant];
Bahcall PS(00)ap/99-conf [galaxy clusters];
Roos & Harun-or-Rashid ap/00,
ap/00 [flatness];
Turner ApJL(02)ap/01;
Schindler ap/01-in
[Ωm];
Waterhouse & Zibin a0804 [variation of Ω];
Lee JCAP(14)-a1307 [from large-scale structure].
Types of Matter > s.a. dark matter;
inflationary scenarios; photon
phenomenology; 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].
@ Reviews: Dine ht/01-conf;
Durrer ap/02-proc;
Fukugita & Peebles ApJ(04)ap [energy inventory].
@ General references: Melia A&A(15)-a1411 [cosmic equation of state];
Clifton a1509-MG14
[is modeling the matter as dust adequate?];
Neeleman et al ApJ(16)-a1601 [HI].
@ 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).
@ Other diffuse background: Henry ApJL(99)ap;
Lagache et al ASS(99)ap [sub-mm];
Zhao et al PLB(09) [free-streaming gas in radiation-dominated era];
Dwek & Krennrich APP(13)-a1209,
news sn(13)aug [extragalactic background light];
Dado & Dar a1411
[common origin for gamma-ray and neutrino backgrounds, GRBs from jets in type Ic supernovae];
Cooray a1602-RSOS
[extragalactic background over 20 decades in wavelength];
> s.a. astronomy at various wavelengths [cosmic radio and infrared backgrounds];
cosmic microwave background; gamma rays;
gravitons; neutrinos.
And fundamental physics: see antimatter;
electroweak theory; quantum fields
in curved spacetime; structure of matter.
Phenomenology: see astronomical phenomena;
magnetism in astrophysics and cosmology;
observational cosmology [including matter and radiation].
Observational Missions
* Past: COBE (Cosmic Background Explorer),
launched in 1989; It reported the first anisotropy in 1992.
* Present and future: WMAP (Wilkinson
Microwave Anisotropy Probe) launched in 2001, reported results in 2003, 2006, 2008
(5-year results), 2011 (7-year results); ESA's Planck satellite launched in 2009.
main page
– abbreviations
– journals – comments
– other sites – acknowledgements
send feedback and suggestions to bombelli at olemiss.edu – modified 9 dec 2019