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2009

Matter temperature after cosmological recombination

Scott, Douglas, Moss, Adam

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The temperature of the atomic matter in the Universe is held to that of the Cosmic Background radiation until decoupling at z~100.

After this it cools faster than the radiation (\propto(1+z)^2 rather than (1+z)) and would have fallen to about 20mK today if astrophysical feedback processes had not heated up the interglactic medium.
We show how the derivative of the Compton coupling equation helps numerically to follow the decoupling process.

Matter temperature after cosmological recombination · Around

Built on

Gamow G., 1949, Rev. Mod. Phys., 21, 367 (quoting unpublished work by Gamow, Metropolis, Teller & Ulam)
1949
Earlier work this paper cites.
Weymann R., 1966, ApJ, 145, 560
1966
Earlier work this paper cites.
Peebles P.J.E., 1971, ‘Physical Cosmology’, Princeton University Press, Princeton, p. 232 \,232
1971
Earlier work this paper cites.

Similar

Seager S., Sasselov D.D., Scott D., 1999, ApJ, 523, L1
1999
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Seager S., Sasselov D.D., Scott D., 2000, ApJS, 128, 407
2000
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Chluba J. C., Rubino-Martin J. A., Sunyaev R. A., 2007, MNRAS, 374, 1310
2007
Cited alongside, same era.

Then

Fendt W.A., Chluba J., Rubiño-Martín J.A., Wandelt B.D., ApJ, in press, arXiv:0807.2577
Original
2008
Later among the works it cites.
Hirata C.M., 2008, PRD, in press, arXiv:0803.0808
Original
2008
Later among the works it cites.
Wong W.Y., Moss A., Scott D., 2008, MNRAS, 386, 1023
2008
Later among the works it cites.

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