Self-similar collapse with cooling and heating in an expanding universe

Details Self-similar collapse with cooling and heating in an expanding universe Self-similar collapse with cooling and heating in an expanding universe

2003-11-05

arxiv.org/abs/astro-ph/0311116v1

Mon.Not.Roy.Astron.Soc. 348 (2004) 89

Astronomy and Astrophysics

Astrophysics

12pages, 29figures. Accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2004.07328.x

We derive self-similar solutions including cooling and heating in an Einstein de-Sitter universe, and investigate the effects of cooling and heating on the gas density and temperature distributions. We assume that the cooling rate has a power-law dependence on the gas density and temperature, $\Lambda$$\propto$$\rho^{A}T^{B}$, and the heating rate is $\Gamma$$\propto$$\rho T$. The values of $A$ and $B$ are chosen by requiring that the cooling time is proportional to the Hubble time in order to obtain similarity solutions. In the region where the cooling rate is greater than the heating rate, a cooling inflow is established, and the gas is compressed and heats up. Because the compression is greater in the inner region than in the outer region, the temperature becomes an increasing profile toward the center. In particular, when a large infall velocity is produced due to an enormous energy loss, the slope of the density approaches a value that depends on $A$, $B$, and the velocity slope, and the slope of the temperature approaches $-$1. On the other hand, in the region where the heating rate is greater than the cooling rate, the infall velocity is suppressed, compression of the gas is weakened, and the gas cools down. The slope of the density becomes shallow due to suppression of the contraction, and the temperature is lower than that without heating. The self-similar collapse presented here gives insights to the effects of cooling and heating on the gas distributions in galaxies and clusters of galaxies.

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