# 2008A&A...484...51C

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 Query : 2008A&A...484...51C

2008A&A...484...51C - Astronomy and Astrophysics, volume 484, 51-65 (2008/6-2)

Warming rays in cluster cool cores.

COLAFRANCESCO S. and MARCHEGIANI P.

Abstract (from CDS):

Cosmic rays are confined in the atmospheres of galaxy clusters and, therefore, they can play a crucial role in the heating of their cool cores. We discuss here the thermal and non-thermal features of a model of cosmic ray heating of cluster cores that can provide a solution to the cooling-flow problems. To this aim, we generalize a model originally proposed by Colafrancesco, Dar & DeRujula (2004A&A...413..441C) and we show that our model predicts specific correlations between the thermal and non-thermal properties of galaxy clusters and enables various observational tests. The model reproduces the observed temperature distribution in clusters by using an energy balance condition in which the X-ray energy emitted by clusters is supplied, in a quasi-steady state, by the hadronic cosmic rays, which act as warming rays'' (WRs). The temperature profile of the intracluster (IC) gas is strictly correlated with the pressure distribution of the WRs and, consequently, with the non-thermal emission (radio, hard X-ray and gamma-ray) induced by the interaction of the WRs with the IC gas and the IC magnetic field. The temperature distribution of the IC gas in both cool-core and non cool-core clusters is successfully predicted from the measured IC plasma density distribution. Under this contraint, the WR model is also able to reproduce the thermal and non-thermal pressure distribution in clusters, as well as their radial entropy distribution, as shown by the analysis of three clusters studied in detail: Perseus, A2199 and Hydra. The WR model provides other observable features of galaxy clusters: a correlation of the pressure ratio (WRs to thermal IC gas) with the inner cluster temperature (PWR/Pth)~(kTinner)–2/3, a correlation of the gamma-ray luminosity with the inner cluster temperature Lγ~(kTinner)4/3, a substantial number of cool-core clusters observable with the GLAST-LAT experiment, a surface brightness of radio halos in cool-core clusters that recovers the observed one, a hard X-ray ICS emission from cool-core clusters that is systematically lower than the observed limits and yet observable with the next generation high-sensitivity and spatial resolution HXR experiments like Simbol-X. The specific theoretical properties and the multi-frequency distribution of the e.m. signals predicted in the WR model render it quite different from the other models so far proposed for the heating of clusters' cool-cores. Such differences make it possible to prove or disprove our model as an explanation for the cooling-flow problems on the basis of multi-frequency observations of galaxy clusters.

Journal keyword(s): cosmology: theory - galaxies: clusters: general - ISM: cosmic rays

Full paper

 Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ACO 133 ClG 01 02 39.0 -21 57 15           ~ 350 1
2 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 675 1
3 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2093 1
4 RX J0821.0+0752 ClG 08 21 02.4 +07 51 47           ~ 56 1
5 NAME HYA SUPERCL SCG 08 57.9 +03 10           ~ 163 0
6 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 279 0
7 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4501 2
8 ClG J1347-1145 ClG 13 47 33.5 -11 45 42           ~ 503 0
9 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1201 0
10 ACO 2163 ClG 16 15 34.1 -06 07 26           ~ 540 0
11 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1128 1
12 ACO 2244 ClG 17 02 34.01 +34 04 41.1           ~ 255 0
13 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 651 2

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2022.05.20-23:56:19