2011A&A...527A..99E


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:13:11

2011A&A...527A..99E - Astronomy and Astrophysics, volume 527A, 99-99 (2011/3-1)

Cosmic ray transport in galaxy clusters: implications for radio halos, gamma-ray signatures, and cool core heating.

ENSSLIN T., PFROMMER C., MINIATI F. and SUBRAMANIAN K.

Abstract (from CDS):

We investigate the interplay of cosmic ray (CR) propagation and advection in galaxy clusters. Propagation in form of CR diffusion and streaming tends to drive the CR radial profiles towards being flat, with equal CR number density everywhere. Advection of CR by the turbulent gas motions tends to produce centrally enhanced profiles. We assume that the CR streaming velocity is of the order of the sound velocity. This is motivated by plasma physical arguments. The CR streaming is then usually larger than typical advection velocities and becomes comparable or lower than this only for periods with trans- and super-sonic cluster turbulence. As a consequence a bimodality of the CR spatial distribution results. Strongly turbulent, merging clusters should have a more centrally concentrated CR energy density profile with respect to relaxed ones with very subsonic turbulence. This translates into a bimodality of the expected diffuse radio and gamma-ray emission of clusters, since more centrally concentrated CR will find higher target densities for hadronic CR proton interactions, higher plasma wave energy densities for CR electron and proton re-acceleration, and stronger magnetic fields. Thus, the observed bimodality of cluster radio halos appears to be a natural consequence of the interplay of CR transport processes, independent of the model of radio halo formation, be it hadronic interactions of CR protons or re-acceleration of low-energy CR electrons. Energy dependence of the CR propagation should lead to spectral steepening of dying radio halos. Furthermore, we show that the interplay of CR diffusion with advection implies first order CR re-acceleration in the pressure-stratified atmospheres of galaxy clusters. Finally, we argue that CR streaming could be important in turbulent cool cores of galaxy clusters since it heats preferentially the central gas with highest cooling rate.

Abstract Copyright:

Journal keyword(s): acceleration of particles - astroparticle physics - radio continuum: galaxies - magnetic fields - galaxies: clusters: intracluster medium - gamma rays: galaxies: clusters

Simbad objects: 53

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Number of rows : 53

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 ACO 2697 ClG 00 03 11.5 -06 05 30           ~ 36 0
2 ACO 2744 ClG 00 14 20.03 -30 23 17.8           ~ 571 0
3 ClG 0016+16 ClG 00 18 33.3 +16 26 36           ~ 472 0
4 2MASX J00274579+2616264 ClG 00 27 45.90 +26 16 25.0           ~ 33 0
5 ACO 141 ClG 01 05 30.2342 -24 39 17.430           ~ 68 0
6 ACO 209 ClG 01 31 57.5 -13 34 35           ~ 250 0
7 ACO 3088 ClG 03 07 02.12 -28 39 57.3           ~ 60 0
8 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 1939 1
9 ACO 521 ClG 04 54 08.6 -10 14 39           ~ 213 0
10 ACO 520 ClG 04 54 19.0 +02 56 49           ~ 381 0
11 ACO 545 ClG 05 32 24.4152 -11 32 35.080           ~ 88 0
12 ACO 3376 ClG 06 01 42.1521 -39 59 06.227           ~ 270 0
13 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 799 1
14 ClG J0717+3745 ClG 07 17 36.50 +37 45 23.0           ~ 357 0
15 B3 0714+378 Rad 07 17 36.50 +37 45 23.0           ~ 169 2
16 2MASX J07473129-1917403 BiC 07 47 31.296 -19 17 40.34   19.60       ~ 393 1
17 ClG 0745-19 ClG 07 47 31.3 -19 17 40           ~ 364 0
18 ACO 611 ClG 08 00 58.7 +36 02 49           ~ 222 0
19 ACO 665 ClG 08 30 45.2 +65 52 55           ~ 402 0
20 ZwCl 0857+2107 ClG 09 00 37.9 +20 54 58           ~ 75 0
21 ACO 754 ClG 09 08 50.1 -09 38 12           ~ 631 1
22 ACO 773 ClG 09 17 51.3 +51 43 20           ~ 261 0
23 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 907 1
24 ACO 781 ClG 09 20 25.4 +30 30 07           ~ 129 0
25 ZwCl 0949+5207 ClG 09 52 49.1 +51 53 05           ~ 112 0
26 ZwCl 1113+0144 ClG 11 15 54.0 +01 29 44           ~ 32 0
27 ACO 1300 ClG 11 32 00.7 -19 53 34           ~ 132 0
28 ACO 1423 ClG 11 57 47.34 +33 42 43.5           ~ 140 0
29 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4208 2
30 ZwCl 1303+2647 ClG 13 05 58.0 +26 30 53   20.1       ~ 21 0
31 ZwCl 1309+2216 ClG 13 11.5 +22 00           ~ 23 0
32 2MASX J13142209-2515456 ClG 13 14 31.5049 -25 15 56.602           ~ 87 0
33 ACO 1914 ClG 14 26 01.3 +37 49 36           ~ 273 0
34 ZwCl 1455+2232 ClG 14 57 15.2 +22 20 30     18.62     ~ 262 0
35 ACO S 780 ClG 14 59 29.1 -18 10 45           ~ 63 0
36 ZwCl 1459+4240 ClG 15 01 20.6251 +42 20 47.148           ~ 48 0
37 RXC J1512.2-2254 ClG 15 12 12.6 -22 54 59           ~ 12 0
38 LEDA 1900245 Bla 15 32 53.780 +30 20 59.41   19.1   15.7   ~ 128 0
39 ACO 2142 ClG 15 58 20.00 +27 14 00.3           ~ 672 0
40 ACO 2163 ClG 16 15 34.1 -06 07 26           ~ 519 0
41 ACO 2219 ClG 16 40 22.1 +46 42 20           ~ 317 0
42 ACO 2256 ClG 17 03 43.5 +78 43 03           ~ 830 1
43 ACO 2255 ClG 17 12 50.04 +64 03 10.6           ~ 502 0
44 ACO 2254 ClG 17 17 45.90 +19 40 22.8           ~ 58 0
45 ACO 2319 ClG 19 20 45.3 +43 57 43           ~ 414 1
46 RXC J2003.5-2323 ClG 20 03 32.3 -23 23 30           ~ 53 0
47 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 566 1
48 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 625 2
49 1RXS J222834.4+203647 ClG 22 28 37.1 +20 36 31           ~ 102 0
50 ACO 2537 ClG 23 08 22.3 -02 11 29           ~ 106 0
51 ACO 2626 ClG 23 36 31.0 +21 09 36           ~ 211 0
52 ACO 2631 ClG 23 37 40.7 +00 16 35           ~ 138 0
53 ACO 2667 ClG 23 51 39.37 -26 05 02.7           ~ 150 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:13:11

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