2018A&A...616A..57R


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST23:19:44

2018A&A...616A..57R - Astronomy and Astrophysics, volume 616A, 57-57 (2018/8-1)

Particle acceleration in the superwinds of starburst galaxies.

ROMERO G.E., MULLER A.L. and ROTH M.

Abstract (from CDS):


Context. Starbursts are galaxies undergoing massive episodes of star formation. The combined effect of stellar winds from hot stars and supernova explosions creates a high-temperature cavity in the nuclear region of these objects. The very hot gas expands adiabatically and escapes from the galaxy creating a superwind which sweeps matter from the galactic disk. The superwind region in the halo is filled with a multi-phase gas with hot, warm, cool, and relativistic components.
Aims. The shocks associated with the superwind of starbursts and the turbulent gas region of the bubble inflated by them might accelerate cosmic rays up to high energies. In this work we calculate the cosmic ray production associated with the superwind using parameters that correspond to the nearby southern starburst galaxy NGC 253, which has been suggested as a potential accelerator of ultra-high-energy cosmic rays.
Methods. We evaluate the efficiency of both diffusive shock acceleration (DSA) and stochastic diffusive acceleration (SDA) in the superwind of NGC 253. We estimate the distribution of both hadrons and leptons and calculate the corresponding spectral energy distributions of photons. The electromagnetic radiation can help to discriminate between the different scenarios analyzed.
Results. We find that the strong mass load of the superwind, recently determined through ALMA observations, strongly attenuates the efficiency of DSA in NGC 253, whereas SDA is constrained by the age of the starburst.
Conclusions. We conclude that NGC 253 and similar starbursts can only accelerate iron nuclei beyond ∼1018eV under very special conditions. If the central region of the galaxy harbors a starved supermassive black hole of ∼106M, as suggested by some recent observations, a contribution in the range 1018-1019eV can be present for accretion rates m∼10–3 in Eddington units. Shock energies of the order of 100EeV might only be possible if very strong magnetic field amplification occurs close to the superwind.

Abstract Copyright: © ESO 2018

Journal keyword(s): acceleration of particles - radiation mechanisms: non-thermal - galaxies: starburst - galaxies: individual

Simbad objects: 12

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Number of rows : 12

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 [AU88] 5.62-41.3 SNR 00 47 33.005 -25 17 19.35           ~ 23 0
2 [AU88] 5.73-39.5 HII 00 47 33.1 -25 17 18           ~ 14 0
3 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2929 2
4 [LT2006b] 5.795-39.05 SNR 00 47 33.178 -25 17 16.93           ~ 35 0
5 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4089 2
6 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5594 4
7 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5331 6
8 NGC 4945 Sy2 13 05 27.279 -49 28 04.44   9.31 14.40 7.55   ~ 1264 2
9 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3995 3
10 NAME Ursa Major Cluster ClG 15 08.8 +67 07           ~ 381 0
11 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3446 3
12 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-23:19:44

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