2013A&A...558A..19W


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:57:03

2013A&A...558A..19W - Astronomy and Astrophysics, volume 558A, 19-19 (2013/10-1)

Mass entrainment and turbulence-driven acceleration of ultra-high energy cosmic rays in Centaurus A.

WYKES SARKA, CROSTON J.H., HARDCASTLE M.J., EILEK J.A., BIERMANN P.L., ACHTERBERG A., BRAY J.D., LAZARIAN A., HAVERKORN M., PROTHEROE R.J. and BROMBERG O.

Abstract (from CDS):

Observations of the FRI radio galaxy CentaurusA in radio, X-ray, and gamma-ray bands provide evidence for lepton acceleration up to several TeV and clues about hadron acceleration to tens of EeV. Synthesising the available observational constraints on the physical conditions and particle content in the jets, inner lobes and giant lobes of CentaurusA, we aim to evaluate its feasibility as an ultra-high-energy cosmic-ray source. We apply several methods of determining jet power and affirm the consistency of various power estimates of ∼1x1043erg/s. Employing scaling relations based on previous results for 3C31, we estimate particle number densities in the jets, encompassing available radio through X-ray observations. Our model is compatible with the jets ingesting ∼3x1021g/s of matter via external entrainment from hot gas and ∼7x1022g/s via internal entrainment from jet-contained stars. This leads to an imbalance between the internal lobe pressure available from radiating particles and magnetic field, and our derived external pressure. Based on knowledge of the external environments of other FRI sources, we estimate the thermal pressure in the giant lobes as 1.5x10–12dyn/cm2, from which we deduce a lower limit to the temperature of ∼1.6x108K. Using dynamical and buoyancy arguments, we infer ∼440-645Myr and ∼560Myr as the sound-crossing and buoyancy ages of the giant lobes respectively, inconsistent with their spectral ages. We re-investigate the feasibility of particle acceleration via stochastic processes in the lobes, placing new constraints on the energetics and on turbulent input to the lobes. The same ``very hot'' temperatures that allow self-consistency between the entrainment calculations and the missing pressure also allow stochastic UHECR acceleration models to work.

Abstract Copyright:

Journal keyword(s): acceleration of particles - cosmic rays - galaxies: active - galaxies: individual: Centaurus A - galaxies: jets - turbulence

Simbad objects: 19

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Number of rows : 19

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 NGC 315 LIN 00 57 48.88335 +30 21 08.8122 12.80 12.20 11.16 11.26   ~ 706 2
2 NGC 383 rG 01 07 24.95870 +32 24 45.2140   13.6 12.14     ~ 719 3
3 UGC 1841 Sy1 02 23 11.41124 +42 59 31.3840   15.71 14.81     ~ 527 2
4 NGC 1044 GiG 02 41 06.183 +08 44 16.72   14.8       ~ 60 1
5 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3544 3
6 Z 541-15 rG 03 29 23.893 +39 47 31.89   14.9       ~ 90 0
7 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 907 1
8 SN 1986A SN* 10 46 36.54 +13 45 00.6   14.4 14.2     SNIa 56 1
9 NGC 4261 LIN 12 19 23.2160630 +05 49 29.700024   13.92 12.87     ~ 1114 0
10 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 971 2
11 NGC 5090 rG 13 21 12.8447 -43 42 16.839   12.59 11.51 10.84   ~ 184 1
12 LEDA 46663 G 13 21 47.1 -45 03 41           ~ 51 0
13 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3995 3
14 NGC 5532 LIN 14 16 52.928 +10 48 26.43   13.3       ~ 318 3
15 2MASX J14530283+3308423 BiC 14 53 02.863 +33 08 42.41           ~ 29 2
16 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 675 1
17 PKS 1553+245 rG 15 56 03.875 +24 26 52.70   15.4       ~ 85 1
18 NGC 6251 Sy2 16 32 31.96990024 +82 32 16.3999540 15.24 14.66 12.89 7.62   ~ 663 0
19 NAME Cen A Jet PoG ~ ~           ~ 45 0

    Equat.    Gal    SGal    Ecl

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2020.07.03-22:57:03

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