2002A&A...390..751H


Query : 2002A&A...390..751H

2002A&A...390..751H - Astronomy and Astrophysics, volume 390, 751-766 (2002/8-1)

Cosmic rays from microquasars: A narrow component to the CR spectrum?

HEINZ S. and SUNYAEV R.

Abstract (from CDS):

We propose that relativistic Galactic jets like those observed in GRS 1915+105 and GRO J1655-40 may produce a small but measurable contribution to the cosmic ray (CR) spectrum. If these jets contain cold protons and heavy ions (as in the case of SS433), it is plausible that this component will consist of a narrow spectral feature, with a mean particle energy corresponding roughly to the bulk kinetic particle energy in the beam, (Γjet)*(mp)*c2. Based on the current estimates of Γjet, this feature will fall into the range of 3-10GeV. The presence of several sources with different Γjet will lead to the superposition of several such peaks. In addition to the narrow peaks, diffusive particle acceleration should also produce a powerlaw, whose low energy cutoff at or above (Γjet)2*(mp)*c2 would be visible as an additional spectral feature. The large metallicities measured in several binary companions of jet sources suggest that this CR component could have an anomalous composition compared to the bulk Galactic CR spectrum. We provide estimates of the effects of adiabatic losses which are the greatest challenge to models of narrow band CR production in microquasar jets. While the total energy contained in the microquasar CR component is highly uncertain, the local CR spectrum in the vicinity of any microquasar should be severely affected. The upcoming AMS 02 experiment will be able probe the low energy CR spectrum for such components and for composition anomalies. The spectrally peculiar gamma-ray emission produced by interaction of the ISM with CRs surrounding microquasars might be detectable by GLAST. If the presence of a microquasar CR proton component can be ruled out observationally, this argument could be turned around in favor of electron-positron jets. We show that existing OSSE/GRO and future INTEGRAL data on the Galactic 511keV line flux put interesting constraints on the particle content of microquasar jets. The process of CR production in relativistic flows inside the Galaxy is fundamentally different from the standard picture of CR production in nonrelativistic shocks in supernova remnants, because the particles injected by a relativistic flow are already relativistic, without any need for diffusive acceleration.

Abstract Copyright:

Journal keyword(s): acceleration of particles - ISM: cosmic rays - ISM: jets and outflows - shock waves - black hole physics - gamma rays: theory

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 M 42 HII 05 35 17 -05 23.4           ~ 4107 0
2 NAME Ori A MoC 05 38 -07.1           ~ 3032 0
3 V* BR Cir HXB 15 20 40.8532547060 -57 10 00.206639033   21.4 21.4     ~ 787 1
4 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1900 1
5 V* V821 Ara HXB 17 02 49.3876391280 -48 47 23.087954544 16.20 16.30 15.5     ~ 2104 0
6 1E 1740.1-2942 X 17 43 -29.7           ~ 24 0
7 AX J1748.0-2829 LXB 17 48 05.060 -28 28 25.80     13.60     ~ 185 0
8 2XMM J180112.4-254436 LXB 18 01 12.40 -25 44 36.1           ~ 395 1
9 V* V4641 Sgr HXB 18 19 21.6343259256 -25 24 25.849595952     13.654   13.092 B9III 478 1
10 SS 433 HXB 19 11 49.5647697480 +04 58 57.827127648   16.854 14.643     A3/7I 2135 4
11 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2646 0
12 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4375 0
13 V* V404 Cyg HXB 20 24 03.8254458776 +33 52 01.962185735           G9/K0III/V 1283 0
14 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1951 2

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