2003A&A...397..645M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST00:18:28

2003A&A...397..645M - Astronomy and Astrophysics, volume 397, 645-658 (2003/1-2)

Exploring the role of jets in the radio/X-ray correlations of GX 339-4.

MARKOFF S., NOWAK M., CORBEL S., FENDER R. and FALCKE H.

Abstract (from CDS):

The Galactic black hole candidate X-ray binary GX 339-4 spends most of its time in the low/hard state, making it an ideal candidate for modeling the assumedly low accretion phase. The radio emission correlates very tightly with the X-rays over more than two orders of magnitude in X-ray flux density, suggesting that the jet plasma also plays a role at the higher frequencies. We compare the predictions of our jet model, with and without acceleration, to thirteen broadband simultaneous or quasi-simultaneous spectra over this changing flux history. In addition, we consider a simple standard thin disk which transitions to an optically thin accretion flow, in order to account for the assumedly thermal optical data seen in some observations. A solution without acceleration cannot describe the data without unrealistic energy requirements, nor explain the non-thermal radio spectrum seen during recent radio outbursts. But because of the low disk luminosity, and possibly the assumed disk geometry, acceleration in the jet is limited only by synchrotron cooling and can extend easily into the X-rays. We present a model which can account for all the broadband spectra included here, by changing only two parameters in the jet model: the input power and the location of the first acceleration zone. However, the model is most sensitive to changes in the jet power, the varying of which can also account for the slope of the observed radio/X-ray correlation analytically. At the highest low/hard state luminosities, the synchrotron self-Compton emission from the jet could be detectable with missions such as GLAST, providing a way to test the extent of the synchrotron contribution. We conclude that jet synchrotron is a possible way to explain the broadband features and this correlation, and discuss ways of incorporating this component into the ``standard'' corona picture.

Abstract Copyright:

Journal keyword(s): X-rays: binaries - X-rays: individual: GX 339-4 - radiation mechanisms: non-thermal - stars: winds, outflows - black hole physics - accretion, accretion disks

Simbad objects: 9

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Number of rows : 9

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 UGC 1841 Sy1 02 23 11.41124 +42 59 31.3840   15.71 14.81     ~ 527 2
2 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 721 0
3 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2115 3
4 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6213 3
5 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1764 0
6 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 638 1
7 2XMM J180112.4-254436 LXB 18 01 12.40 -25 44 36.1           ~ 361 1
8 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3925 0
9 V* V404 Cyg HXB 20 24 03.820 +33 52 01.90 14.50 14.20 12.7     K0IV 1090 0

    Equat.    Gal    SGal    Ecl

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2020.07.13-00:18:28

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