2020MNRAS.498.5772R


Query : 2020MNRAS.498.5772R

2020MNRAS.498.5772R - Mon. Not. R. Astron. Soc., 498, 5772-5785 (2020/November-2)

Rapid compact jet quenching in the Galactic black hole candidate X-ray binary MAXI J1535-571.

RUSSELL T.D., LUCCHINI M., TETARENKO A.J., MILLER-JONES J.C.A., SIVAKOFF G.R., KRAUSS F., MULAUDZI W., BAGLIO M.C., RUSSELL D.M., ALTAMIRANO D., CECCOBELLO C., CORBEL S., DEGENAAR N., VAN DEN EIJNDEN J., FENDER R., HEINZ S., KOLJONEN K.I.I., MAITRA D., MARKOFF S., MIGLIARI S., PARIKH A.S., PLOTKIN R.M., RUPEN M., SARAZIN C., SORIA R. and WIJNANDS R.

Abstract (from CDS):

We present results from six epochs of quasi-simultaneous radio, (sub-)millimetre, infrared, optical, and X-ray observations of the black hole X-ray binary MAXI J1535-571. These observations show that as the source transitioned through the hard-intermediate X-ray state towards the soft-intermediate X-ray state, the jet underwent dramatic and rapid changes. We observed the frequency of the jet spectral break, which corresponds to the most compact region in the jet where particle acceleration begins (higher frequencies indicate closer to the black hole), evolves from the infrared band into the radio band (decreasing by ∼3 orders of magnitude) in less than a day. During one observational epoch, we found evidence of the jet spectral break evolving in frequency through the radio band. Estimating the magnetic field and size of the particle acceleration region shows that the rapid fading of the high-energy jet emission was not consistent with radiative cooling; instead, the particle acceleration region seems to be moving away from the black hole on approximately dynamical time-scales. This result suggests that the compact jet quenching is not caused by local changes to the particle acceleration, rather we are observing the acceleration region of the jet travelling away from the black hole with the jet flow. Spectral analysis of the X-ray emission shows a gradual softening in the few days before the dramatic jet changes, followed by a more rapid softening ∼1-2 d after the onset of the jet quenching.

Abstract Copyright: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): acceleration of particles, accretion, accretion discs - ISM: jets and outflows - submillimetre: general - X-rays: binaries - X-rays: individual (MAXI J1535-571) - Astrophysics - High Energy Astrophysical Phenomena

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 - 2021
#notes
1 QSO B1424-41 QSO 14 27 56.29756536 -42 06 19.4375991   18.48 17.7 16.30   ~ 402 1
2 MAXI J1535-571 XB* 15 35 19.73 -57 13 48.1           ~ 76 0
3 V* IL Lup HXB 15 47 08.2766679321 -47 40 10.284971214     11.96     ~ 427 1
4 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1075 0
5 3FGL J1617.4-5846 AGN 16 17 17.8913859288 -58 48 07.860059063   18.23       ~ 107 1
6 PMN J1631-5256 Rad 16 31 07.351 -52 56 35.60           ~ 3 0
7 MAXI J1659-152 LXB 16 59 01.680 -15 15 28.73           ~ 204 0
8 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1857 0
9 MAXI J1836-194 XB* 18 35 43.440 -19 19 10.48           ~ 116 0
10 X Aql X-1 LXB 19 11 16.0572031521 +00 35 05.876658556           ~ 1053 1
11 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2396 0
12 QSO B2052-474 QSO 20 56 16.35981874 -47 14 47.6276461   18.29 19.1 18.07   ~ 279 1

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2021.09.26-08:18:35

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