2018MNRAS.481.2646M


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.18CEST04:09:37

2018MNRAS.481.2646M - Mon. Not. R. Astron. Soc., 481, 2646-2665 (2018/December-1)

The 1989 and 2015 outbursts of V404 Cygni: a global study of wind-related optical features.

MATA SANCHEZ D., MUNOZ-DARIAS T., CASARES J., CHARLES P.A., ARMAS PADILLA M., FERNANDEZ-ONTIVEROS J.A., JIMENEZ-IBARRA F., JONKER P.G., LINARES M., TORRES M.A.P., SHAW A.W., RODRIGUEZ-GIL P., VAN GRUNSVEN T., BLAY P., CABALLERO-GARCIA M.D., CASTRO-TIRADO A., CHINCHILLA P., FARINA C., FERRAGAMO A., LOPEZ-MARTINEZ F., RUBINO-MARTIN J.A. and SUAREZ-ANDRES L.

Abstract (from CDS):

The black hole transient V404 Cygni exhibited a bright outburst in June 2015 that was intensively followed over a wide range of wavelengths. Our team obtained high time resolution optical spectroscopy ( ¡ ∼¡ 90 s), which included a detailed coverage of the most active phase of the event. We present a data base consisting of 651 optical spectra obtained during this event, that we combine with 58 spectra gathered during the fainter December 2015 sequel outburst, as well as with 57 spectra from the 1989 event. We previously reported the discovery of wind-related features (P-Cygni and broad-wing line profiles) during both 2015 outbursts. Here, we build diagnostic diagrams that enable us to study the evolution of typical emission line parameters, such as line fluxes and equivalent widths, and develop a technique to systematically detect outflow signatures. We find that these are present throughout the outburst, even at very low optical fluxes, and that both types of outflow features are observed simultaneously in some spectra, confirming the idea of a common origin. We also show that the nebular phases depict loop patterns in many diagnostic diagrams, while P-Cygni profiles are highly variable on time-scales of minutes. The comparison between the three outbursts reveals that the spectra obtained during June and December 2015 share many similarities, while those from 1989 exhibit narrower emission lines and lower wind terminal velocities. The diagnostic diagrams presented in this work have been produced using standard measurement techniques and thus may be applied to other active low-mass X-ray binaries.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): accretion, accretion discs - stars: winds, outflows - ISM: jets, outflows - X-rays: binaries

Simbad objects: 11

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Number of rows : 11

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 SV* HV 5682 XB* 05 13 50.809 -69 51 47.30     16.566 16.606 16.62 ~ 307 0
2 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 602 0
3 CRTS J135716.8-093238 HXB 13 57 16.8357614768 -09 32 38.793867836           M4.5V 124 0
4 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1753 1
5 V* V4641 Sgr HXB 18 19 21.6342721789 -25 24 25.849323550     13.654   13.092 B9III 409 1
6 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2368 0
7 USNO-A2.0 1200-15039207 * 20 23 53.3850394981 +33 52 24.228814935   14.1   12.9   ~ 3 0
8 V* V404 Cyg HXB 20 24 03.820 +33 52 01.90 14.50 14.20 12.7     K0IV 1127 0
9 UCAC3 248-227136 * 20 24 07.1798596622 +33 50 51.683789955   13.32   12.778 11.85 ~ 7 0
10 HD 340611 WD* 20 34 21.8849808924 +25 03 49.749569866 10.687 11.471 11.546 11.648 11.728 DA2.4 288 0
11 BD+25 4655 HS* 21 59 41.9751489837 +26 25 57.398356446 8.27 9.39 9.68     sdO6 104 0

    Equat.    Gal    SGal    Ecl

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2021.05.18-04:09:37

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