2014A&A...561A.137R


Query : 2014A&A...561A.137R

2014A&A...561A.137R - Astronomy and Astrophysics, volume 561A, 137-137 (2014/1-1)

Disc-loss episode in the Be shell optical counterpart to the high-mass X-ray binary IGR J21343+4738.

REIG P. and ZEZAS A.

Abstract (from CDS):

Present X-ray missions are regularly discovering new X-ray and γ-ray sources. The identification of their counterparts at other wavelengths allows us to determine their nature. The main goal of this work is to determine the properties of the optical counterpart to the INTEGRAL source IGR J21343+4738, and to study its long-term optical variability. Although its nature as a Be/X-ray binary has been suggested, little is known about its physical parameters. We have been monitoring IGR J21343+4738 since 2009 in the optical band. We present BVRI optical photometric and spectroscopic observations covering the wavelength band 4000-7500 Å. The photometric data allowed us to derive the colour excess E(B-V) and estimate the distance. The blue-end spectra were used to determine the spectral type of the optical companion, while the spectra around the Hα line allowed us to study the long-term structural changes in the circumstellar disc. We find that the optical counterpart to IGR J21343+4738 is a V=14.1 B1IVe shell star located at a distance of ∼8.5 kpc. The Hα line changed from an absorption-dominated profile to an emission-dominated profile, and then back again into absorption. In addition, fast line profile asymmetries were observed once the disc developed. Although the Balmer lines are the most strongly affected by shell absorption, we find that shell characteristics are also observed in He I lines. The optical spectral variability of IGR J21343+4738 is attributed to the formation of an equatorial disc around the Be star and the development of an enhanced density perturbation that revolves inside the disc. We have witnessed the formation and dissipation of the circumstellar disc. The strong shell profile of the Hα and He I lines and the fact that no transition from the shell phase to a pure emission phase is observed imply that we are seeing the system near edge-on.

Abstract Copyright:

Journal keyword(s): stars: individual: IGR J21343+4738 - X-rays: binaries - stars: neutron - stars: emission-line, Be

VizieR on-line data: <Available at CDS (J/A+A/561/A137): list.dat sp/*>

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 V* V635 Cas HXB 01 18 31.9704429246 +63 44 33.071137750 17.05 16.64 15.19 14.34 13.22 B0.2Ve 677 0
2 EM* GGA 104 HXB 01 47 00.2121223849 +61 21 23.661992704 11.76 12.09 11.366 11.00 10.52 B1IIIe 174 0
3 V* BQ Cam HXB 03 34 59.9116460415 +53 10 23.296351781   17.16 15.42 14.26 13.04 O8.5Ve 413 1
4 V* X Per HXB 03 55 23.0778791365 +31 02 45.045745259 6.090 6.840 6.720     O9.5III 924 0
5 LS V +44 17 HXB 04 40 59.3295352454 +44 31 49.258751047 11.02 11.42 10.73 10.28 9.76 B0.2Ve 102 0
6 HD 245770 HXB 05 38 54.5749436467 +26 18 56.839215267 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 900 0
7 IGR J06074+2205 HXB 06 07 26.6120418797 +22 05 47.759512772   12.85 12.21 11.80 11.32 B0.5Ve 34 1
8 V* V572 Pup HXB 08 12 28.3576629560 -31 14 52.138780764 12.14 13.03 12.74 12.44   B0.2IVe 62 0
9 HD 102567 Be* 11 48 00.0214627917 -62 12 24.900348093 8.24 9.06 9.00 9.62   O/Bne 295 0
10 V* V850 Cen HXB 13 01 17.0966951298 -61 36 06.636402972   15.6 14.40     B2Vne 286 0
11 GSC 03588-00834 HXB 21 03 35.7101268891 +45 45 05.568943629   15.34 14.20 13.49 12.75 B0Ve 156 0
12 2MASS J21342037+4738002 HXB 21 34 20.3718012674 +47 38 00.206178882   14.68 14.16 13.80 13.42 ~ 16 0

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2021.09.22-00:43:49

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