MWC 656 is unlikely to contain a black hole

被引：5
|
作者：
Janssens, S. [1 ]
Shenar, T. [2 ]
Degenaar, N. [2 ]
Bodensteiner, J. [3 ]
Sana, H. [1 ]
Audenaert, J. [1 ]
Frost, A. J. [4 ]
机构：
[1] Univ Leuven, KU Leuven, Dept Phys, Celestijnenlaan 200D, B-3001 Leuven, Belgium
[2] Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
[3] European Org Astron Res Southern Hemisphere ESO, Karl-Schwarzschild-Str 2, Garching 85748, Germany
[4] European Southern Observ, Alonso Cordova 3107, Santiago, Chile
来源：
ASTRONOMY & ASTROPHYSICS | 2023年 / 677卷
基金：
欧洲研究理事会;
关键词：
stars: individual: MWC 656; stars: emission-line; Be - binaries: spectroscopic; stars: black holes; X-RAY-EMISSION; CATACLYSMIC VARIABLES; BINARY; STAR; 1ST; SPECTROSCOPY; SPECTROGRAPH; EVOLUTION; II;
D O I：
10.1051/0004-6361/202347318
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Contact. MWC 656 was reported to be the first known Be star with a black-hole (BH) companion on a 60 d period. The mass of the proposed BH companion is estimated to be between 4 and 7 M-circle dot. This estimate is based on radial velocity (RV) measurements derived from the Fe II lambda 4583 emission line of the Be star disc and from the He II lambda 4686 emission line, assumed to be formed in a disc around the putative BH. Aims. Using new high-resolution spectroscopic data, we investigate whether MWC 656 truly contains a BH. Methods. We used the cross-correlation method to calculate the RVs of both the Be star and the He II lambda 4686 emission line to derive a new orbital solution. We also used a spectral disentangling method to look for the spectral signature of a companion. Results. We derived an orbital period of 59.028 +/- 0.011 d and a mass ratio of q = M-He II/M-Be = 0.12 +/- 0.03, much lower than the previously reported value of q = 0.41 +/- 0.07. By adopting a mass for the Be star of M-Be = 7.8 +/- 2.0 M-circle dot, the mass of the companion is 0.94 +/- 0.34 M-circle dot. For the upper limit of M-Be = 16 M-circle dot and q = 0.15, the mass of the companion is 2.4 M-circle dot. Performing the disentangling on mock spectra shows that the spectral signature of a non-degenerate stellar companion with such a low mass cannot be retrieved using our data. Conclusions. Our measurements do not support the presence of a BH companion in MWC 656. Rather, the derived upper limit on the mass of the companion indicates that it is either a neutron star, a white dwarf, or a hot helium star. Far-UV data will aid in rejecting or confirming a hot helium-star companion.
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页数：12
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