Issue |
A&A
Volume 634, February 2020
|
|
---|---|---|
Article Number | L7 | |
Number of page(s) | 8 | |
Section | Letters to the Editor | |
DOI | https://doi.org/10.1051/0004-6361/201937318 | |
Published online | 31 January 2020 |
Letter to the Editor
A detailed non-LTE analysis of LB-1: Revised parameters and surface abundances
1
Instituto de Astrofísica de Canarias, 38 200 La Laguna, Tenerife, Spain
e-mail: ssimon@iac.es
2
Universidad de La Laguna, Universidad de La Laguna, 38 205 La Laguna, Tenerife, Spain
3
Centro de Astrobiología, ESAC campus, Villanueva de la Cañada, 28 692 Villafranca del Castillo, Spain
4
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14 482 Potsdam, Germany
5
Nordic Optical Telescope, Rambla José Ana Fernández Pérez 7, 38 711 Breña Baja, Spain
6
Astrophysics Research Centre, School of Mathematics & Physics, Queen’s University, Belfast BT7 1NN, UK
Received:
14
December
2019
Accepted:
8
January
2020
Context. It has recently been proposed that LB-1 is a binary system at 4 kpc consisting of a B-type star of 8 M⊙ and a massive stellar black hole (BH) of 70 M⊙. This finding challenges our current theories of massive star evolution and formation of BHs at solar metallicity.
Aims. Our objective is to derive the effective temperature, surface gravity, and chemical composition of the B-type component in order to determine its nature and evolutionary status and, indirectly, to constrain the mass of the BH.
Methods. We use the non-LTE stellar atmosphere code FASTWIND to analyze new and archival high-resolution data.
Results. We determine (Teff, log g) values of (14 000 ± 500 K, 3.50 ± 0.15 dex) that, combined with the Gaia parallax, imply a spectroscopic mass, from log g, of 3.2+2.1−1.9 M⊙ and an evolutionary mass, assuming single star evolution, of 5.2+0.3−0.6 M⊙. We determine an upper limit of 8 km s−1 for the projected rotational velocity and derive the surface abundances; we find the star to have a silicon abundance below solar, and to be significantly enhanced in nitrogen and iron and depleted in carbon and magnesium. Complementary evidence derived from a photometric extinction analysis and Gaia yields similar results for Teff and log g and a consistent distance around 2 kpc.
Conclusions. We propose that the B-type star is a slightly evolved main sequence star of 3–5 M⊙ with surface abundances reminiscent of diffusion in late B/A chemically peculiar stars with low rotational velocities. There is also evidence for CN-processed material in its atmosphere. These conclusions rely critically on the distance inferred from the Gaia parallax. The goodness of fit of the Gaia astrometry also favors a high-inclination orbit. If the orbit is edge-on and the B-type star has a mass of 3–5 M⊙, the mass of the dark companion would be 4–5 M⊙, which would be easier to explain with our current stellar evolutionary models.
Key words: techniques: spectroscopic / binaries: spectroscopic / stars: black holes / stars: abundances / stars: early-type / stars: fundamental parameters
© ESO 2020
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