Everything that glitters is not gold: V1315 Cas is not a dormant black hole

Author:

Zak J12ORCID,Jones D234ORCID,Boffin H M J1ORCID,Beck P G235ORCID,Klencki J1,Bodensteiner J1,Shenar T6ORCID,Van Winckel H7,Skarka M89ORCID,Arellano-Córdova K10,Viuho J411,Sowicka P12ORCID,Guenther E W13ORCID,Hatzes A13

Affiliation:

1. European Southern Observatory , D-85748 Garching, Germany

2. Instituto de Astrofísica de Canarias , E-38200 La Laguna, Tenerife, Spain

3. Departamento de Astrofísica, Universidad de La Laguna , E-38206 La Laguna, Tenerife, Spain

4. Nordic Optical Telescope , Rambla José Ana Fernández Pérez 7, E-38711 Breña Baja, Spain

5. Institut für Physik, Karl-Franzens Universität Graz, Universitätsplatz 5/II , NAWI Graz, A-8010 Graz, Austria

6. Anton Pannekoek Institute for Astronomy, University of Amsterdam , 1090 GE Amsterdam , the Netherlands

7. Institute of Astronomy , KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium

8. Department of Theoretical Physics and Astrophysics, Masaryk Univesity , Kotlářská 2, CZ-60200 Brno, Czech Republic

9. Astronomical Institute of the Czech Academy of Sciences , Fričova 298, CZ-25165 Ondřejov, Czech Republic

10. Institute for Astronomy, University of Edinburgh , Royal Observatory, Edinburgh EH9 3HJ, UK

11. DAWN, Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark

12. Nicolaus Copernicus Astronomical Center , Bartycka 18, PL-00-716 Warsaw, Poland

13. Thueringer Landessternwarte Tautenburg , Sternwarte 5, D-07778 Tautenburg, Germany

Abstract

ABSTRACT The quest for quiet or dormant black holes has been ongoing since several decades. Ellipsoidal variables possibly indicate the existence of a very high-mass invisible companion and are thought to be one of the best ways to find such dormant black holes. This, however, is not a panacea as we show here with one example. We indeed report the discovery of a new semidetached interacting binary, V1315 Cas, discovered as an ellipsoidal variable. Using data from photometric surveys (ASAS-SN, TESS) and high-resolution spectroscopy, we derived a nearly circular orbit with an orbital period of Porb = 34.54 d. The binary system consists of an evolved F-type star primary that is likely still filling its Roche lobe and a B-type star secondary. Using phoebe2, we derived the following masses and radii: for the primary, $M_p =0.84 \pm 0.03 \, \rm {M}_{\odot}$ and $R_p =18.51^{+0.12}_{-0.07} \, \rm {R}_{\odot}$; for the secondary, $M_s =7.3 \pm 0.3 \, \rm {M}_{\odot}$ and $R_s =4.02^{+2.3}_{-2.0}\, \rm {R}_{\odot}$. Modelling the evolution of the system with mesa, we found an age of ∼7.7 × 107 yr. The system is at the end of a period of rapid non-conservative mass transfer that reversed its mass ratio, while significantly widening its orbit. The primary shows carbon depletion and nitrogen overabundance, indicative of CNO-processed material being exposed due to mass transfer. An infrared excess and stationary H α emission suggest the presence of a circumstellar or circumbinary disc. V1315 Cas will likely become a detached stripped star binary.

Funder

European Union

FWO

KU Leuven

Spanish Ministry of Science and Innovation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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