A stripped-companion origin for Be stars: clues from the putative black holes HR 6819 and LB-1

TLDR: In this paper, the authors disentangle the observed composite spectra into two components: a rapidly rotating Be star and a slowly rotating B star with low surface gravity, and show that the system is a binary and does not contain a detached black hole.

Abstract: HR 6819 is a bright ($V=536$), blue star recently proposed to be a triple containing a detached black hole (BH) We show that the system is a binary and does not contain a BH Using spectral decomposition, we disentangle the observed composite spectra into two components: a rapidly rotating Be star and a slowly rotating B star with low surface gravity $(\log g \approx 275)$ Both stars show periodic radial velocity (RV) variability, but the RV semi-amplitude of the B star's orbit is $K_{\rm B}= (627 \pm 1)\,\rm km\,s^{-1}$, while that of the Be star is only $K_{\rm Be} = (45\pm 2)\,\rm km\,s^{-1}$ This implies that the B star is less massive by at least a factor of 10 The surface abundances of the B star bear imprints of CNO burning We argue that the B star is a bloated, recently stripped helium star with mass $\approx 05\,M_{\odot}$ that is currently contracting to become a hot subdwarf The orbital motion of the Be star obviates the need for a BH to explain the B star's motion A stripped-star model reproduces the observed luminosity of the system, while a normal star with the B star's temperature and gravity would be more than 10 times too luminous HR 6819 and the binary LB-1 probably formed through similar channels We use MESA models to investigate their evolutionary history, finding that they likely formed from intermediate-mass ($3-7\,M_{\odot}$) primaries stripped by slightly lower-mass secondaries and are progenitors to Be + sdOB binaries such as $\phi$ Persei The lifetime of their current evolutionary phase is on average $2\times 10^5$ years, of order half a percent of the total lifetime of the Be phase This implies that many Be stars have hot subdwarf and white dwarf companions, and that a substantial fraction ($20-100\%$) of field Be stars form through accretion of material from a binary companion