No close companions to a sample of bright sdB stars. (arXiv:2002.04545v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Silvotti_R/0/1/0/all/0/1">Roberto Silvotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ostensen_R/0/1/0/all/0/1">Roy H. Ostensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Telting_J/0/1/0/all/0/1">John H. Telting</a>
In this article we present preliminary results on the upper limits to the
mass of a companion for 8 apparently single subdwarf B stars, derived from
high-precision radial velocity measurements obtained from Harps-N spectra.
These limits, corresponding to a few Jupiter masses, show that these stars do
not have close companions and keep open the unresolved question of the
mechanism that caused the almost complete loss of the envelope for the giant
precursors of these stars. For 4 stars with a larger data coverage, it was also
possible to set upper limits to the mass of a more massive companion in a wider
orbit.
In this article we present preliminary results on the upper limits to the
mass of a companion for 8 apparently single subdwarf B stars, derived from
high-precision radial velocity measurements obtained from Harps-N spectra.
These limits, corresponding to a few Jupiter masses, show that these stars do
not have close companions and keep open the unresolved question of the
mechanism that caused the almost complete loss of the envelope for the giant
precursors of these stars. For 4 stars with a larger data coverage, it was also
possible to set upper limits to the mass of a more massive companion in a wider
orbit.
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