Mass ratio in SS433 revisited. (arXiv:1902.11137v1 [astro-ph.HE])

Mass ratio in SS433 revisited. (arXiv:1902.11137v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Cherepashchuk_A/0/1/0/all/0/1">A.M. Cherepashchuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Postnov_K/0/1/0/all/0/1">K.A. Postnov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Belinski_A/0/1/0/all/0/1">A.A. Belinski</a> (Sternberg Astronomical Institute, Moscow)

We revisit the determination of binary mass ratio in the Galactic microquasar
SS433 based on recent GRAVITY VLTI measurements of mass and angular momentum
outflow through a circumbinary disc. The new observations combined with the
constancy of the binary orbital period over $sim 30$ yrs confirm that the mass
ratio in SS433 is $q=M_mathrm{x}/M_mathrm{v}gtrsim 0.6$. For the assumed
optical star mass $M_mathrm{v}$ ranging from $sim 8$ to 15 $M_odot$ such a
mass ratio suggests a low limit of the compact object mass of $M_mathrm{x}sim
5-9 M_odot$, placing the compact object in SS433 as a stellar-mass black hole.

We revisit the determination of binary mass ratio in the Galactic microquasar
SS433 based on recent GRAVITY VLTI measurements of mass and angular momentum
outflow through a circumbinary disc. The new observations combined with the
constancy of the binary orbital period over $sim 30$ yrs confirm that the mass
ratio in SS433 is $q=M_mathrm{x}/M_mathrm{v}gtrsim 0.6$. For the assumed
optical star mass $M_mathrm{v}$ ranging from $sim 8$ to 15 $M_odot$ such a
mass ratio suggests a low limit of the compact object mass of $M_mathrm{x}sim
5-9 M_odot$, placing the compact object in SS433 as a stellar-mass black hole.

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