Tidal disruptions of rotating stars by a supermassive black hole. (arXiv:1901.05644v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kagaya_K/0/1/0/all/0/1">Kazuki Kagaya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_S/0/1/0/all/0/1">Shin'ichirou Yoshida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tanikawa_A/0/1/0/all/0/1">Ataru Tanikawa</a>
We compare mass infall rates of tidal-disruption debris of a non-rotating and
of a rotating star when they come close to a supermassive black hole at the
center of a galaxy. Remarkably the mass distribution of debris bound to the
black hole as a function of specific energy shows clear difference between
rotating and non-rotating stars, even if the stellar rotation is far from the
break-up limit. The debris of a star whose initial spin is parallel to the
orbital angular momentum has a mass distribution which extends to lower energy
than that of non-rotating star. The debris of a star with anti-parallel spin
has a larger energy compared with a non-rotating counterpart. As a result,
debris from a star with anti-parallel spin is bound more tightly and the
mass-infall rate rises later in time, while that of a star with a parallel spin
is loosely bound and falls back to the black hole earlier. The different rising
timescales of mass-infall rate may affect the early phase of flares due to the
tidal disruptions.
We compare mass infall rates of tidal-disruption debris of a non-rotating and
of a rotating star when they come close to a supermassive black hole at the
center of a galaxy. Remarkably the mass distribution of debris bound to the
black hole as a function of specific energy shows clear difference between
rotating and non-rotating stars, even if the stellar rotation is far from the
break-up limit. The debris of a star whose initial spin is parallel to the
orbital angular momentum has a mass distribution which extends to lower energy
than that of non-rotating star. The debris of a star with anti-parallel spin
has a larger energy compared with a non-rotating counterpart. As a result,
debris from a star with anti-parallel spin is bound more tightly and the
mass-infall rate rises later in time, while that of a star with a parallel spin
is loosely bound and falls back to the black hole earlier. The different rising
timescales of mass-infall rate may affect the early phase of flares due to the
tidal disruptions.
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