Radio Emission from the unbound Debris of Tidal Disruption Events. (arXiv:1903.02575v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Yalinewich_A/0/1/0/all/0/1">Almog Yalinewich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steinberg_E/0/1/0/all/0/1">Elad Steinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piran_T/0/1/0/all/0/1">Tsvi Piran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krolik_J/0/1/0/all/0/1">Julian H. Krolik</a>
When a star gets too close to a supermassive black hole, it is torn apart by
the tidal forces. Roughly half of the stellar mass becomes unbound and flies
away at tremendous velocities. In this work we explore the idea that the shock
produced by the interaction of the unbound debris with the ambient medium gives
rise to the synchrotron radio emission observed in several TDEs. We use a
moving mesh numerical simulation to study the evolution of the unbound debris
and the bow shock around it. We find that as the periapse distance of the star
decreases, the outflow becomes faster and wider. A tidal disruption event whose
periapse distance is a factor of 7 smaller than the tidal radius can account
for the radio emission observed in ASASSN-14li. This model also allows us to
obtain a more accurate estimate for the gas density around the centre of the
host galaxy of ASASSN-14li.
When a star gets too close to a supermassive black hole, it is torn apart by
the tidal forces. Roughly half of the stellar mass becomes unbound and flies
away at tremendous velocities. In this work we explore the idea that the shock
produced by the interaction of the unbound debris with the ambient medium gives
rise to the synchrotron radio emission observed in several TDEs. We use a
moving mesh numerical simulation to study the evolution of the unbound debris
and the bow shock around it. We find that as the periapse distance of the star
decreases, the outflow becomes faster and wider. A tidal disruption event whose
periapse distance is a factor of 7 smaller than the tidal radius can account
for the radio emission observed in ASASSN-14li. This model also allows us to
obtain a more accurate estimate for the gas density around the centre of the
host galaxy of ASASSN-14li.
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