The circumstellar matter of type II intermediate luminosity optical transients (ILOTs). (arXiv:2010.14490v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Soker_N/0/1/0/all/0/1">Noam Soker</a> (Technion, Israel)
I find that a 0.1-1Mo outflowing equatorial dusty disk (torus) that the
binary system progenitor of an intermediate luminosity optical transient (ILOT)
ejects several years to several months before and during the outburst can
reduce the total emission to an equatorial observer by two orders of magnitude
and shifts the emission to wavelengths of mainly >10mum. This is termed a type
II ILOT (ILOT II). To reach this conclusion I use calculations of type II
active galactic nuclei and apply them to the equatorial ejecta (disk/torus) of
ILOTs II. This reduction in emission can last for tens of years after outburst.
Most of the radiation escapes along the polar directions. The attenuation of
the emission for wavelengths of <5mum can be more than three orders of
magnitudes, and the emission at <2mum is negligible. Jets that the binary
system launches during the outburst can collide with polar CSM and emit
radiation above the equatorial plane and dust in the polar outflow can reflect
emission from the central source. Therefore, during the event itself the
equatorial observer might detect an ILOT. I strengthen the previously suggested
ILOT II scenario to the event N6946-BH1, where a red giant star disappeared in
the visible.
I find that a 0.1-1Mo outflowing equatorial dusty disk (torus) that the
binary system progenitor of an intermediate luminosity optical transient (ILOT)
ejects several years to several months before and during the outburst can
reduce the total emission to an equatorial observer by two orders of magnitude
and shifts the emission to wavelengths of mainly >10mum. This is termed a type
II ILOT (ILOT II). To reach this conclusion I use calculations of type II
active galactic nuclei and apply them to the equatorial ejecta (disk/torus) of
ILOTs II. This reduction in emission can last for tens of years after outburst.
Most of the radiation escapes along the polar directions. The attenuation of
the emission for wavelengths of <5mum can be more than three orders of
magnitudes, and the emission at <2mum is negligible. Jets that the binary
system launches during the outburst can collide with polar CSM and emit
radiation above the equatorial plane and dust in the polar outflow can reflect
emission from the central source. Therefore, during the event itself the
equatorial observer might detect an ILOT. I strengthen the previously suggested
ILOT II scenario to the event N6946-BH1, where a red giant star disappeared in
the visible.
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