Dust formation in embryonic pulsar-aided supernovae. (arXiv:1812.04773v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Omand_C/0/1/0/all/0/1">Conor Omand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kashiyama_K/0/1/0/all/0/1">Kazumi Kashiyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murase_K/0/1/0/all/0/1">Kohta Murase</a>
We investigate effects of energetic pulsar wind nebulae (PWNe) on dust
formation and evolution. Dust emission has been observed in many supernova
remnants that also have neutron stars as compact remnants. We study the
dependence of dust formation time and size on properties of the ejecta and
central pulsar. We find that a pulsar with an initial spin period $P sim
1mbox{-}10,rm ms$ and a dipole magnetic field $B sim 10^{12mbox{-}15},rm
G$ can either accelerate or delay dust formation, with a timescale of several
months to over ten years, and reduce the average size of dust by a factor of
$sim$ 10 or more compared to the non-pulsar case. We also find that infrared
dust emission may be detectable in typical superluminous supernovae out to
$sim$ 100-1000 Mpc in 2-5 years after the explosion, although this depends
sensitively on the spectral index of nonthermal emission from the nebula. We
discuss implications to previous supernova observations. Some discrepancies
between dust formation models and observations, such as the formation time in
SN1987A or the dust size in the Crab Nebula, could be explained by the
influence of a pulsar, and knowledge of the dust emission will be important for
future ALMA observations of superluminous supernovae.
We investigate effects of energetic pulsar wind nebulae (PWNe) on dust
formation and evolution. Dust emission has been observed in many supernova
remnants that also have neutron stars as compact remnants. We study the
dependence of dust formation time and size on properties of the ejecta and
central pulsar. We find that a pulsar with an initial spin period $P sim
1mbox{-}10,rm ms$ and a dipole magnetic field $B sim 10^{12mbox{-}15},rm
G$ can either accelerate or delay dust formation, with a timescale of several
months to over ten years, and reduce the average size of dust by a factor of
$sim$ 10 or more compared to the non-pulsar case. We also find that infrared
dust emission may be detectable in typical superluminous supernovae out to
$sim$ 100-1000 Mpc in 2-5 years after the explosion, although this depends
sensitively on the spectral index of nonthermal emission from the nebula. We
discuss implications to previous supernova observations. Some discrepancies
between dust formation models and observations, such as the formation time in
SN1987A or the dust size in the Crab Nebula, could be explained by the
influence of a pulsar, and knowledge of the dust emission will be important for
future ALMA observations of superluminous supernovae.
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