Ejecta-circumstellar medium interaction in high-density environment to kilonova emission: Application for GRB 191019A. (arXiv:2401.14418v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wang_S/0/1/0/all/0/1">Suo-Ning Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_H/0/1/0/all/0/1">Hou-Jun Lü</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_Y/0/1/0/all/0/1">Yong Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_H/0/1/0/all/0/1">Hao-Yu Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rice_J/0/1/0/all/0/1">Jared Rice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_M/0/1/0/all/0/1">Meng-Hua Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liang_E/0/1/0/all/0/1">En-Wei Liang</a>
The nearby long-duration GRB 191019A recently detected by {em Swift} lacks
an associated supernova and belongs to a host galaxy with little star formation
activity, suggesting that the origin of this burst is the result of the merger
of two compact objects with dynamical interactions in a high-density medium of
an active galactic nucleus (AGN). By motivating of this event, it occurs in
such high-density environment, the ejecta- circumstellar medium (CSM)
interaction cannot be ignored to contribute a possible kilonova emission. Here,
we theoretically calculate the kilonova emission by considering the
contribution of the ejecta-CSM interaction in the high-density environment. We
find that the contribution to the kilonova emission from the ejecta-CSM
interaction will dominate at a later time, and a smaller ejecta mass will have
a stronger kilonova emission from the ejecta-CSM interaction. Moreover, we try
to apply it to GRB 191019A, but we find that it is difficult to identify the
possible kilonova emission from the observations due to the contribution of the
bright host galaxy. On the other hand, it requires a less injected mass (less
than $M_{rm ej}=2times10^{-5}M_{odot}$) if one can detect the kilonova
emission associated with a GRB 191019A-like event in the future. The
r-process-powered and spin energy contributions from the magnetar are also
discussed.
The nearby long-duration GRB 191019A recently detected by {em Swift} lacks
an associated supernova and belongs to a host galaxy with little star formation
activity, suggesting that the origin of this burst is the result of the merger
of two compact objects with dynamical interactions in a high-density medium of
an active galactic nucleus (AGN). By motivating of this event, it occurs in
such high-density environment, the ejecta- circumstellar medium (CSM)
interaction cannot be ignored to contribute a possible kilonova emission. Here,
we theoretically calculate the kilonova emission by considering the
contribution of the ejecta-CSM interaction in the high-density environment. We
find that the contribution to the kilonova emission from the ejecta-CSM
interaction will dominate at a later time, and a smaller ejecta mass will have
a stronger kilonova emission from the ejecta-CSM interaction. Moreover, we try
to apply it to GRB 191019A, but we find that it is difficult to identify the
possible kilonova emission from the observations due to the contribution of the
bright host galaxy. On the other hand, it requires a less injected mass (less
than $M_{rm ej}=2times10^{-5}M_{odot}$) if one can detect the kilonova
emission associated with a GRB 191019A-like event in the future. The
r-process-powered and spin energy contributions from the magnetar are also
discussed.
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