A necessary condition for supernova fallback invading newborn neutron-star magnetosphere. (arXiv:2103.09461v3 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Zhong_Y/0/1/0/all/0/1">Yici Zhong</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:+Shigeyama_T/0/1/0/all/0/1">Toshikazu Shigeyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takasao_S/0/1/0/all/0/1">Shinsuke Takasao</a>
We numerically investigate the dynamics of a supernova fallback accretion
confronting with a relativistic wind from a newborn neutron star (NS). The time
evolution of the accretion shock in the radial direction is basically
characterized by the encounter radius of the flow $r_mathrm{enc}$ and a
dimensionless parameter $zeta equiv L/dot M_mathrm{fb}c^2$, where $L$ is
the NS wind luminosity and $dot M_mathrm{fb}$ is the fallback mass accretion
rate. We find that the critical condition for the fallback matter to reach near
the NS surface can be simply described as $zeta < zeta_mathrm{min} equiv
GM_*/c^2r_mathrm{enc}$ or $r_mathrm{enc}L/G M_* dot M_mathrm{fb} < 1$
independent of the wind Lorentz factor, where $M_*$ is the NS mass. With
combining the condition for the fallback matter to bury the surface magnetic
field under the NS crust, we discuss the possibility that the trifurcation of
NSs into rotation-powered pulsars, central compact objects (CCOs), and
magnetars can be induced by supernova fallback.
We numerically investigate the dynamics of a supernova fallback accretion
confronting with a relativistic wind from a newborn neutron star (NS). The time
evolution of the accretion shock in the radial direction is basically
characterized by the encounter radius of the flow $r_mathrm{enc}$ and a
dimensionless parameter $zeta equiv L/dot M_mathrm{fb}c^2$, where $L$ is
the NS wind luminosity and $dot M_mathrm{fb}$ is the fallback mass accretion
rate. We find that the critical condition for the fallback matter to reach near
the NS surface can be simply described as $zeta < zeta_mathrm{min} equiv
GM_*/c^2r_mathrm{enc}$ or $r_mathrm{enc}L/G M_* dot M_mathrm{fb} < 1$
independent of the wind Lorentz factor, where $M_*$ is the NS mass. With
combining the condition for the fallback matter to bury the surface magnetic
field under the NS crust, we discuss the possibility that the trifurcation of
NSs into rotation-powered pulsars, central compact objects (CCOs), and
magnetars can be induced by supernova fallback.
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