Millisecond Pulsars and Black Holes in Globular Clusters. (arXiv:1902.05963v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ye_C/0/1/0/all/0/1">Claire S. Ye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kremer_K/0/1/0/all/0/1">Kyle Kremer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_S/0/1/0/all/0/1">Sourav Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_C/0/1/0/all/0/1">Carl L. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasio_F/0/1/0/all/0/1">Frederic A. Rasio</a>
Over a hundred millisecond radio pulsars (MSPs) have been observed in
globular clusters (GCs), motivating theoretical studies of the formation and
evolution of these sources through stellar evolution coupled to stellar
dynamics. Here we study MSPs in GCs using realistic $N$-body simulations with
our Cluster Monte Carlo code. We show that neutron stars (NSs) formed in
electron-capture supernovae (including both accretion-induced and
merger-induced collapse of white dwarfs) can be spun up through mass transfer
to form MSPs. Both NS formation and spin-up through accretion are greatly
enhanced through dynamical interaction processes. We find that our models for
average GCs at the present day with masses $approx 2 times 10^5,M_odot$ can
produce up to $10-20$ MSPs, while a very massive GC model with mass $approx
10^6,M_odot$ can produce close to $100$. We show that the number of MSPs is
anti-correlated with the total number of stellar-mass black holes (BHs)
retained in the host cluster. The radial distributions are also affected: MSPs
are more concentrated towards the center in a host cluster with a smaller
number of retained BHs. As a result, the number of MSPs in a GC could be used
to place constraints on its BH population. Intrinsic properties of our model
pulsars, such as their magnetic fields and spin periods, although hard to
determine precisely, are in good overall agreement with observations.
Interestingly, our models also demonstrate the possibility of dynamically
forming NS–NS and NS–BH binaries in GCs, although the predicted numbers are
very small.
Over a hundred millisecond radio pulsars (MSPs) have been observed in
globular clusters (GCs), motivating theoretical studies of the formation and
evolution of these sources through stellar evolution coupled to stellar
dynamics. Here we study MSPs in GCs using realistic $N$-body simulations with
our Cluster Monte Carlo code. We show that neutron stars (NSs) formed in
electron-capture supernovae (including both accretion-induced and
merger-induced collapse of white dwarfs) can be spun up through mass transfer
to form MSPs. Both NS formation and spin-up through accretion are greatly
enhanced through dynamical interaction processes. We find that our models for
average GCs at the present day with masses $approx 2 times 10^5,M_odot$ can
produce up to $10-20$ MSPs, while a very massive GC model with mass $approx
10^6,M_odot$ can produce close to $100$. We show that the number of MSPs is
anti-correlated with the total number of stellar-mass black holes (BHs)
retained in the host cluster. The radial distributions are also affected: MSPs
are more concentrated towards the center in a host cluster with a smaller
number of retained BHs. As a result, the number of MSPs in a GC could be used
to place constraints on its BH population. Intrinsic properties of our model
pulsars, such as their magnetic fields and spin periods, although hard to
determine precisely, are in good overall agreement with observations.
Interestingly, our models also demonstrate the possibility of dynamically
forming NS–NS and NS–BH binaries in GCs, although the predicted numbers are
very small.
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