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Modeling Pulsars in dense star clusters

Published online by Cambridge University Press:  11 March 2020

Claire S. Ye Open the ORCID record for Claire S. Ye [Opens in a new window] ,
Kyle Kremer Open the ORCID record for Kyle Kremer [Opens in a new window] ,
Sourav Chatterjee ,
Carl L. Rodriguez  and
Frederic A. Rasio
Claire S. Ye
Affiliation:
Department of Physics & Astronomy, Northwestern University, Evanston, IL60208, USA email: shiye2015@u.northwestern.edu Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA
Kyle Kremer
Affiliation:
Department of Physics & Astronomy, Northwestern University, Evanston, IL60208, USA email: shiye2015@u.northwestern.edu Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA
Sourav Chatterjee
Affiliation:
Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai400005, India
Carl L. Rodriguez
Affiliation:
Harvard Institute for Theory and Computation, 60 Garden St, Cambridge, MA02138, USA
Frederic A. Rasio
Affiliation:
Department of Physics & Astronomy, Northwestern University, Evanston, IL60208, USA email: shiye2015@u.northwestern.edu Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Northwestern University, Evanston, IL60208, USA
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Abstract

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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 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 ≍ 2 × 105M⊙ can produce up to 10 – 20 MSPs, while a very massive GC model with mass ≍ 106M⊙ 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. As a result, the number of MSPs in a GC could be used to place constraints on its BH population. Some intrinsic properties of MSP systems in our models (such as the magnetic fields and spin periods) are in good overall agreement with observations.

Keywords

globular clusters: generalstars: neutronpulsars: generalstars: kinematics and dynamicsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 549 - 552
Copyright
© International Astronomical Union 2020

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