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Formation of millisecond pulsars - NS initial mass and EOS constraints

Published online by Cambridge University Press:  21 February 2013

Michał Bejger ,
Morgane Fortin ,
Paweł Haensel  and
J. Leszek Zdunik
Michał Bejger
Affiliation:
N. Copernicus Astronomical Center PAS, Bartycka 18, PL-00-716 Warsaw, Poland email: bejger@camk.edu.pl, haensel@camk.edu.pl, jlz@camk.edu.pl
Morgane Fortin
Affiliation:
N. Copernicus Astronomical Center PAS, Bartycka 18, PL-00-716 Warsaw, Poland email: bejger@camk.edu.pl, haensel@camk.edu.pl, jlz@camk.edu.pl LUTH, UMR 8102 du CNRS, Observatoire de Paris, F-92195 Meudon Cedex, France email: morgane.fortin@obspm.fr
Paweł Haensel
Affiliation:
N. Copernicus Astronomical Center PAS, Bartycka 18, PL-00-716 Warsaw, Poland email: bejger@camk.edu.pl, haensel@camk.edu.pl, jlz@camk.edu.pl
J. Leszek Zdunik
Affiliation:
N. Copernicus Astronomical Center PAS, Bartycka 18, PL-00-716 Warsaw, Poland email: bejger@camk.edu.pl, haensel@camk.edu.pl, jlz@camk.edu.pl
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Abstract

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Recent measurement of a high millisecond pulsar mass (PSR J1614-2230, 1.97± 0.04 M⊙) compared with the low mass of PSR J0751+1807 (1.26± 0.14 M⊙) indicates a large span of masses of recycled pulsars and suggests a broad range of neutron stars masses at birth. We aim at reconstructing the pre-accretion masses for these pulsars while taking into account interaction of the magnetic field with a thin accretion disk, magnetic field decay and relativistic 2D solutions for stellar configurations for a set of equations of state. We briefly discuss the evolutionary scenarios leading to the formation of these neutron stars and study the influence of the equation of state.

Keywords

Stars: neutronpulsars: individualaccretion disksequation of statemagnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 109 - 112
Copyright
Copyright © International Astronomical Union 2013

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