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Title:
On isolated millisecond pulsars formed by the coalescence of neutron stars and massive white dwarfs
Authors:
Sun, Shengnan; Li, Lin; Liu, Helei; Lü, Guoliang; Wang, Zhaojun; Zhu, Chunhua
Affiliation:
AA(School of Physical Science and Technology, Xinjiang University, Urumqi, Xinjiang 830046, China), AB(School of Physical Science and Technology, Xinjiang University, Urumqi, Xinjiang 830046, China; Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1st Street, Urumqi, Xinjiang 830011, China; Key Laboratory of Electronic Equipment Structure Design, Ministry of Education, Xidian University, Xian, Shaanxi 710071, China), AC(School of Physical Science and Technology, Xinjiang University, Urumqi, Xinjiang 830046, China), AD(School of Physical Science and Technology, Xinjiang University, Urumqi, Xinjiang 830046, China), AE(School of Physical Science and Technology, Xinjiang University, Urumqi, Xinjiang 830046, China), AF(School of Physical Science and Technology, Xinjiang University, Urumqi, Xinjiang 830046, China)
Publication:
Publications of the Astronomical Society of Australia, Volume 36, id. e005 (PASA Homepage)
Publication Date:
02/2019
Origin:
CUP
Astronomy Keywords:
pulsars, general stars, neutron star, white dwarf
Abstract Copyright:
2019: Astronomical Society of Australia
DOI:
10.1017/pasa.2018.51
Bibliographic Code:
2019PASA...36....5S

Abstract

This paper uses population synthesis to investigate the possible origin of isolated millisecond pulsars as born from the coalescence of a neutron star and a white dwarf. Results show that the galactic birth rate of isolated millisecond pulsars is likely to lie between 5.8×10-5 yr-1 and 2.0×10-4 yr-1, depending on critical variables, such as the stability of mass transfer via the Roche lobe and the value of kick velocity. In addition to this, this paper estimates that the solar mass of isolated millisecond pulsars can range from 1.5 and 2.0 Mʘ, making them more massive than other `normal' pulsars. Finally, the majority of isolated millisecond pulsars in our simulations have spin periods ranging from several to 20 ms, which is consistent with previous observations.
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