Is the 1.5-ms pulsar a young neutron star?

Details Is the 1.5-ms pulsar a young neutron star? Is the 1.5-ms pulsar a young neutron star?

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986natur.323..786b&link_type=abstract

Nature (ISSN 0028-0836), vol. 323, Oct. 30, 1986, p. 786-788. NASA-supported research.

Computer Science

37

Companion Stars, Early Stars, Neutron Stars, Pulsars, Stellar Mass Accretion, B Stars, O Stars, Stellar Evolution, Stellar Magnetic Fields, Thermomagnetic Effects

Scientific paper

The 1.5 ms pulsar PSR 1937+214 is an unusual object; its extremely short period and slow spin-down rate imply a magnetic field of 4×108G, much lower than that of a canonical pulsar. The authors propose that PSR 1937+214 is a young neutron star spun up by accretion from a high-mass companion in a close binary system. The super-critical mass transfer rates expected in such a binary system should allow the neutron star to be spun up in the comparatively short time of ≡104yr. A high-mass binary system is expected to disrupt when the companion explodes in a supernova. It is claimed that such a spin-up model in a high-mass system can explain the lack of a companion, low magnetic field, and high spin rate of PSR 1937+214.

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