Computer Science
Scientific paper
Aug 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.304..423h&link_type=abstract
Nature (ISSN 0028-0836), vol. 304, Aug. 4, 1983, p. 423-425.
Computer Science
50
Emission Spectra, Pulsars, Stellar Evolution, Stellar Models, X Ray Sources, Main Sequence Stars, Neutron Stars, Red Giant Stars, Stellar Magnetic Fields, Stellar Mass Accretion, Stellar Temperature, White Dwarf Stars
Scientific paper
An upper bound is calculated for the X ray luminosity of the binary pulsar PSR1953+29 and discussed in terms of effects on theretical models for the pulsar's formation and spin-up. The upper limit was obtained by summing the detected counts measured by the Einstein Observatory within a circle of radius 150 arcsec and subtracting local background fluxes. A flux upper bound of less than 4 x 10 to the 32 erg/sec, a neutron star radius of 15 km, a temperature less than 1,000,000 K, and a pulsar age of at least 3000 year are obtained. The neutron star could be much older than 10,000,000 yr, the spin-down rate is up to 10 to the minus 17 str/sec, and formation occurred by accretion when the companion was in a red giant phase. The pulsar has a mass of about 0.3 solar mass, travels an orbit of about 10 to the 13 cm, and evolved from a white dwarf near its Chandrasekhar limit. It is suggested that the magnetic surface field of the pulsar has stabilized near 1 billion G.
Helfand David J.
Ruderman Malvin A.
Shaham Jacob
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