Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...242..125e&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 242, no. 1, Feb. 1991, p. 125-127.
Astronomy and Astrophysics
Astrophysics
9
Binary Stars, Companion Stars, Pulsars, Stellar Evolution, Stellar Mass Ejection, Evaporation, Missing Mass (Astrophysics), Stellar Magnetic Fields, X Ray Binaries
Scientific paper
Nonconservative evolution of the binary with the evaporation of the secondary, according to the mechanism proposed by van den Heuvel and van Paradijs (1988), depends on the value of f (fraction of the impinging flux responsible for the evaporation), magnetic field strength and pulsar period. For neutron stars with magnetic field strength of 500 million G, if f is above 0.027, the stellar wind from the secondary is so large that the secondary fills its Roche lobe again, and perhaps the accretion and evaporation phases will be altered. For f in the range 0.018 to 0.027, it may be possible for the secondary to evaporate completely. If f is less than 0.018, the evaporation process is almost insignificant. For neutron stars with magnetic field strength of 1 billion and 5 billion G, evaporation is possible if f values are in the ranges of 0.07 to 0.11 and 0.89 to 1 accordingly.
Ergma E. V.
Fedorova Alexandra V.
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