Self-sustained strong mass transfer without Roche lobe overflow - Cygnus X-3

Details Self-sustained strong mass transfer without Roche lobe overflow - Cygnus X-3 Self-sustained strong mass transfer without Roche lobe overflow - Cygnus X-3

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...342l..31t&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 342, July 1, 1989, p. L31-L34.

Astronomy and Astrophysics

Astrophysics

29

Cygnus Constellation, Mass Transfer, Roche Limit, Stellar Evolution, Stellar Winds, X Ray Binaries, Companion Stars, Neutron Stars, Self Excitation

Scientific paper

It is proposed that the binary evolution of Cyg X-3 is driven by a self-excited wind from a solar composition companion star sustained by radiation from a neutron star primary. Observations would then imply that the companion is a white dwarf underfilling its Roche lobe, with mass between 0.01 and 0.03 solar masses. Cyg X-3 could then be in the late stage of very low mass X-ray binary evolution expected to result in a millisecond pulsar binary similar to the eclipsing system PSR 1957 + 20.

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