Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...146l...3b&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 146, no. 1, May 1985, p. L3-L5.
Astronomy and Astrophysics
Astrophysics
24
Binary Stars, Dwarf Stars, Mass Transfer, Neutron Stars, Angular Momentum, Pulsars, Radii, Stellar Evolution, Stellar Mass
Scientific paper
The authors consider mass transfer from a zero hydrogen abundance electron-degenerate secondary to a 1.4 M_sun; neutron-star primary. They find that for secondary masses: (1) below m2 ≡ 0.005 M_sun;, and (2) between 0.40 M_sun; and 0.66 M_sun;, runaway mass transfer and disruption of the secondary may occur. For m2 ≡ 0.005 M_sun; the instability is reached within the age of the galaxy. For m2 > 0.66 M_sun; the mass transfer is found to be always unstable, whereas for 0.005 M_sun; ≤ m2 ≤ 0.40 M_sun; it is always stable. The amount of angular momentum available in the case of unstable mass transfer from a secondary with mass ≤0.005 M_sun; is insufficient to produce a single radio pulsar with a period <3 milliseconds. Unstable mass transfer from a degenerate companion with m2 > 0.66 M_sun; can, however, produce a 1.55 msec pulsar.
Bonsema F. J. P.
van den Heuvel Edward Peter Jacobus
No associations
LandOfFree
Stability of mass transfer in a neutron star plus degenerate dwarf binary does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Stability of mass transfer in a neutron star plus degenerate dwarf binary, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Stability of mass transfer in a neutron star plus degenerate dwarf binary will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1630427