Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...263..277w&link_type=abstract
Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 277-288.
Astronomy and Astrophysics
Astrophysics
85
B Stars, Main Sequence Stars, Neutron Stars, X Ray Sources, X Ray Stars, Binary Stars, Cassiopeia Constellation, Companion Stars, Early Stars, O Stars, Stellar Magnitude, Stellar Mass Accretion, Stellar Rotation, White Dwarf Stars
Scientific paper
The greater than 0.0001 solar mass/year loss rates required to power X-ray sources, if associated compact objects are white dwarfs, are many orders of magnitude greater than even the highest estimates for the main sequence Be stars Chi Per and Gamma Cas, confirming that the compact objects in these systems are neutron stars. While observed mass loss rates are of the order of that required to power the X-ray emission from a neutron star, X-ray measurements have established rates at least an order of magnitude above UV estimates, supporting earlier suggestions of an inclination dependence in the mass loss from rapidly rotating main sequence OB stars which results in mass loss rates in the orbital plane that are at least one order of magnitude higher, or terminal velocities that are at least a factor of 2.0 lower, than is indicated by UV measurements.
Holt Stephen S.
Parmar Arvind N.
Swank Jean H.
White Nicholas E.
No associations
LandOfFree
A comparison of the X-ray properties of X Persei and Gamma Cassiopeiae 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 A comparison of the X-ray properties of X Persei and Gamma Cassiopeiae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A comparison of the X-ray properties of X Persei and Gamma Cassiopeiae will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-927934