Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· References in the article
· Citations to the Article (99) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (3)
· Also-Read Articles (Reads History)
· Translate This Page
A comparison of the X-ray properties of X Persei and Gamma Cassiopeiae
White, N. E.; Swank, J. H.; Holt, S. S.; Parmar, A. N.
AA(NASA, Goddard Space Flight Center, Laboratory for High Energy Astrophysics, Greenbelt; Maryland, University, College Park, MD), AB(NASA, Goddard Space Flight Center, Laboratory for High Energy Astrophysics, Greenbelt, MD), AC(NASA, Goddard Space Flight Center, Laboratory for High Energy Astrophysics, Greenbelt, MD), AD(London, University College, Mullard Space Science Laboratory, Dorking, Surrey, England)
Astrophysical Journal, Part 1, vol. 263, Dec. 1, 1982, p. 277-288. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
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
Bibliographic Code:


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.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences

More Article Retrieval Options

HELP for Article Retrieval

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
arXiv e-prints