The nature of Aquila X-1

Details The nature of Aquila X-1 The nature of Aquila X-1

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978natur.271..633m&link_type=abstract

Nature, vol. 271, Feb. 16, 1978, p. 633, 634. NASA-supported research.

Computer Science

7

Stellar Models, Stellar Spectrophotometry, Ubv Spectra, X Ray Sources, Atmospheric Heating, Companion Stars, Dwarf Stars, Eddington Approximation, Electrophotometry, Interstellar Extinction, Mass Transfer, Roche Limit, Stellar Atmospheres, Supernovae, X Ray Stars

Scientific paper

Photometry in the UBV spectra was used to observe Aquila X-1. This X-ray source, usually producing flux on the order of 1-10% that of the Crab Nebula, often behaves in a manner resembling the behavior of galactic X-ray stars. A description of the calibration methods used in the observations is presented, with attention to photoelectric-photographic methods. These observations suggest a quiescent spectral class near Ko, i.e., a dwarf at a distance of 1.6 kpc. The more intense X-ray emissions are said to be generated from internal heating of the stellar atmosphere, with additional energy supplied by a low-mass companion star. This explaination is at variance with the semi-detached Roche model.

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