Time-resolved spectrophotometry of the emission lines in the galactic X-ray source H2252-035

Details Time-resolved spectrophotometry of the emission lines in the galactic X-ray source H2252-035 Time-resolved spectrophotometry of the emission lines in the galactic X-ray source H2252-035

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..726c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 267, April 15, 1983, p. 726-731.

Astronomy and Astrophysics

Astrophysics

5

Dwarf Novae, Emission Spectra, Galactic Radiation, Stellar Spectrophotometry, X Ray Sources, Accretion Disks, Balmer Series, Electron Density (Concentration), H Lines, Milky Way Galaxy, Orbital Elements, Stellar Mass Accretion, Stellar Models, Temporal Resolution

Scientific paper

The galactic X-ray source H2252-035 has been the object of a concentrated observational effort, since Griffiths et al. (1980) have identified it with a cataclysmic variable-like spectrum. Since the observed 859 s periodicity corresponds to the beat frequency between the X-ray and orbital periods, it has been interpreted as related to a reprocessing of the X-ray flux into optical emission in some region of the system which is rotating with the orbital period and heated by beamed X-ray emission from the compact star. In connection with the present investigation, H2252-035 has been observed with a 120 inch (3 m) telescope and image dissector scanner on 1980 September 9/10 and on 1981 September 20/21. At a time resolution of approximately 2 minutes, four bright emission lines showed short time-scale flickering and a pronounced orbital period variation in phase with the continuum modulation. A two-component model for the line emission region is proposed.

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