Time-resolved spectrophotometry of the nova-like variable RW Trianguli

Details Time-resolved spectrophotometry of the nova-like variable RW Trianguli Time-resolved spectrophotometry of the nova-like variable RW Trianguli

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..239k&link_type=abstract

Astrophysical Journal, Part 1, vol. 267, Apr. 1, 1983, p. 239-255.

Astronomy and Astrophysics

Astrophysics

56

Eclipsing Binary Stars, Emission Spectra, Stellar Spectrophotometry, Variable Stars, Accretion Disks, H Lines, Helium, Light Curve, Novae, Orbital Elements, Radial Velocity, Stellar Rotation, Temporal Resolution

Scientific paper

Time-resolved, photometric-quality spectra are presented for the nova-like system RW Tri which yield continuum photometry, emission line fluxes, line profiles, and radial velocities at all phases of the period of RW Tri. Results show that the continuum light curve exhibits a deep eclipse and no evidence of a hot spot, and the light curve of the He II 4686 emission line has an eclipse centered on the continuum eclipse and of equal duration. The He II emission region is found to rotate at only a fraction of the expected Keplerian velocity and the wings of the emission line do not shrink in eclipse as expected for a rotationally broadened line. The He I emission line is determined to show the double component structure expected from an accretion disk and has a rotational velocity three times larger than that of He II. Narrow He I absorption lines are found which show radial velocity variations in phase with the emission lines. A third emission line component is detected which is visible for only one-half of the orbital period with radial velocity variations approximately 180 degrees out of phase with those of the disk. A model is developed in which the He II emission is confined to the inner disk, or to a corona above the inner disk, while the He I and H emission are formed in a much more extended volume.

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