Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292..481a&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 2, p. 481-493
Astronomy and Astrophysics
Astrophysics
20
Absorption Spectra, Cataclysmic Variables, Dwarf Novae, Emission Spectra, Light Curve, Radial Velocity, Astronomical Spectroscopy, Balmer Series, Charge Coupled Devices, Helium, Hydrogen, Mass Ratios, Mass Transfer, Reflecting Telescopes, Spectrographs, Temporal Resolution
Scientific paper
Time resolved spectroscopy is presented of the SU UMa type dwarf nova VY Aqr in superoutburst and quiescence. From the radial velocity variations found in outburst I derive on the basis of the value for the superhump period an orbital period of 0.06348 (12) days (or possibly 0.06787(13) days). The radial-velocity amplitude is 29(5) km/s. In the outburst spectra taken approximately 5 days after maximum light evidence is found for the presence of a blue shifted narrow emission component superposed on the broad absorption lines, which is not found in spectra taken 2 nights later. Also a change of approximately 150 km/s in the system velocity is found over these 2 nights. Using various observational constraints I derive q = MWD/MRD approximately equal 8-10 and i approximately equal 30-40 deg. The orbital period and mass ratio of VY Aqr are very similar to those of the well known SU UMa type dwarf nova OY Car. However, the amplitudes of the outburst in VY Aqr are approximately 3 magnitude larger than those of OY Car. I argue that this is due to a lower mass transfer rate during quiescence in VY Aqr compared to OY Car, which results in VY Aqr being relatively fainter in quiescence.
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