A radial velocity study of the dwarf nova TZ Persei

Details A radial velocity study of the dwarf nova TZ Persei A radial velocity study of the dwarf nova TZ Persei

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.274..127r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 274, Issue 1, pp. 127-133.

Astronomy and Astrophysics

Astronomy

4

Accretion, Accretion Discs, Binaries: Spectroscopic, Stars: Individual: Tz Per, Novae, Cataclysmic Variables

Scientific paper

A radial velocity study of the Hα emission line of the dwarf nova TZ Per is presented. TZ Per has a spectroscopic period of 6.2520+/-0.0096h. With this period and published JHK photometry, a distance of >~380 pc is inferred. This Z Cam star has both slow outbursts and a short outburst cycle, and time-resolved spectra were obtained on both the rise and the decline of a dwarf nova outburst. TZ Per does not obey the relation between orbital period and outburst decline time found by Bailey and calibrated by Szkody & Mattei. This is probably because the disc is hot all the time, relative to dwarf novae such as U Gem or SS Cyg.

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