Light Variation Curves Associated with Candidate PG Cataclysmic Variable Celestial Bodies

Details Light Variation Curves Associated with Candidate PG Cataclysmic Variable Celestial Bodies Light Variation Curves Associated with Candidate PG Cataclysmic Variable Celestial Bodies

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996stin...9633652j&link_type=abstract

Tiantiwuli Xuebao, vol. 13, p. 225-231

Astronomy and Astrophysics

Astronomy

Astronomical Observatories, Luminosity, Cataclysmic Variables, Eclipsing Binary Stars, Brightness, Telescopes, Charge Coupled Devices, Celestial Bodies

Scientific paper

In 1989, we used the Beijing Astronomical Observatory Xinglong observation station's 60/90/180 centimeter Schmitt telescope as well as Thomson red sensitive CCD to carry out luminosity observations on 14 PG candidate cataclysmic variables. The luminosity curve characteristics clearly show that PG0027 + 260, PG0818 + 513, and PG 1030 + 590 are cataclysmic eclipsing binaries. PG1341--079 is a possible cataclysmic eclipsing binary. PG1551 + 719 is an SU UMa type dwarf nova. Besides this, there are also light change curves associated with 6 celestial bodies which have flickering characteristics of cataclysmic variables. As a result, among PG samples, the success rate for cataclysmic variables is 79% PG1030 + 590's orbital period is 3:279, PG17l7 + 413's flickering change range clearly varies within two months. There is no clear correlation between it and intrinsic brightness. The explanation is that the flickering range changes may possibly be localized effects associated with brightness bands.

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