Analysis of the Southern Eclipsing Variables V431 Sagittarii, V576 Centauri, BF Pavonis, and AT Aquarii

Details Analysis of the Southern Eclipsing Variables V431 Sagittarii, V576 Centauri, BF Pavonis, and AT Aquarii Analysis of the Southern Eclipsing Variables V431 Sagittarii, V576 Centauri, BF Pavonis, and AT Aquarii

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...199.0601s&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #06.01; Bulletin of the American Astronomical Society, Vol. 33, p.1310

Astronomy and Astrophysics

Astronomy

Scientific paper

We present an update on our analyses of unpublished, complete light curves for V431 Sagittarii (BVRcIc), BF Pavonis (BVRcIc), V576 Centauri (UBVRcIc), and AT Aquarii (BVRcIc). Preliminary light curve analyses and standard magnitudes are presented. We correct one eclipse timing for V431 Sgr, J.D. 2448130.6145(3) given at AAS 197,Poster #129.08, so that the improved ephemeris is J.D. Hel Min I = 2448127.5959(2)d + 0.27388054(16)XE. The improved ephemerides for V576 Cen, and AT Aquarii are 2448695.5787(34)d + 0.37802984(14)XE and 2448125.6132(25)d + 0.30409545(37)XE, respectively. For most of the history of BF Pav, the period has remained at a constant 0.3055790(25)d. However, measurements over the most recent 500 or so orbits may show a startling period change to 0.30231788(26)d. Observers are urged to take more times of minima on this interesting eclipsing binary. These analyses was conducted entirely by nine undergraduate students during the fall semester, 2001. This research was partially supported by a grant from NASA administered by the American Astronomical Society. These observations were taken by R.G.S. at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc. under contract with the National Science Foundation.

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