Long-Term VRI Photometry of Pulsating Red Giants

Details Long-Term VRI Photometry of Pulsating Red Giants Long-Term VRI Photometry of Pulsating Red Giants

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.4614p&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #46.14; Bulletin of the American Astronomical Society, Vol. 32, p.1479

Astronomy and Astrophysics

Astronomy

Scientific paper

We report up to 5000 days of VRI photometry, from a robotic photometric telescope, of 37 pulsating red giants, namely: TV Psc, EG And, Z Psc, RZ And, 4 Ori, RX Lep, η Gem, μ Gem, UW Lyn, ψ 1 Aur, V523 Mon, V614 Mon, HD 52690, Y Lyn, BC CMi, X Cnc, UX Lyn, RS Cnc, VY UMa, ST UMa, TU CVn, FS Com, 35 Com, SW Vir, 30 Her, α 1 Her, V642 Her, R Lyr, HD 174621, V450 Aql, V1293 Aql, δ Sge, EU Del, V1070 Cyg, W Cyg, μ Cep, and ν Cep. V, R, and I variations are generally in phase. The length and density of the data enable us to look for variations on time scales ranging from days to years. We use both power-spectrum (Fourier) analysis, and autocorrelation analysis, as well as light-curve analysis; these three approaches are complementary. The variations range from regular to irregular but, in most of the stars, we find a period in the range of 20 to 200 days which is probably due to low-order radial pulsation. In many of the stars, we also find a period which is an order of magnitude longer. It may be due to rotation, or it may be due to a new kind of convectively-induced oscillatory thermal mode, recently proposed by Peter Wood. Supported by NASA, NSF, and NSERC Canada.

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