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Title:
Ellipsoidal Variable V1197 Orionis: Absolute Light-Velocity Analysis for Known Distance
Authors:
Wilson, R. E.; Chochol, D.; Komžík, R.; Van Hamme, W.; Pribulla, T.; Volkov, I.
Affiliation:
AA(Astronomy Department, University of Florida, Gainesville, FL 32611, USA ), AB(Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia ), AC(Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia ), AD(Department of Physics, Florida International University, Miami, FL 33199, USA ), AE(Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, D-07740 Jena, Germany ; On leave from Slovak Academy of Sciences, Tatranská Lomnica, Slovakia.), AF(Sternberg State Astronomical Institute, Universitetskij Prospect 13, Moscow 119992, Russia )
Publication:
The Astrophysical Journal, Volume 702, Issue 1, pp. 403-413 (2009). (ApJ Homepage)
Publication Date:
09/2009
Origin:
IOP
ApJ Keywords:
binaries: close, methods: data analysis, stars: distances, stars: fundamental parameters, stars: individual: V1197 Orionis, stars: oscillations
DOI:
10.1088/0004-637X/702/1/403
Bibliographic Code:
2009ApJ...702..403W

Abstract

V1197 Orionis light curves from a long-term observing program for red giant binaries show ellipsoidal variation of small amplitude in the V and RC bands, although not clearly in U and B. Eclipses are not detected. All four bands show large irregular intrinsic variations, including fleeting quasi-periodicities identified by power spectra, that degrade analysis and may be caused by dynamical tides generated by orbital eccentricity. To deal with the absence of eclipses and consequent lack of astrophysical and geometrical information, direct use is made of the Hipparcos parallax distance while the V and RC light curves and (older) radial velocity curves are analyzed simultaneously in terms of absolute flux. The red giant's temperature is estimated from new spectra. This type of analysis, called Inverse Distance Estimation for brevity, is new and can also be applied to other ellipsoidal variables. Advantages gained by utilization of definite distance and temperature are discussed in regard to how radius, fractional lobe filling, and mass ratio information are expressed in the observations. The advantages were tested in solutions of noisy synthetic data. Also discussed and tested by simulations are ideas on the optimal number of light curves to be solved simultaneously under various conditions. The dim companion has not been observed or discussed in the literature but most solutions find its mass to be well below that of the red giant. Solutions show red giant masses that are too low for evolution to the red giant stage within the age of the Galaxy, although that result is probably an artifact of the intrinsic brightness fluctuations.
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