Eclipsing binaries observed with the WIRE satellite. I, Discovery and photometric analysis of the new bright A0 IV eclipsing binary ψ Centauri
Bruntt, H., Southworth, J. (John), Torres, G., Penny, Alan (Alan J.), Clausen, J. V. and Buzasi, D. L.. (2006) Eclipsing binaries observed with the WIRE satellite. I, Discovery and photometric analysis of the new bright A0 IV eclipsing binary ψ Centauri. Astronomy & Astrophysics, Vol.456 (No.2). pp. 651-658. ISSN 0004-6361
WRAP_Southworth_68_Eclipsing_binaries.pdf - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Official URL: http://dx.doi.org/10.1051/0004-6361:20065628
Context. Determinations of stellar mass and radius with realistic uncertainties at the level of 1% provide important constraints on
models of stellar structure and evolution.
Aims. We present a high-precision light curve of the A0 IV star ψ Centauri, from the star tracker on board the wire satellite and the Solar Mass Ejection Imager camera on the Coriolis spacecraft. The data show that ψ Cen is an eccentric eclipsing binary system with a relatively long orbital period.
Methods. The wire light curve extends over 28.7 nights and contains 41 334 observations with 2 mmag point-to-point scatter. The eclipse depths are 0.28 and 0.16 mag, and show that the two eclipsing components of ψ Cen have very different radii. As a consequence,
the secondary eclipse is total. We find the eccentricity to be e = 0.55 with an orbital period of 38.8 days from combining the wire light curve with data taken over two years from the Solar Mass Ejection Imager camera.
Results. We have fitted the light curve with ebop and have assessed the uncertainties of the resulting parameters using Monte Carlo simulations. The fractional radii of the stars and the inclination of the orbit have random errors of only 0.1% and 0.01◦, respectively,but the systematic uncertainty in these quantities may be somewhat larger. We have used photometric calibrations to estimate the
effective temperatures of the components of ψ Cen to be 10450 ± 300 and 8800 ± 300K indicating masses of about 3.1 and 2.0 M. There is evidence in the wire light curve for g-mode pulsations in the primary star.
|Item Type:||Journal Article|
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Faculty of Science > Physics|
|Library of Congress Subject Headings (LCSH):||Eclipsing binaries, Stars -- Masses, Stars -- Evolution, Stars -- Temperature|
|Journal or Publication Title:||Astronomy & Astrophysics|
|Official Date:||September 2006|
|Page Range:||pp. 651-658|
|Access rights to Published version:||Open Access|
|Funder:||Air Force Research Laboratory (Wright-Patterson Air Force Base, Ohio) (AFRL), United States. National Aeronautics and Space Administration (NASA), University of California, San Diego, University of Birmingham, Forskningsrådet for Natur og Univers [Danish Science Research Council] (FNU), Danmarks Grundforskningsfond [Danish National Research Foundation], Instrumentcenter for Dansk Astrofysik [Instrument Centre for Danish Astrophsics] (IDA), National Science Foundation (U.S.) (NSF), United States. National Aeronautics and Space Administration (NASA)|
|Grant number:||NNG05GA41G (NASA), AST-0406183 (NSF), BLF57-04 (NASA)|
Aerts, C., & Kolenberg, K. 2005, A&A, 431, 615
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