Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61+0.45 M⊙ binary in a multiple system

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dc.contributor.authorHelminiak, K. G.
dc.contributor.authorKonacki, M.
dc.contributor.authorRozyczka, M.
dc.contributor.authorKaluzny, J.
dc.contributor.authorRatajczak, M.
dc.contributor.authorBorkowski, J.
dc.contributor.authorSybilski, P.
dc.contributor.authorMuterspaugh, M. W.
dc.contributor.authorReichart, D. E.
dc.contributor.authorIvarsen, K. M.
dc.contributor.authorHaislip, J. B.
dc.contributor.authorCrain, J. A.
dc.contributor.authorFoster, A. C.
dc.contributor.authorNysewander, M. C.
dc.contributor.authorLaCluyze, A. P.
dc.date.accessioned2025-01-20T23:57:15Z
dc.date.available2025-01-20T23:57:15Z
dc.date.issued2012
dc.description.abstractWe present the orbital and physical parameters of a newly discovered low-mass detached eclipsing binary from the All-Sky Automated Survey (ASAS) data base: ASAS J0113283821.1 A, which is a member of a visual binary system with the secondary component separated by about 1.4 arcsec. The radial velocities have been calculated from the high-resolution spectra obtained with the 1.9-m Radcliffe telescope/Grating Instrument for Radiation Analysis with a Fibre-Fed Echelle (GIRAFFE) spectrograph, the 3.9-m Anglo-Australian Telescope (AAT)/University College London Echelle Spectrograph (UCLES) and the 3.0-m Shane telescope/Hamilton Spectrograph (HamSpec) on the basis of the todcor technique and the positions of the Ha emission lines. For the analysis, we have used V- and I-band photometry obtained with the 1.0-m Elizabeth telescope and the 0.41-m Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT), supplemented with the publicly available ASAS light curve of the system. We have found that ASAS J0113283821.1 A is composed of two late-type dwarfs, which have masses of M1 = 0.612 +/- 0.030 M? and M2 = 0.445 +/- 0.019 M? and radii of R1 = 0.596 +/- 0.020 R? and R2 = 0.445 +/- 0.024 R?. Both show a substantial level of activity, which manifests in strong Ha and H beta emission and the presence of cool spots. The influence of the third light on the eclipsing pair properties has also been evaluated and the photometric properties of component B have been derived. A comparison with several popular stellar evolution models shows that the system is on its main-sequence evolution stage and that it is probably more metal-rich than the Sun. We have also found several clues to suggest that component B itself is a binary composed of two nearly identical similar to 0.5-M? stars.
dc.fuente.origenWOS
dc.identifier.doi10.1111/j.1365-2966.2012.21510.x
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1111/j.1365-2966.2012.21510.x
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/95200
dc.identifier.wosidWOS:000307888300030
dc.issue.numero2
dc.language.isoen
dc.pagina.final1256
dc.pagina.inicio1245
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectbinaries: eclipsing
dc.subjectbinaries: spectroscopic
dc.subjectbinaries: visual
dc.subjectstars: fundamental parameters
dc.subjectstars: individual: ASAS J010538-3821
dc.subject1
dc.subjectstars: low-mass
dc.titleOrbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61+0.45 M⊙ binary in a multiple system
dc.typeartículo
dc.volumen425
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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