Orbital period changes and the higher-order multiplicity fraction amongst SuperWASP eclipsing binaries

Lohr, M. E.; Norton, A. J.; Payne, S. G.; West, R. G.; Wheatley, P. J.

doi:10.1051/0004-6361/201525747

“…The latter group would have equal numbers of positive and negative values of period derivative, and indeed we find nearly equal numbers (three positive and four negative) among those cases with large parabolic variations. Similar numbers of positive and negative valued quadratic changes in O-C were also found among eclipsing binaries in the SuperWASP survey (Lohr et al 2015), consistent with the idea that many of these are triples with incompletely covered, long orbits. We caution that some of the weaker parabolic trends may result from long term variations in starspot activity and not orbital motion (for example, the case of KIC 02708156 in Figure 1.2).…”

Section: Discussionsupporting

confidence: 76%

KEPLERECLIPSING BINARIES WITH STELLAR COMPANIONS

Gies

¹

,

Matson

²

,

Guo

³

et al. 2015

View full text Add to dashboard Cite

Many short-period binary stars have distant orbiting companions that have played a role in driving the binary components into close separation. Indirect detection of a tertiary star is possible by measuring apparent changes in eclipse times of eclipsing binaries as the binary orbits the common center of mass. Here we present an analysis of the eclipse timings of 41 eclipsing binaries observed throughout the NASA Kepler mission of long duration and precise photometry. This subset of binaries is characterized by relatively deep and frequent eclipses of both stellar components. We present preliminary orbital elements for seven probable triple stars among this sample, and we discuss apparent period changes in seven additional eclipsing binaries that may be related to motion about a tertiary in a long period orbit. The results will be used in ongoing investigations of the spectra and light curves of these binaries for further evidence of the presence of third stars.

show abstract

“…The latter group would have equal numbers of positive and negative values of period derivative, and indeed we find nearly equal numbers (three positive and four negative) among those cases with large parabolic variations. Similar numbers of positive and negative valued quadratic changes in O − C were also found among eclipsing binaries in the SuperWASP survey (Lohr et al 2015), consistent with the idea that many of these are triples with incompletely covered, long orbits. We caution that some of the weaker parabolic trends may result from long term variations in starspot activity and not orbital motion (for example, the case of KIC 02708156 in Fig.…”

Section: Discussionsupporting

confidence: 76%

Kepler Eclipsing Binaries with Stellar Companions

Gies

¹

,

Matson

²

,

Guo

³

et al. 2015

Preprint

View full text Add to dashboard Cite

Many short-period binary stars have distant orbiting companions that have played a role in driving the binary components into close separation. Indirect detection of a tertiary star is possible by measuring apparent changes in eclipse times of eclipsing binaries as the binary orbits the common center of mass. Here we present an analysis of the eclipse timings of 41 eclipsing binaries observed throughout the NASA Kepler mission of long duration and precise photometry. This subset of binaries is characterized by relatively deep and frequent eclipses of both stellar components. We present preliminary orbital elements for seven probable triple stars among this sample, and we discuss apparent period changes in seven additional eclipsing binaries that may be related to motion about a tertiary in a long period orbit. The results will be used in ongoing investigations of the spectra and light curves of these binaries for further evidence of the presence of third stars.

show abstract

“…The period of V752 Cen has been increasing continuously at a rate of dP/dt = +5.05×10 −7 day •year −1 (+0.044s•year −1 ) after that sudden period change happened. The period change is almost the same as that determined by Lohr et al (2015), which was +0.04379s • year −1 . It can be explained by mass transfer from the less massive component star to the more massive one, and the mass transfer rate is estimated to be dM 2 dt = 2.52 × 10 −7 M⊙/year.…”

Section: Modeling the Light Curvessupporting

confidence: 77%

V752 Cen - A triple-lined spectroscopic contact binary with sudden and continuous period changes

Xiao

¹

,

Soonthornthum

²

,

SB

³

et al. 2019

Monthly Notices of the Royal Astronomical Society

3

0

View full text Add to dashboard Cite

V752 Cen is a triple-lined spectroscopic contact binary. Its multi-color light curves were obtained in the years 1971 and 2018, independently. Photometric analyses reveal that the two sets of light curves produce almost consistent results. It contains a Wsubtype totally eclipsing binary, and its mass ratio and fill-out factor are q = 3.35(1) and f = 29(2) %. The absolute elements of its two component stars were determined to be M 1 = 0.39(2)M ⊙ , M 2 = 1.31(7)M ⊙ , R 1 = 0.77(1)R ⊙ , R 2 = 1.30(2)R ⊙ , L 1 = 0.75(3)L ⊙ and L 2 = 2.00(7)L ⊙ . The period of V752 Cen is 0.37023198 day. The 0.37-d period remained constant from its first measurement in 1971 until the year 2000. However, it changed suddenly around the year 2000 and has been increasing continuously at a rate of dP/dt = +5.05 × 10 −7 day · year −1 since then, which can be explained by mass transfer from the less massive component star to the more massive one with a rate of dM2 dt = 2.52 × 10 −7 M ⊙ /year. The period variation of V752 Cen over the 48 years in which the period has been monitored is really unusual, and is potentially related to effects from the possible presence of a nearby third star or of a pair of stars in a second binary.

show abstract

Orbital period changes and the higher-order multiplicity fraction amongst SuperWASP eclipsing binaries

Cited by 29 publications

References 29 publications

KEPLERECLIPSING BINARIES WITH STELLAR COMPANIONS

KEPLERECLIPSING BINARIES WITH STELLAR COMPANIONS

Kepler Eclipsing Binaries with Stellar Companions

V752 Cen - A triple-lined spectroscopic contact binary with sudden and continuous period changes

Contact Info

Product

Resources

About