Radial velocity curves of HD 101799.

Sisteró, R. F.; Sistero, M. E. Castore de

doi:10.1086/111556

Cited by 4 publications

(9 citation statements)

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“…The orbital semi-major axis is calculated to be a = 2.59(±0.05)R⊙. It should be mentioned that the mass ratio of V752 Cen was determined to be q = 0.31 from spectroscopic observations (Sisteró & Castore de Sisteró 1974), which was similar to our value (1/3.35 = 0.30). V752 Cen is a triple-lined spectroscopic quadruple system, and the tertiary and fourth components may make up a far away binary system (Schumacher 2009).…”

Section: Discussionsupporting

confidence: 87%

“…The star eclipsed at primary minimum is hotter but less massive than the star eclipsed at secondary minimum. The orbital inclination is i( • ) = 82.07, and the totally Sisteró (1974): (M1 + M2)sin 3 i = 1.648 ± 0.089M⊙ , the absolute parameters of the two component stars are calculated and listed in Table 4. The orbital semi-major axis is calculated to be a = 2.59(±0.05)R⊙.…”

Section: Discussionmentioning

confidence: 99%

“…They claimed that V752 Cen was a completely eclipsing binary system and its components nearly filled their respective Roche lobes (a semi-detached system). The radial velocity curves of V752 Cen were also published by Sisteró & Castore de Sisteró (1974), which revealed that V752 Cen was a double-lined eclipsing binary with the spectral type of its two component stars to be F8 and F5. However, Leung (1976) claimed that V752 Cen was a contact binary with a fill-out factor of f = 6.3 % after he reanalyzed the light curves obtained by Sisteró & Castore de Sisteró (1971, 1973.…”

Section: Introductionmentioning

confidence: 95%

“…In 1970, Bond (1970) reported three newly discovered W UMa type contact binaries, one of which was V752 Cen (HD 101799, V = 9.1 m ). Later, Sisteró & Castore de Sisteró (1971Sisteró ( , 1973 observed V752 Cen photometrically and obtained U BV light curves. They claimed that V752 Cen was a completely eclipsing binary system and its components nearly filled their respective Roche lobes (a semi-detached system).…”

Section: Introductionmentioning

confidence: 99%

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

Xiao

Soonthornthum

et al. 2019

Monthly Notices of the Royal Astronomical Society

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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.

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Section: Discussionsupporting

confidence: 87%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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

Xiao

Soonthornthum

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…More than half (7/10) of the catalogued X-ray sources detected in our follow-up exhibiting variability are identified as AGNs. The other three of the remaining catalogued and identified sources are stars (one of which is XMMSL1 J114247.5-354904, the counterpart to V* V752 Cen / HD 101799: an eclipsing binary with an 8-hour period; Sisteró & Castore de Sisteró 1974). Thus, a point of consideration in future GW follow-up campaigns is that if a GW counterpart occurred in an X-ray-active galaxy, the automated source ranking system would classify it as a known source getting brighter.…”

Section: What We Foundmentioning

confidence: 99%

Swift-XRT Follow-up of Gravitational-wave Triggers in the Second Advanced LIGO/Virgo Observing Run

Klingler

Kennea

Evans

et al. 2019

ApJS

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The Neil Gehrels Swift Observatory carried out prompt searches for gravitational wave (GW) events detected by the LIGO/Virgo Collaboration (LVC) during the second observing run ("O2"). Swift performed extensive tiling of eight LVC triggers, two of which had very low false-alarm rates (GW 170814 and the epochal GW 170817), indicating a high confidence of being astrophysical in origin; the latter was the first GW event to have an electromagnetic counterpart detected. In this paper we describe the follow-up performed during O2 and the results of our searches. No GW electromagnetic counterparts were detected; this result is expected, as GW 170817 remained the only astrophysical event containing at least one neutron star after LVC's later retraction of some events. A number of X-ray sources were detected, with the majority of identified sources being active galactic nuclei. We discuss the detection rate of transient X-ray sources and their implications in the Corresponding author: N. J. Klingler njk5441@psu.edu arXiv:1909.11586v2 [astro-ph.HE] 11 Oct 2019 2 KLINGLER ET AL.O2 tiling searches. Finally, we describe the lessons learned during O2, and how these are being used to improve the Swift follow-up of GW events. In particular, we simulate a population of GRB afterglows to evaluate our source ranking system's ability to differentiate them from unrelated and uncatalogued X-ray sources. We find that ≈ 60 − 70% of afterglows whose jets are oriented towards Earth will be given high rank (i.e., "interesting" designation) by the completion of our second follow-up phase (assuming their location in the sky was observed), but that this fraction can be increased to nearly 100% by performing a third follow-up observation of sources exhibiting fading behavior.

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Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation

Bilir

Karataş

Demircan

et al. 2005

Monthly Notices of the Royal Astronomical Society

106

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We study the kinematics of 129 W UMa binaries and we discuss its implications on the contact binary evolution. The sample is found to be heterogeneous in the velocity space. That is, kinematically younger and older contact binaries exist in the sample. A kinematically young (0.5 Gyr) subsample (moving group) is formed by selecting the systems that satisfy the kinematical criteria of moving groups. After removing the possible moving group members and the systems that are known to be members of open clusters, the rest of the sample is called the field contact binary (FCB) group. The FCB group is further divided into four groups according to the orbital period ranges. Then, a correlation is found in the sense that shorter‐period less‐massive systems have larger velocity dispersions than the longer‐period more‐massive systems. Dispersions in the velocity space indicate a 5.47‐Gyr kinematical age for the FCB group. Compared with the field chromospherically active binaries (CABs), presumably detached binary progenitors of the contact systems, the FCB group appears to be 1.61 Gyr older. Assuming an equilibrium in the formation and destruction of CAB and W UMa systems in the Galaxy, this age difference is treated as an empirically deduced lifetime of the contact stage. Because the kinematical ages (3.21, 3.51, 7.14 and 8.89 Gyr) of the four subgroups of the FCB group are much longer than the 1.61‐Gyr lifetime of the contact stage, the pre‐contact stages of the FCB group must dominantly be producing the large dispersions. The kinematically young (0.5 Gyr) moving group covers the same total mass, period and spectral ranges as the FCB group. However, the very young age of this group does not leave enough room for pre‐contact stages, and thus it is most likely that these systems were formed in the beginning of the main sequence or during the pre‐main‐sequence contraction phase, either by a fission process or most probably by fast spiralling in of two components in a common envelope.

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Radial velocity curves of HD 101799.

Cited by 4 publications

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

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

Swift-XRT Follow-up of Gravitational-wave Triggers in the Second Advanced LIGO/Virgo Observing Run

Kinematics of W Ursae Majoris type binaries and evidence of the two types of formation

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