A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System

Zhang, Bin; Qian, S.; Zhi, Qi‐Jun; Liu, N.-P.; Dong, Ai‐Jun; Michel, R.; Zhu, L.-Y.; Li, K.; Zhang, J.; Wang, Q.-S.

doi:10.1088/1538-3873/aafeab

Cited by 9 publications

(8 citation statements)

References 50 publications

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“…Such short period low mass binaries are rare, with only a few being known around the 0.2 d period (cf. Zhang et al 2019 ;Fang et al 2019 ). Given we find no evidence for a variability of the radial velocity of these stars, we expect that these binaries are not related to the low mass star we obtained spectra for and are likely spatially nearby sources.…”

Section: Short Period Binariesmentioning

confidence: 99%

The puzzling story of flare inactive ultra fast rotating M dwarfs. II. Searching for radial velocity variations

Ramsay

Hakala

Doyle

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Observations made using TESS revealed a sample of low mass stars which show a periodic modulation on a period <0.2 d. Surprisingly many of these Ultra Fast Rotating (UFR) stars showed no evidence of flare activity which would be expected from such rapidly rotating stars. We present results from a spectroscopic survey of UFRs using the Nordic Optical Telescope to search for radial velocity variations which could reveal evidence for binarity. Our sample of 29 sources have a photometric period between 0.1-0.2d, cover spectral classes of M0-4V, and show no evidence for flares. We detect only one source with clear radial velocity shifts, with another two having Gaia RUWE values which suggests they are binaries. Further observations reveal the former star possibly contains a brown dwarf companion with a mass of M2>58 MJup and probability P(M2<90 MJup) = 50%. There is no evidence for the companion in our spectra, strengthening the case for a brown dwarf companion. We also examine the folded TESS light curves of all our targets, finding at least two are eclipsing binaries and one which has been contaminated by a spatially nearby δ Sct star. We estimate that around 1/4 of our targets may have been contaminated by short period variable stars. However, the majority of our targets are consistent with being single, low mass stars whose variability is due to starspots. We outline the possible reasons why they are not flare active despite being such rapid rotators.

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Section: Short Period Binariesmentioning

confidence: 99%

The puzzling story of flare inactive ultra fast rotating M dwarfs. II. Searching for radial velocity variations

Ramsay

Hakala

Doyle

et al. 2022

Monthly Notices of the Royal Astronomical Society

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show abstract

“…Such short period low mass binaries are rare, with only a few being known around the 0.2 d period (c.f. Zhang et al 2019;Fang et al 2019). Given we find no evidence for a variability of the radial velocity of these stars we expect that these binaries are not related to the low mass star we obtained spectra for and are likely spatially nearby sources.…”

Section: Short Period Binariesmentioning

confidence: 99%

The Puzzling Story of Flare Inactive Ultra Fast Rotating M dwarfs. II. Searching for radial velocity variations

Ramsay,

Hakala,

Doyle

et al. 2022

Preprint

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Observations made using TESS revealed a sample of low mass stars which show a periodic modulation on a period < 0.2 d. Surprisingly many of these Ultra Fast Rotating (UFR) stars showed no evidence of flare activity which would be expected from such rapidly rotating stars. We present results from a spectroscopic survey of UFRs using the Nordic Optical Telescope to search for radial velocity variations which could reveal evidence for binarity. Our sample of 29 sources have a photometric period between 0.1-0.2d, cover spectral classes of M0-4V, and show no evidence for flares. We detect only one source with clear radial velocity shifts, with another two having Gaia RUWE values which suggests they are binaries. Further observations reveal the former star possibly contains a brown dwarf companion with a mass of M 2 >58 M Jup and probability P(M 2 <90 M Jup ) = 50%. There is no evidence for the companion in our spectra, strengthening the case for a brown dwarf companion. We also examine the folded TESS light curves of all our targets, finding at least two are eclipsing binaries and one which has been contaminated by a spatially nearby 𝛿 Sct star. We estimate that around 1/4 of our targets may have been contaminated by short period variable stars. However, the majority of our targets are consistent with being single, low mass stars whose variability is due to starspots. We outline the possible reasons why they are not flare active despite being such rapid rotators.

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“…We used the basic sinusoidal equation to model the cyclic changes of the O-C values of the target as applied to many active binary stars (e.g. Tian et al 2009;Zhang et al 2019). Using the method of differential correction, the parameters of the sinusoidal changes were derived 6, together with the Applegate model's parameters.…”

Section: Orbital Period Variationsmentioning

confidence: 99%

Investigation of near-contact semi-detached binary WUMi through observations and evolutionary models

Soydugan

Soydugan²,

Aliçavuş

2020

Res. Astron. Astrophys.

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W UMi is a near contact, semi-detached, double-lined eclipsing binary star with an orbital period of 1.7 days. Simultaneous analysis of new BVR multi-color light curves and radial velocity data yields the main astrophysical parameters of the binary and its component stars. We determined mass and radius to be M 1 =3.22±0.08 M ⊙ , R 1 =3.63±0.04 R ⊙ for the primary star and M 2 =1.44±0.05 M ⊙ , R 2 =3.09±0.03 R ⊙ for the secondary star. Based on analysis of mid-eclipse times, variation in the orbital period is represented by a cyclic term and a downward parabola. Mass loss from the system is suggested for a secular decrease (-0.02 s yr −1 ) in the period. Both the mechanisms of a hypothetical tertiary star orbiting around W UMi and the surface magnetic activity of the less massive cooler companion were used to interpret periodic changes. Observational parameters were found to be consistent with binary stellar evolution models produced in the non-conservative approach of MESA at a higher metallicity than the Sun and an age of about 400 Myr for the system. Evidence that the system is rich in metal was obtained from spectral and kinematic analysis as well as evolution models. W UMi, a high mass ratio system compared to classical semi-detached binaries, is an important example since it is estimated from binary evolutionary models that the system may reach its contact phase in a short time interval.

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A Detached Eclipsing Binary with a Period Shorter than 0.2 Days in a Triple System

Cited by 9 publications

References 50 publications

The puzzling story of flare inactive ultra fast rotating M dwarfs. II. Searching for radial velocity variations

The puzzling story of flare inactive ultra fast rotating M dwarfs. II. Searching for radial velocity variations

The Puzzling Story of Flare Inactive Ultra Fast Rotating M dwarfs. II. Searching for radial velocity variations

Investigation of near-contact semi-detached binary WUMi through observations and evolutionary models

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