MML 53: a new low-mass, pre-main sequence eclipsing binary in the Upper Centaurus-Lupus region discovered by SuperWASP

Hebb, Leslie; Stempels, H. C.; Aigrain, S.; Cameron, A. Collier; Hodgkin, S. T.; Irwin, Jonathan; Maxted, P. F. L.; Pollacco, D.; Street, R. A.; Wilson, David M.; Stassun, Keivan G.

doi:10.1051/0004-6361/201014059

Cited by 20 publications

(48 citation statements)

References 42 publications

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“…In some spectra we also observed a faint, stationary third peak between the primary and secondary peaks, consistent with the presence of a third component in the system first noted by Torres et al (2006) and confirmed by Hebb et al (2010). As this peak could not be unambiguously identified in all of our observations, we did not attempt to derive radial velocities for this component.…”

Section: Radial Velocitiessupporting

confidence: 79%

“…A very low S /N in the observation of Julian Date 2 454 971 prevented a clear cross-correlation function for that night; consequently, it was not used in the spectroscopic analysis, leaving 12 nights with usable data. Our cross-correlation functions for MML 53 typically show two distinct peaks, corresponding to the two eclipsing components, whose velocities vary in time with the orbital period determined from the discovery light curve of Hebb et al (2010).…”

Section: Radial Velocitiesmentioning

confidence: 95%

“…The reduced χ 2 about the mean value is χ 2 ν = 2.53, indicating an additional systematic error term of ≈0.08 km s −1 . (Hebb et al 2010). Phase 0.0 corresponds to T 0 , the time of minimum light of the primary eclipse.…”

Section: Radial Velocitiesmentioning

confidence: 99%

“…The ephemeris was determined by Hebb et al (2010) from over 10 000 photometric data points obtained by SuperWASP between 2006-2008, and thus the period measured from the light curve is much more precise than could be determined from the radial velocity data alone which span only three weeks. In addition, we find no significant difference in the derived epoch or the other orbital parameters if we allow T 0 to be a fitted parameter (see text below), so for our final results, we fix T 0 to the value derived from the light curve.…”

Section: Orbit Solution and Physical Propertiesmentioning

confidence: 99%

“…Here, we present a radial velocity curve and individual mass measurements for the newly discovered low-mass PMS eclipsing binary, MML 53 (Hebb et al 2010). In the first paper in this series, we showed for the first time that MML 53, which was previously identified as a late-type, lithium rich member of the 15 Myr old UCL star forming region (Mamajek et al 2002), is in fact a detached EB.…”

Section: Introductionmentioning

confidence: 99%

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Precise orbit solution of MML 53, a low-mass, pre-main sequence eclipsing binary in Upper Centaurus Lupus

Hebb

Cegla

Stassun

et al. 2011

A&A

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Aims. We present a double-lined orbit solution for MML 53, the recently discovered low-mass pre-main sequence eclipsing binary. Methods. Using high-resolution spectra from the SMARTS 1.5 m echelle spectrograph, we measure precise radial velocities and derive the orbital parameters of the system. Results. The 2.1 d orbit of the eclipsing pair is circular, and we find the minimum masses of the eclipsing components to be M 1 sin 3 i = 0.97 M and M 2 sin 3 i = 0.84 M , with formal uncertainties of 2.0% and an additional systematic uncertainty of ≈2.5% most likely caused by large star spots on the primary star. MML 53 has been previously identified as a member of the Upper Centaurus Lupus (UCL) star forming region (age ∼15 Myr). The systemic radial velocity from our orbit solution, v γ = +1.4 ± 0.3 ± 0.8 km s −1 (statistical and systematic), is also consistent with kinematic membership in this association. In addition, we detect a change in v γ between 2006 and 2009 providing further evidence for the presence of a the third body in a wide (several year) orbit.

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Section: Radial Velocitiessupporting

confidence: 79%

Section: Radial Velocitiesmentioning

confidence: 95%

Section: Radial Velocitiesmentioning

confidence: 99%

Section: Orbit Solution and Physical Propertiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Precise orbit solution of MML 53, a low-mass, pre-main sequence eclipsing binary in Upper Centaurus Lupus

Hebb

Cegla

Stassun

et al. 2011

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Empirical tests of pre-main-sequence stellar evolution models with eclipsing binaries

Stassun

Feiden

Torres

2014

New Astronomy Reviews

142

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We examine the performance of standard pre-main-sequence (PMS) stellar evolution models against the accurately measured properties of a benchmark sample of 26 PMS stars in 13 eclipsing binary (EB) systems having masses 0.04-4.0 M ⊙ and nominal ages ≈1-20 Myr. We provide a definitive compilation of all fundamental properties for the EBs, with a careful and consistent reassessment of observational uncertainties. We also provide a definitive compilation of the various PMS model sets, including physical ingredients and limits of applicability. No set of model isochrones is able to successfully reproduce all of the measured properties of all of the EBs. In the H-R diagram, the masses inferred for the individual stars by the models are accurate to better than 10% at 1 M ⊙ , but below 1 M ⊙ they are discrepant by 50-100%. Adjusting the observed radii and temperatures using empirical relations for the effects of magnetic activity helps to resolve the discrepancies in a few cases, but fails as a general solution. We find evidence that the failure of the models to match the data is linked to the triples in the EB sample; at least half of the EBs possess tertiary companions. Excluding the triples, the models reproduce the stellar masses to better than ∼10% in the H-R diagram, down to 0.5 M ⊙ , below which the current sample is fully contaminated by tertiaries. We consider several mechanisms by which a tertiary might cause changes in the EB properties and thus corrupt the agreement with stellar model predictions. We show that the energies of the tertiary orbits are comparable to that needed to potentially explain the scatter in the EB properties through injection of heat, perhaps involving tidal interaction. It seems from the evidence at hand that this mechanism, however it operates in detail, has more influence on the surface properties of the stars than on their internal structure, as the lithium abundances are broadly in good agreement with model predictions. The EBs that are members of young clusters appear individually coeval to within 20%, but collectively show an apparent age spread of ∼50%, suggesting true age spreads in young clusters. However, this apparent spread in the EB ages may also be the result of scatter in the EB properties induced by tertiaries.

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CoRoT 223992193: A new, low-mass, pre-main sequence eclipsing binary with evidence of a circumbinary disk

Gillen

Aigrain

McQuillan

et al. 2014

A&A

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We present the discovery of CoRoT 223992193, a double-lined, detached eclipsing binary, comprising two pre-main sequence M dwarfs, discovered by the CoRoT space mission during a 23-day observation of the 3 Myr old NGC 2264 star-forming region. Using multi-epoch optical and near-IR follow-up spectroscopy with FLAMES on the Very Large Telescope and ISIS on the William Herschel Telescope we obtain a full orbital solution and derive the fundamental parameters of both stars by modelling the light curve and radial velocity data. The orbit is circular and has a period of 3.8745745 ± 0.0000014 days. The masses and radii of the two stars are 0.67 ± 0.01 and 0.495 ± 0.007 M and 1.30 ± 0.04 and 1.11 +0.04 −0.05 R , respectively. This system is a useful test of evolutionary models of young low-mass stars, as it lies in a region of parameter space where observational constraints are scarce; comparison with these models indicates an apparent age of ∼3.5-6 Myr. The systemic velocity is within 1σ of the cluster value which, along with the presence of lithium absorption, strongly indicates cluster membership. The CoRoT light curve also contains large-amplitude, rapidly evolving out-of-eclipse variations, which are difficult to explain using starspots alone. The system's spectral energy distribution reveals a mid-infrared excess, which we model as thermal emission from a small amount of dust located in the inner cavity of a circumbinary disk. In turn, this opens up the possibility that some of the out-of-eclipse variability could be due to occultations of the central stars by material located at the inner edge or in the central cavity of the circumbinary disk.

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MML 53: a new low-mass, pre-main sequence eclipsing binary in the Upper Centaurus-Lupus region discovered by SuperWASP

Cited by 20 publications

References 42 publications

Precise orbit solution of MML 53, a low-mass, pre-main sequence eclipsing binary in Upper Centaurus Lupus

Precise orbit solution of MML 53, a low-mass, pre-main sequence eclipsing binary in Upper Centaurus Lupus

Empirical tests of pre-main-sequence stellar evolution models with eclipsing binaries

CoRoT 223992193: A new, low-mass, pre-main sequence eclipsing binary with evidence of a circumbinary disk

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