The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Huélamo, N.; Vaz, L. P. R.; Torres, C. A. O.; Bergeron, P.; Melo, C.; Quast, G.; Barrado, D.; Sterzik, M.; Chauvin, G.; Bouy, H.; Landin, N. R.

doi:10.1051/0004-6361/200811514

Cited by 12 publications

(13 citation statements)

References 48 publications

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“…SB2 EBs that contain at least one low-mass main-sequence star (M   M 0.7 ☉ ) are especially useful for testing the treatment of convection and degeneracy in evolutionary models (e.g., Feiden & Chaboyer 2013). To date, several dozen low-mass SB2 EBs are known (e.g., Torres & Ribas 2002;Ribas 2003;Bayless & Orosz 2006;López-Morales & Shaw 2007;Vaccaro et al 2007;Devor 2008;Fernandez et al 2009;Huélamo et al 2009;Irwin et al 2009;Morales et al 2009aMorales et al , 2009bRozyczka et al 2009;Irwin et al 2011;Kraus et al 2011;Birkby et al 2012;Lee et al 2013;Zhou et al 2015). Many have larger radii than predicted by evolutionary models for their mass, effective temperature, and age.…”

Section: Introductionmentioning

confidence: 99%

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Han

Muirhead

Swift³

et al. 2017

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Several low-mass eclipsing binary stars show larger than expected radii for their measured mass, metallicity, and age. One proposed mechanism for this radius inflation involves inhibited internal convection and starspots caused by strong magnetic fields. One particular eclipsing binary, T-Cyg1-12664, has proven confounding to this scenario. Çakırlı et al. measured a radius for the secondary component that is twice as large as model predictions for stars with the same mass and age, but a primary mass that is consistent with predictions. Iglesias-Marzoa et al. independently measured the radii and masses of the component stars and found that the radius of the secondary is not in fact inflated with respect to models, but that the primary is, which is consistent with the inhibited convection scenario. However, in their mass determinations, Iglesias-Marzoa et al. lacked independent radial velocity measurements for the secondary component due to the star's faintness at optical wavelengths. The secondary component is especially interesting, as its purported mass is near the transition from partially convective to a fully convective interior. In this article, we independently determined the masses and radii of the component stars of T-Cyg1-12664 using archival Kepler data and radial velocity measurements of both component stars obtained with IGRINS on the Discovery Channel Telescope and NIRSPEC and HIRES on the Keck Telescopes. We show that neither of the component stars is inflated with respect to models. Our results are broadly consistent with modern stellar evolutionary models for main-sequence M dwarf stars and do not require inhibited convection by magnetic fields to account for the stellar radii.

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Section: Introductionmentioning

confidence: 99%

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Han

Muirhead

Swift³

et al. 2017

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“…Since they are also transiting, we can measure their basic parameters, namely their mass and their radius. This has been possible for a few very low-mass objects (e.g., Huélamo et al 2009;Shkolnik et al 2008;Díaz et al 2014;Lillo-Box et al 2015) so these detections increase the sample. This is important in order to understand the properties of these sources since they allow a direct measurement of their density and surface gravity.…”

Section: Discussionmentioning

confidence: 99%

Search for light curve modulations amongKeplercandidates

Lillo-Box

Ribas

Barrado

et al. 2016

A&A

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Context. Light curve modulations in the sample of Kepler planet candidates allows the disentangling of the nature of the transiting object by photometrically measuring its mass. This is possible by detecting the effects of the gravitational pull of the companion (ellipsoidal modulations) and in some cases, the photometric imprints of the Doppler effect when observing in a broad band (Doppler beaming). Aims. We aim to photometrically unveil the nature of some transiting objects showing clear light curve modulations in the phasefolded Kepler light curve. Methods. We selected a subsample among the large crop of Kepler objects of interest (KOIs) based on their chances to show detectable light curve modulations, i.e., close (a < 12 R ) and large (in terms of radius, according to their transit signal) candidates. We modeled their phase-folded light curves with consistent equations for the three effects, namely, reflection, ellipsoidal and beaming (known as REB modulations). Results. We provide detailed general equations for the fit of the REB modulations for the case of eccentric orbits. These equations are accurate to the photometric precisions achievable by current and forthcoming instruments and space missions. By using this mathematical apparatus, we find three close-in very low-mass companions (two of them in the brown dwarf mass domain) orbiting main-sequence stars (KOI-554, KOI-1074, and KOI-3728), and reject the planetary nature of the transiting objects (thus classifying them as false positives). In contrast, the detection of the REB modulations and transit/eclipse signal allows the measurement of their mass and radius that can provide important constraints for modeling their interiors since just a few cases of low-mass eclipsing binaries are known. Additionally, these new systems can help to constrain the similarities in the formation process of the more massive and close-in planets (hot Jupiters), brown dwarfs, and very low-mass companions.

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“…For a use of WD to date a multiple system, and interesting exercise has been carried out recently by Huélamo et al (2009), as it will described in the next subsection (3.1.5). In addition, the WD mass function has been used to estimate de ages of the galactic population (Kepler et al 2007).…”

Section: White Dwarfsmentioning

confidence: 99%

“…As can be seen, even in this optimal situation the EB does not provide a strong constraint for the age. Another comparison can be found in Huélamo et al (2009), in this case with a triplet which includes a EB and a visual WD. Despite the fact the spectroscopic properties of the WD can be established with a certain degree of precision, the overall properties of the system remain elusive.…”

Section: Sizes: Eclipsing Binariesmentioning

confidence: 99%

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Clusters: Age Scales for Stellar Physics

Barrado

2016

EAS Publications Series

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Abstract. Ages are key to truly understand a large plethora of astrophysical phenomena. On the other hand, stellar clusters are open windows to understand stellar evolution, specifically, the change with time and mass of different stellar properties. As such, they are our laboratories where different theories can be tested, but without accurate ages, our knowledge would impaired. We revisit here a large number of age-dating techniques and discuss their advantages and draw-backs. In addition, a step-by step process is suggested in order to built a coherent age scale ladder, minimizing the error budget and the sources of uncertainty.

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The triple system HIP 96515: a low-mass eclipsing binary with a DB white dwarf companion

Cited by 12 publications

References 48 publications

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Magnetic Inflation and Stellar Mass. I. Revised Parameters for the Component Stars of the Kepler Low-mass Eclipsing Binary T-Cyg1-12664

Search for light curve modulations amongKeplercandidates

Clusters: Age Scales for Stellar Physics

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