Absolute parameters of young stars: GG Lup and μ1 Sco

Budding, E.; Butland, R.; Blackford, Mark G.

doi:10.1093/mnras/stv234

Cited by 18 publications

(11 citation statements)

References 28 publications

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“…Based on the g band data we determine a polarimetric inclination of 63.8 • ± 2.7, where the uncertainty is based on the same bootstrap analysis used in section 4.2. This agrees, within the errors, with the inclination of 65.4 • ± 1.0 (van Antwerpen & Moon 2010) and 64.4 • ± 0.3 (Budding et al 2015) from light curve analysis. The precision of our measurement could probably be improved with additional observations.…”

Section: Inclinationsupporting

confidence: 89%

“…µ 1 Sco is a semi-detached binary where the secondary is close to or just filling its Roche lobe (van Antwerpen & Moon 2010;Budding et al 2015). According to Budding et al (2015) the secondary's over-sized character implies on-going late-state interactive stellar evolution, believed to be of the 'Case A' type (i.e. it's still on the main sequence), though the primary is little effected.…”

Section: µ 1 Scomentioning

confidence: 99%

“…Drawing on decades of radial velocity and photometry, and their own observations, van Antwerpen & Moon (2010) determine the orbit to be circular with an inclination of 65.4 ± 1.0 • and a semi-major axis of 12.90 ± 0.04 R , and a period of 1.4462700(5) days (identical to Maury 1920 who was the first to study it extensively), with a primary photometric minimum at ephemeris HJD 2449534.17700(9). The mass of the B1.5 V primary is found to be 8.49 ± 0.05 M and the B8-B3 secondary 5.33 ± 0.05 M , the radius of the primary is 4.07 ± 0.05 R and the secondary 4.38 ± 0.05 R (van Antwerpen & Moon 2010) -which makes it considerably oversized for its mass (Budding et al 2015). A full list of parameters pertinent to the current work is given later in section 3.…”

Section: Phase-locked Polarization In Early-type Binariesmentioning

confidence: 99%

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Phase-locked polarization by photospheric reflection in the semidetached eclipsing binary μ1 Sco

Cotton

Bailey

Kedziora-Chudczer

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report the detection of phase-locked polarization in the bright (mV = 2.98 − 3.24) semidetached eclipsing binary μ1 Sco (HD 151890). The phenomenon was observed in multiple photometric bands using two different HIPPI-class (HIgh Precision Polarimetric Instrument) polarimeters with telescopes ranging in size from 35-cm to 3.9-m. The peak-to-trough amplitude of the polarization is wavelength dependent and large, ∼700 parts-per-million in green light, and is easily seen with even the smallest telescope. We fit the polarization phase curve with a SYNSPEC/VLIDORT polarized radiative transfer model and a Wilson-Devinney geometric formalism, which we describe in detail. Light from each star reflected by the photosphere of the other, together with a much smaller contribution from tidal distortion and eclipse effects, wholly accounts for the polarization amplitude. In the past polarization in semidetached binaries has been attributed mostly to scattering from extra-stellar gas. Our new interpretation facilitates determining masses of such stars in non-eclipsing systems.

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Section: Inclinationsupporting

confidence: 89%

Section: µ 1 Scomentioning

confidence: 99%

Section: Phase-locked Polarization In Early-type Binariesmentioning

confidence: 99%

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Phase-locked polarization by photospheric reflection in the semidetached eclipsing binary μ1 Sco

Cotton

Bailey

Kedziora-Chudczer

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…A concrete example is the HIP 82514 system, which is an eclipsing binary. As a consequence, the radii and temperatures of the individual central stellar components can be accurately determined, leading to an unusually reliable photometric distance of ∼135 pc (Budding et al 2015). Meanwhile, the distance based on the HIPPARCOS parallax is 154 pc, and the Gaia DR2 distance is 268 pc.…”

Section: Membership Of Sco-cenmentioning

confidence: 99%

“…To test the accuracy of these estimations for the BEAST sample, we cross-checked them against the three systems of the sample that are both known eclipsing binaries and doublelined spectroscopic binaries, such that individual masses can be determined in an entirely model-free manner: HIP 74950 (Budding et al 2015), HIP 78168 (David et al 2019), and HIP 82514 (Budding et al 2015). The primary masses as determined dynamically are 4.16, 5.58, and 8.3 M sun respectively, while the corresponding SpT-inferred primary masses are 3.3, 5.9, and 9.0 M sun .…”

Section: Stellar Massesmentioning

confidence: 99%

BEAST begins: sample characteristics and survey performance of the B-star Exoplanet Abundance Study

Janson

Delorme

Gratton

et al. 2021

A&A

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While the occurrence rate of wide giant planets appears to increase with stellar mass at least up through the A-type regime, B-type stars have not been systematically studied in large-scale surveys so far. It therefore remains unclear up to what stellar mass this occurrence trend continues. The B-star Exoplanet Abundance Study (BEAST) is a direct imaging survey with the extreme adaptive optics instrument SPHERE, targeting 85 B-type stars in the young Scorpius-Centaurus (Sco-Cen) region with the aim to detect giant planets at wide separations and constrain their occurrence rate and physical properties. The statistical outcome of the survey will help determine if and where an upper stellar mass limit for planet formation occurs. In this work, we describe the selection and characterization of the BEAST target sample. Particular emphasis is placed on the age of each system, which is a central parameter in interpreting direct imaging observations. We implement a novel scheme for age dating based on kinematic sub-structures within Sco-Cen, which complements and expands upon previous age determinations in the literature. We also present initial results from the first epoch observations, including the detections of ten stellar companions, of which six were previously unknown. All planetary candidates in the survey will need follow up in second epoch observations, which are part of the allocated observational programme and will be executed in the near future.

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Analysis of apsidal motion in eclipsing binaries using TESS data

Claret

Giménez

Baroch

et al. 2021

A&A

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Context. The measurement of apsidal motion rates in eccentric eclipsing binaries is a unique way to gain insight into the internal structure of stars through the internal density concentration parameter, k2. High-quality physical parameters of the stellar components, together with precise measurements of the advance of the periastron, are needed for the comparison with values derived from models. Aims. As a product of the Transiting Exoplanet Survey Satellite (TESS) mission, high-precision light curves of a large number of eclipsing binaries are now available. Using a selection of well-studied, double-lined eccentric eclipsing binary systems, we aim to determine their apsidal motion rates and place constraints on the internal density concentration and compare with the predictions from state-of-the-art theoretical models. Methods. We computed times of minimum light using the TESS light curves of 34 eclipsing binaries with precise absolute parameters. We used the changing difference over time between primary and secondary eclipse timings to determine the apsidal motion rate. To extend the time baseline, we combined the high-precision TESS timings with reliable archival data. On the other hand, for each component of our sample of double-lined eclipsing binaries, we computed grids of evolutionary stellar models for the observed stellar mass exploring ranges of values of the overshooting parameter fov, the mixing-length parameter, and the metallicity. To find the best solution for the two components we adopted a χ2 statistic to infer the optimal values of the overshooting parameter and the mixing-length parameter. The theoretical internal structure constants to be compared with the observed values were calculated by integrating the differential equations of Radau for each stellar model. Results. We have determined the apsidal motion rate of 27 double-lined eclipsing binaries with precise physical parameters. The obtained values, corrected for their relativistic contribution, yield precise empirical parameters of the internal stellar density concentration. The comparison of these results with the predictions based on new theoretical models shows very good agreement. Small deviations are identified but remain within the observational uncertainties and the path for a refined comparison is indicated.

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Absolute parameters of young stars: GG Lup and μ1 Sco

Cited by 18 publications

References 28 publications

Phase-locked polarization by photospheric reflection in the semidetached eclipsing binary μ1 Sco

Phase-locked polarization by photospheric reflection in the semidetached eclipsing binary μ1 Sco

BEAST begins: sample characteristics and survey performance of the B-star Exoplanet Abundance Study

Analysis of apsidal motion in eclipsing binaries using TESS data

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