HD 50975: a yellow supergiant in a spectroscopic binary system

Sperauskas, J.; Začs, L.; Raudeliunas, S.; Мусаев, Ф. А.; Puzin, V. B.

doi:10.1051/0004-6361/201322888

Cited by 3 publications

(3 citation statements)

References 28 publications

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“…Like for the RSGs, the binary fraction of the rarer yellow supergiants (F-and G-types) is also highly uncertain. For a few cases, orbital periods of around a few hundred days have been determined (Prieto et al 2008;Sperauskas et al 2014). Besides, when (some of) these stars go through the classic instability strip, they will Coefficient of variation as a function of characteristic timescales t ch for the different types of supergiants as indicated in the respective legends.…”

Section: Discussionmentioning

confidence: 99%

Variability of Massive Stars in M31 from the Palomar Transient Factory

Soraisam

Bildsten

Drout

et al. 2020

ApJ

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Using data from the (intermediate) Palomar Transient Factory (iPTF), we characterize the time variability of ≈ 500 massive stars in M31. Our sample is those stars which are spectrally typed by Massey and collaborators, including Luminous Blue Variables, Wolf-Rayets, and warm and cool supergiants. We use the high-cadence, long-baseline (≈ 5 years) data from the iPTF survey, coupled with data-processing tools that model complex features in the light curves. We find widespread photometric (R-band) variability in the upper Hertzsprung Russell diagram (or CMD) with an increasing prevalence of variability with later spectral types. Red stars (V − I > 1.5) exhibit larger amplitude fluctuations than their bluer counterparts. We extract a characteristic variability timescale, t ch , via wavelet transformations that are sensitive to both continuous and localized fluctuations. Cool supergiants are characterized by longer timescales (> 100 days) than the hotter stars. The latter have typical timescales of tens of days but cover a wider range, from our resolution limit of a few days to longer than 100 days timescales. Using a 60-night block of data straddling two nights with a cadence of around 2 minutes, we extracted t ch in the range 0.1-10 days with amplitudes of a few percent for 13 stars. Though there is broad agreement between the observed variability characteristics in the different parts of the upper CMD with theoretical predictions, detailed comparison requires models with a more comprehensive treatment of the various physical processes operating in these stars such as pulsation, subsurface convection, and the effect of binary companions.

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Section: Discussionmentioning

confidence: 99%

Variability of Massive Stars in M31 from the Palomar Transient Factory

Soraisam

Bildsten

Drout

et al. 2020

ApJ

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“…The period distribution of mass-transferring systems in Box III is roughly flat in log(P) in the range between ∼50 and 1000 days. The long periods of these systems may make it challenging to assess their binary nature in typical spectroscopic surveys (unless a long-term monitoring campaign is possible, e.g., Sperauskas et al 2014). An alternative approach could be to systematically search for eclipsing binaries with yellow supergiants in photometric variability surveys.…”

Section: Binary-interaction Products In the Hr Diagrammentioning

confidence: 99%

Partial-envelope stripping and nuclear-timescale mass transfer from evolved supergiants at low metallicity

Klencki

Istrate

Nelemans

et al. 2022

A&A

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Stable mass transfer from a massive post-main sequence (post-MS) donor is thought to be a short-lived event of thermal-timescale mass transfer (∼10−3 M⊙ yr−1) which within ≲104 yr strips the donor star of nearly its entire H-rich envelope, producing a hot, compact helium star. This long-standing picture is based on stellar models with rapidly expanding Hertzprung gap (HG) donor stars. Motivated by a finding that in low-metallicity binaries, post-MS mass transfer may instead be initiated by donors already at the core-helium burning (CHeB) stage, we used the MESA stellar-evolution code to compute grids of detailed massive binary models at three metallicities: those of the Sun, the Large Magellanic Cloud (LMC, ZFe; LMC/ZFe; ⊙ ≈ 0.36), and the Small Magellanic Cloud (SMC, ZFe; SMC/ZFe; ⊙ ≈ 0.2). Our grids span a wide range in orbital periods (∼3 to 5000 days) and initial primary masses (10 M⊙ to 36 − 53 M⊙, depending on metallicity). We find that metallicity strongly influences the course and outcome of mass-transfer evolution. We identify two novel types of post-MS mass transfer: (a) mass exchange on the long nuclear timescale (ΔTMT ≳ 105 yr, Ṁ ∼ 10−5 M⊙ yr−1) that continues until the end of the CHeB phase, and (b) rapid mass transfer leading to detached binaries with mass losers that are only partially stripped of their envelopes. At LMC and SMC compositions, the majority of binary models with donor masses ≥17 M⊙ follow one of these two types of evolution. In neither (a) nor (b) does the donor become a fully stripped helium star by the end of CHeB. Boundaries between the different types of post-MS mass transfer evolution are associated with the degree of rapid post-MS expansion of massive stars and, for a given metallicity, are sensitive to the assumptions about internal mixing. At low metallicity, due to partial envelope stripping, we predict fewer hot fully stripped stars formed through binary interactions as well as higher compactness of the presupernova core structures of mass losers. Nuclear-timescale post-MS mass transfer suggests a strong preference for metal-poor host galaxies of ultra-luminous X-ray sources with black-hole (BH) accretors and massive donors, some of which might be the immediate progenitors of binary BH mergers. It also implies a population of interacting binaries with blue and yellow supergiant donors. Partially stripped stars could potentially explain the puzzling nitrogen-enriched slowly rotating (super)giants in the LMC.

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“…The long periods of these systems may make it challenging to assess their binary nature in typical spectroscopic surveys (unless a long-term monitoring campaign is possible, e.g. Sperauskas et al 2014). An alternative approach could be to systematically search for eclipsing binaries with yellow supergiants in photometric variability surveys.…”

Section: Binary-interaction Products In the Hr Diagrammentioning

confidence: 99%

Partial-envelope stripping and nuclear-timescale mass transfer from evolved supergiants at low metallicity

Klencki,

Istrate,

Nelemans

et al. 2021

Preprint

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Stable mass transfer from a massive post-main sequence (post-MS) donor is thought to be a short-lived event of thermal-timescale mass transfer (∼ 10 −3 M yr −1 ) which within 10 4 yr strips the donor star of nearly its entire H-rich envelope, producing a hot, compact helium star. This long-standing picture is based on stellar models with rapidly-expanding Hertzprung gap (HG) donor stars. Motivated by a finding that in low-metallicity binaries, post-MS mass transfer may instead be initiated by donors already at the corehelium burning (CHeB) stage, we use the MESA stellar-evolution code to compute grids of detailed massive binary models at three metallicities: those of the Sun, the Large Magellanic Cloud (LMC, Z Fe;LMC /Z Fe; ≈ 0.36), and the Small Magellanic Cloud (SMC, Z Fe;SMC /Z Fe; ≈ 0.2). Our grids span a wide range in orbital periods (∼ 3 to 5000 days) and initial primary masses (10 M to 36-53 M , depending on metallicity). We find that metallicity strongly influences the course and outcome of mass-transfer evolution. We identify two novel types of post-MS mass transfer: (a) mass exchange on the long nuclear timescale (∆T MT 10 5 yr, Ṁ ∼ 10 −5 M yr −1 ) that continues until the end of the CHeB phase, and (b) rapid mass transfer leading to detached binaries with mass-losers that are only partially stripped of their envelopes. At LMC and SMC compositions, the majority of binary models with donor masses ≥ 17 M follow one of these two types of evolution. In neither (a) or (b) does the donor become a fully stripped helium star by the end of CHeB. Boundaries between the different types of post-MS mass transfer evolution are associated with the degree of rapid post-MS expansion of massive stars and, for a given metallicity, are sensitive to the assumptions about internal mixing. At low metallicity, due to partial envelope stripping, we predict fewer hot fully stripped stars formed through binary interactions as well as higher compactness of the pre-supernova core structures of mass losers. Nuclear-timescale post-MS mass transfer suggests a strong preference for metal-poor host galaxies of ultra-luminous X-ray sources with black-hole (BH) accretors and massive donors, some of which might be the immediate progenitors of binary BH mergers. It also implies a population of interacting binaries with blue and yellow supergiant donors. Partially-stripped stars could potentially explain the puzzling nitrogen-enriched slowly-rotating (super)giants in the LMC.

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HD 50975: a yellow supergiant in a spectroscopic binary system

Cited by 3 publications

References 28 publications

Variability of Massive Stars in M31 from the Palomar Transient Factory

Variability of Massive Stars in M31 from the Palomar Transient Factory

Partial-envelope stripping and nuclear-timescale mass transfer from evolved supergiants at low metallicity

Partial-envelope stripping and nuclear-timescale mass transfer from evolved supergiants at low metallicity

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