Characterization of the variability in the O+B eclipsing binary HD 165246

Johnston, C.; Aimar, N.; Abdul-Masih, M.; Bowman, D. M.; White, Timothy R.; Hawcroft, C.; Sana, H.; Sekaran, S.; Dsilva, K.; Tkachenko, A.; Aerts, C.

doi:10.1093/mnras/stab488

Cited by 16 publications

(14 citation statements)

References 116 publications

(173 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Regarding HD 308813, we confirm its single-lined spectroscopic binary status (see also Mahy et al 2022). In the same vein, HD 165246, which we identified as SB1, was also found by Johnston et al (2021) as an SB1 eclipsing binary system 19 with a period of 4.5927 d. After revisiting the literature, we can highlight that -to our best knowledge -we have identified one clear SB1 system (HD 152200) and another potential SB1 system (HD 46485) previously studied in Burssens et al (2020).…”

Section: Conclusion and Future Prospectssupporting

confidence: 52%

“…Most information about orbital parameters quoted in the table have been extracted from the recent study by Mahy et al (2022), except for three stars. One of them (HD 152200) is a newly discovered SB1 system, HD 46485 is confirmed "bona fide" SB1 system, and the third one (HD 165246) was studied in detail by Johnston et al (2021).…”

Section: Further Notes About the Properties Of Sb1 Systems And The Ch...mentioning

confidence: 99%

See 1 more Smart Citation

The IACOB project VIII. Searching for empirical signatures of binarity in fast-rotating O-type stars

Britavskiy¹,

S.²,

Holgado³

et al. 2023

Preprint

View full text Add to dashboard Cite

Context. The empirical distribution of projected rotational velocities (v sin i) in massive O-type stars is characterized by a dominant slow velocity component and a tail of fast rotators. Binary interaction has been proposed to play a dominant role in the formation of this tail. Aims. We perform a complete and homogeneous search for empirical signatures of binarity in a sample of 54 fast rotating stars with the aim of evaluating this hypothesis. This working sample has been extracted from a larger sample of 415 Galactic O-type stars which covers the full range of v sin i values. Methods. We use new and archival multi-epoch spectra in order to detect spectroscopic binary systems. We complement this information with Gaia proper motions and TESS photometric data to aid in the identification of runaway stars and eclipsing binaries, respectively. We also benefit from additional published information to provide a more complete overview of the empirical properties of our working sample of fast-rotating O-type stars.Results. The identified fraction of single-lined spectroscopic binary (SB1) systems and apparently single stars among the fast-rotating sample is ∼18% and ∼70%, respectively. The remaining 12% correspond to four secure double-line spectroscopic binaries (SB2) with at least one of the components having a v sin i > 200 km s −1 (∼8%), and a small sample of 2 stars (∼4%) for which the SB2 classification is doubtful: they could actually be single stars with a remarkable line-profile variability. When comparing these percentages with those corresponding to the slow rotating sample we find that our sample of fast rotators is characterized by a slightly larger percentage of SB1 systems (∼18% vs. ∼13%) and a considerably smaller fraction of clearly detected SB2 systems (8% vs. 33%). Overall, there seems to be a clear deficit of spectroscopic binaries (SB1+SB2) among fast rotating O-type stars (∼26% vs. ∼46%). On the contrary, the fraction of runaway stars is significantly higher in the fast-rotating domain (∼33-50%) than among those stars with v sin i < 200 km s −1 . Lastly, almost 65% of the apparently single fast-rotating stars are runaways. As a by-product, we have discovered a new over contact SB2 system (HD 165921) and two fast-rotating SB1 systems (HD 46485 and HD 152200) Also, we propose HD 94024 and HD 12323 (both SB1 systems with a v sin i < 200 km s −1 ) as candidates to host a quiescent stellar-mass black hole. Conclusions. Our empirical results seem to be in good agreement with the idea that the tail of fast-rotating O-type stars (with v sin i > 200 km s −1 ) is mostly populated by post-interaction binary products. In particular, we find that the final statistics of identified spectroscopic binaries and apparently single stars are in good agreement with newly computed predictions obtained with the binary population synthesis code BPASS and previous estimations obtained by previous authors.

show abstract

Section: Conclusion and Future Prospectssupporting

confidence: 52%

Section: Further Notes About the Properties Of Sb1 Systems And The Ch...mentioning

confidence: 99%

The IACOB project VIII. Searching for empirical signatures of binarity in fast-rotating O-type stars

Britavskiy¹,

S.²,

Holgado³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…We do not analyse the simulated LPV generated using the bruce code, as this is beyond the scope of the current paper and because it is only a toy model. For recent applications of the famias software package for identifying the mode geometry of pulsating stars, see Brunsden et al (2018), Aerts et al (2019), Moździerski et al (2019) and Johnston et al (2021).…”

Section: Analysis Methods Of Future Cubespec Datamentioning

confidence: 99%

The CubeSpec space mission

Bowman¹,

Vandenbussche²,

Sana³

et al. 2022

A&A

Self Cite

View full text Add to dashboard Cite

Context. There is currently a niche for providing high-cadence, high resolution, time-series optical spectroscopy from space, which can be filled by using a low-cost cubesat mission. The Belgian-led ESA/KU Leuven CubeSpec mission is specifically designed to provide space-based, low-cost spectroscopy with specific capabilities that can be optimised for a particular science need. Approved as an ESA in-orbit demonstrator, the CubeSpec satellite’s primary science objective will be to focus on obtaining high-cadence, high resolution optical spectroscopic data to facilitate asteroseismology of pulsating massive stars. Aims. In this first paper, we aim to search for pulsating massive stars suitable for the CubeSpec mission, specifically β Cep stars, which typically require time-series spectroscopy to identify the geometry of their pulsation modes. Methods. Based on the science requirements needed to enable asteroseismology of massive stars with the capabilities of CubeSpec’s spectrograph, we combined a literature study for pulsation with the analysis of recent high-cadence time-series photometry from the Transiting Exoplanet Survey Satellite (TESS) mission to classify the variability for stars brighter than V ≤ 4 mag and between O9 and B3 in spectral type. Results. Among the 90 stars that meet our magnitude and spectral type requirements, we identified 23 promising β Cep stars with high-amplitude (non-)radial pulsation modes with frequencies below 7 d−1. Using further constraints on projected rotational velocities, pulsation amplitudes, and the number of pulsation modes, we devised a prioritised target list for the CubeSpec mission according to its science requirements and the potential of the targets for asteroseismology. The full target catalogue further provides a modern TESS-based review of line profile and photometric variability properties among bright O9–B3 stars.

show abstract

“…Although this work focuses on massive stars, our general technique could also be applied to assess uncertainties on lower-mass stellar radii. They are relevant in the context of inferring stellar properties through eclipsing star (Maiz-Apellaniz et al 2004;Sota et al 2008;Handler et al 2012;Williams et al 2013;Cazorla et al 2017;Pozo Nuñez et al 2019;Trigueros Páez et al 2021;Johnston et al 2021) and transiting exoplanets observations (e.g., Henry et al 2000;Charbonneau et al 2000;Mandel & Agol 2002;Seager & Mallen-Ornelas 2003). The observed radius of a companion star/exoplanet obtained through these methods rely on the assumptions in radius of the primary/host star (e.g., Johnson et al 2017).…”

Section: Observational Implicationsmentioning

confidence: 99%

Dissecting the microphysics behind the metallicity-dependence of massive stars radii

Xin,

Renzo,

Metzger

2022

Preprint

View full text Add to dashboard Cite

Understanding the radii of massive stars throughout their evolution is important to answering numerous questions about stellar physics, from binary interactions on the main sequence to the pre-supernova radii. One important factor determining a star's radius is the fraction of its mass in elements heavier than Helium (metallicity, 𝑍). However, the metallicity enters stellar evolution through several distinct microphysical processes, and which dominates can change throughout stellar evolution and with the overall magnitude of 𝑍. We perform a series of numerical experiments with 15𝑀 MESA models computed doubling separately the metallicity entering the radiative opacity, the equation of state, and the nuclear reaction network to isolate the impact of each on stellar radii. We explore separately models centered around two metallicity values: one near solar 𝑍 = 0.02 and another sub-solar 𝑍 ∼ 10 −3 , and consider several key epochs from the end of the main sequence to core carbon depletion. We find that the metallicity entering the opacity dominates at most epochs for the solar metallicity models, contributing to on average ∼ 60 − 90% of the total change in stellar radius. Nuclear reactions have a larger impact (∼ 50 − 70%) during most epochs in the subsolar 𝑍 models. The methodology introduced here can be employed more generally to propagate known microphysics errors into uncertainties on macrophysical observables including stellar radii.

show abstract

Characterization of the variability in the O+B eclipsing binary HD 165246

Cited by 16 publications

References 116 publications

The IACOB project VIII. Searching for empirical signatures of binarity in fast-rotating O-type stars

The IACOB project VIII. Searching for empirical signatures of binarity in fast-rotating O-type stars

The CubeSpec space mission

Dissecting the microphysics behind the metallicity-dependence of massive stars radii

Contact Info

Product

Resources

About