Asteroseismology of Massive Stars with the TESS Mission: The Runaway β Cep Pulsator PHL 346 = HN Aqr

Handler, G.; Pigulski, A.; Daszyńska‐Daszkiewicz, J.; Irrgang, A.; Kilkenny, D.; Guo, Zhao; Przybilla, N.; Aliçavuş, Filiz Kahraman; Kallinger, T.; Pascual-Granado, J.; Niemczura, E.; Różański, Tomasz; Chowdhury, S.; Buzasi, Derek L.; Mirouh, Giovanni M.; Bowman, D. M.; Johnston, C.; Pedersen, May G.; Moravveji, E.; Gazeas, K.; Cat, P. De; Vanderspek, R.; Ricker, G.

doi:10.3847/2041-8213/ab095f

Cited by 26 publications

(21 citation statements)

References 41 publications

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“…Some of the pulsating stars or candidates reported here are located at rather large distances from the Galactic plane and are therefore candidate runaway stars. This is interesting both from the stellar evolutionary and asteroseismic point of view because the flight time of a runaway star provides a limit on the stellar age that can be imposed on seismic models (Handler et al 2019). Having such a constraint at hand could be of similar importance to basic stellar parameters from pulsators in eclipsing binaries.…”

Section: Discussionmentioning

confidence: 99%

New Beta Cephei Stars from the KELT Project

Labadie-Bartz

Handler

Pepper

et al. 2020

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We present the results of a search for Galactic β Cephei stars, which are massive pulsating stars with both pressure modes and mixed modes. Thus, these stars can serve as benchmarks for seismological studies of the interiors of massive stars. We conducted the search by performing a frequency analysis on the optical light curves of known Oand B-type stars with data from the Kilodegree Extremely Little Telescope exoplanet survey. We identify 113 β Cephei stars, of which 86 are new discoveries, which altogether represent a 70% increase in the number currently known. An additional 97 candidates are identified. Among our targets, we find five new eclipsing binaries and 22 stars with equal frequency spacings suggestive of rotational splitting of nonradial pulsation modes. Candidates for runaway stars among our targets and a number of interesting individual objects are discussed. Most of the known and newly discovered β Cephei stars will be observed by the Transiting Exoplanet Survey Satellite mission, providing by far the most comprehensive observational data set of massive main-sequence pulsating stars of sufficient quality for detailed asteroseismic studies. Future analysis of these light curves has the potential to dramatically increase our understanding of the structure of stellar interiors and the physical processes taking place therein. Unified Astronomy Thesaurus concepts: Beta Cepheid variable stars (148); Asteroseismology (73); Stellar oscillations (1617); Multi-periodic variable stars (1079); Pulsating variable stars (1307); Short period variable stars (1453); Early-type variable stars (432); Light curves (918); Light curve classification (1954); Surveys (1671); B stars (128) Supporting material: data behind figure, machine-readable tables

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Section: Discussionmentioning

confidence: 99%

New Beta Cephei Stars from the KELT Project

Labadie-Bartz

Handler

Pepper

et al. 2020

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“…Such an observing strategy is optimized to find transiting exoplanets orbiting bright stars across the sky, but TESS data are also extremely valuable for massive star asteroseismology. Amongst the earliest studies of massive star variability as viewed by TESS are those by Handler et al (2019), Bowman et al (2019b) and Pedersen et al (2019) in which the diverse variability of massive stars is demonstrated using a total sample of more than 200 massive stars. The study by Handler et al (2019) considers one of the first β Cep stars observed by the TESS mission, which revealed it to be multi-periodic and subsequent asteroseismic modeling indicated it was a runaway star because of its inferred age.…”

Section: The Tess Missionmentioning

confidence: 99%

“…Thus, detailed forward seismic modeling of many high-mass TESS targets are expected in the not-so-distant future. We refer the reader to Handler et al (2019) for the first modeling study of a β Cep star using TESS data. Despite the relatively small sample size so far compared to intermediate-mass stars, asteroseismic studies of massive stars have demonstrated the need to include improved prescriptions for convective core overshooting and envelope mixing given that current evolution models underestimate the core masses of massive stars and consequently also their mainsequence lifetimes.…”

Section: Space-based Studiesmentioning

confidence: 99%

Asteroseismology of High-Mass Stars: New Insights of Stellar Interiors With Space Telescopes

Bowman

2020

Front. Astron. Space Sci.

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Massive stars are important metal factories in the Universe. They have short and energetic lives, and many of them inevitably explode as a supernova and become a neutron star or black hole. In turn, the formation, evolution and explosive deaths of massive stars impact the surrounding interstellar medium and shape the evolution of their host galaxies. Yet the chemical and dynamical evolution of a massive star, including the chemical yield of the ultimate supernova and the remnant mass of the compact object, strongly depend on the interior physics of the progenitor star. We currently lack empirically calibrated prescriptions for various physical processes at work within massive stars, but this is now being remedied by asteroseismology. The study of stellar structure and evolution using stellar oscillations-asteroseismology-has undergone a revolution in the last two decades thanks to high-precision time series photometry from space telescopes. In particular, the long-term light curves provided by the MOST, CoRoT, BRITE, Kepler/K2, and TESS missions provided invaluable data sets in terms of photometric precision, duration and frequency resolution to successfully apply asteroseismology to massive stars and probe their interior physics. The observation and subsequent modeling of stellar pulsations in massive stars has revealed key missing ingredients in stellar structure and evolution models of these stars. Thus, asteroseismology has opened a new window into calibrating stellar physics within a highly degenerate part of the Hertzsprung-Russell diagram. In this review, I provide a historical overview of the progress made using ground-based and early space missions, and discuss more recent advances and breakthroughs in our understanding of massive star interiors by means of asteroseismology with modern space telescopes.

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“…Although approximate prescriptions have been developed to take these into account in one-dimensional models (e.g., Endal & Sofia 1978;Pinsonneault et al 1989;Zahn 1992;Maeder & Zahn 1998;Heger et al 2000;Meynet et al 2013), the rigorous validation of transport processes in massive stars is still underway. Although the pulsational properties of O-type stars are mostly unknown, in principle, asteroseismology is a powerful tool to gain such information and has indeed been successfully applied in the case of a small sample of pulsating B-type stars (e.g., Briquet et al 2012;Moravveji et al 2015;Pápics et al 2017;Buysschaert et al 2018;Handler et al 2019).…”

Section: Surface Angular Velocitymentioning

confidence: 99%

The effects of surface fossil magnetic fields on massive star evolution – II. Implementation of magnetic braking in mesa and implications for the evolution of surface rotation in OB stars

Keszthelyi

Meynet

Shultz

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The time evolution of angular momentum and surface rotation of massive stars is strongly influenced by fossil magnetic fields via magnetic braking. We present a new module containing a simple, comprehensive implementation of such a field at the surface of a massive star within the Modules for Experiments in Stellar Astrophysics (mesa) software instrument. We test two limiting scenarios for magnetic braking: distributing the angular momentum loss throughout the star in the first case, and restricting the angular momentum loss to a surface reservoir in the second case. We perform a systematic investigation of the rotational evolution using a grid of OB star models with surface magnetic fields (M = 5 − 60 M , Ω/Ω crit = 0.2 − 1.0, B p = 1 − 20 kG). We then employ a representative grid of B-type star models (M = 5, 10, 15 M , Ω/Ω crit = 0.2, 0.5, 0.8, B p = 1, 3, 10, 30 kG) to compare to the results of a recent selfconsistent analysis of the sample of known magnetic B-type stars. We infer that magnetic massive stars arrive at the zero age main sequence with a range of rotation rates, rather than with one common value. In particular, some stars are required to have close-to-critical rotation at the ZAMS. However, magnetic braking yields surface rotation rates converging to a common low value, making it difficult to infer the initial rotation rates of evolved, slowly-rotating stars.

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Asteroseismology of Massive Stars with the TESS Mission: The Runaway β Cep Pulsator PHL 346 = HN Aqr

Cited by 26 publications

References 41 publications

New Beta Cephei Stars from the KELT Project

New Beta Cephei Stars from the KELT Project

Asteroseismology of High-Mass Stars: New Insights of Stellar Interiors With Space Telescopes

The effects of surface fossil magnetic fields on massive star evolution – II. Implementation of magnetic braking in mesa and implications for the evolution of surface rotation in OB stars

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