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, Z.; Meynet, Georges; Shultz, Matt; David-Uraz, Alexandre; ud‐Doula, Asif; Townsend, R. H. D.; Wade, G. A.; Georgy, Cyril; Petit, Véronique; Owocki, S. P.

doi:10.1093/mnras/staa237

Cited by 61 publications

(53 citation statements)

References 139 publications

(226 reference statements)

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“…Note that if fossil fields should survive until the pre-MS phase, magnetic coupling could be ensured for stars of any masses, although this would concern however a very small fraction of OB stars (only ∼ 7% have surface magnetic fields; e.g. Keszthelyi et al 2020 and references therein).…”

Section: Applicability To Intermediate Mass Stars (2 − 5m ⊙ )mentioning

confidence: 99%

On the origin of the bimodal rotational velocity distribution in stellar clusters: rotation on the pre-main sequence

Bastian

Kamann

Amard

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We address the origin of the observed bimodal rotational distribution of stars in massive young and intermediate age stellar clusters. This bimodality is seen as split main sequences at young ages and also has been recently directly observed in the Vsini distribution of stars within massive young and intermediate age clusters. Previous models have invoked binary interactions as the origin of this bimodality, although these models are unable to reproduce all of the observational constraints on the problem. Here, we suggest that such a bimodal rotational distribution is set-up early within a cluster’s life, i.e. within the first few Myr. Observations show that the period distribution of low-mass ($\lesssim\! 2 \, \mathrm{M}_\odot$) pre-main-sequence (PMS) stars is bimodal in many young open clusters, and we present a series of models to show that if such a bimodality exists for stars on the PMS that it is expected to manifest as a bimodal rotational velocity (at fixed mass/luminosity) on the main sequence for stars with masses in excess of ∼1.5 M⊙. Such a bimodal period distribution of PMS stars may be caused by whether stars have lost (rapid rotators) or been able to retain (slow rotators) their circumstellar discs throughout their PMS lifetimes. We conclude with a series of predictions for observables based on our model.

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Section: Applicability To Intermediate Mass Stars (2 − 5m ⊙ )mentioning

confidence: 99%

On the origin of the bimodal rotational velocity distribution in stellar clusters: rotation on the pre-main sequence

Bastian

Kamann

Amard

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Furthermore, based on dedicated studies, such as MiMeS (Wade et al, 2016), the BOB campaign (Morel et al, 2015), and the BRITE spectropolarimetric survey (Neiner et al, 2017), ∼10% of massive stars are inferred to host a large-scale magnetic field with polar field strengths that range from ∼100 G up to a few kG. The degeneracies within evolutionary models are also more complex when dealing with the presence of magnetic fields in massive stars (Alecian et al, 2014;Shultz et al, 2018;Keszthelyi et al, 2019Keszthelyi et al, , 2020.…”

Section: Introductionmentioning

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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“…Recent modelling approaches 4 using the mesa software instrument have accounted for two surface effects of fossil magnetic fields in massive star models (Keszthelyi et al 2019(Keszthelyi et al , 2020. These approaches rely on two long-term phenomena which result from the magnetospheric-wind interaction, namely, massloss quenching (which reduces the mass-loss rate of the star, e.g.…”

Section: Impact Of Magnetic Fieldmentioning

confidence: 99%

“…We use mesa r-12115 and modelling assumptions that are similar to those of Keszthelyi et al (2020). The initial abundances are adopted as Z ini = 0.014, Y ini = 0.266, X ini = 0.72, and the initial distribution of metals follows the description of Asplund et al (2009), with isotopic ratios adopted from Lodders (2003).…”

Section: Mesa Model Descriptionmentioning

confidence: 99%

“…In addition to precise measurements of radii and luminosities, we assess the benefit of having seismic constraints, when available. In order to further strengthen the robustness of these results, we additionally use mesa software (Paxton et al 2011(Paxton et al , 2013(Paxton et al , 2015(Paxton et al , 2018(Paxton et al , 2019 where the effects of surface fossil magnetic fields have previously been implemented by Keszthelyi et al (2019Keszthelyi et al ( , 2020.…”

Section: Introductionmentioning

confidence: 99%

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Fundamental properties of a selected sample of Ap stars: Inferences from interferometric and asteroseismic constraints

Deal

Cunha

Keszthelyi

et al. 2021

A&A

Self Cite

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Context. Magnetic fields influence the formation and evolution of stars and impact the observed stellar properties. magnetic A-type stars (Ap stars) are a prime example of this. Access to precise and accurate determinations of their stellar fundamental properties, such as masses and ages, is crucial to understand the origin and evolution of fossil magnetic fields. Aims. We propose using the radii and luminosities determined from interferometric measurements, in addition to seismic constraints when available, to infer fundamental properties of 14 Ap stars préviously characterised. Methods. We used a grid-based modelling approach, employing stellar models computed with the CESTAM stellar evolution code, and the parameter search performed with the AIMS optimisation method. The stellar model grid was built using a wide range of initial helium abundances and metallicities in order to avoid any bias originating from the initial chemical composition. The large frequency separations (Δν) of HR 1217 (HD 24712) and α Cir (HD 128898), two rapidly oscillating Ap stars of the sample, were used as seismic constraints. Results. We inferred the fundamental properties of the 14 stars in the sample. The overall results are consistent within 1σ with previous studies, however, the stellar masses inferred in this study are higher. This trend likely originates from the broader range of chemical compositions considered in this work. We show that the use of Δν in the modelling significantly improves our inferences, allowing us to set reasonable constraints on the initial metallicity which is, otherwise, unconstrained. This gives an indication of the efficiency of atomic diffusion in the atmospheres of roAp stars and opens the possibility of characterising the transport of chemical elements in their interiors.

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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

Cited by 61 publications

References 139 publications

On the origin of the bimodal rotational velocity distribution in stellar clusters: rotation on the pre-main sequence

On the origin of the bimodal rotational velocity distribution in stellar clusters: rotation on the pre-main sequence

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

Fundamental properties of a selected sample of Ap stars: Inferences from interferometric and asteroseismic constraints

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