Three-dimensional Simulations of Massive Stars. I. Wave Generation and Propagation

Edelmann, P. V. F.; Ratnasingam, R. P.; Pedersen, May G.; Bowman, D. M.; Prat, V.; Rogers, T. M.

doi:10.3847/1538-4357/ab12df

Cited by 99 publications

(127 citation statements)

References 59 publications

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“…However there were few firm detections of IGWs in massive stars before this study 15,16,21 . Recent two-dimensional (2D) and 3D spherical numerical simulations using a realistic stellar structure model predict the excitation of IGWs by turbulent core convection, and an amplitude spectrum for IGWs with a value between 0.8 and 3 for the frequency exponent gamma [26][27][28] . On the other hand, 3D simulations in a Cartesian box in idealized conditions predict a steeper IGW amplitude spectrum with 3.25 as the frequency exponent 30 As a next step, spectroscopy of these stars will allow the determination of fundamental stellar parameters, which are necessary to perform asteroseismic modelling and to constrain interior properties, including the measurement of a star's age, core mass and interior rotation profile.…”

Section: Discussionmentioning

confidence: 99%

Low-frequency gravity waves in blue supergiants revealed by high-precision space photometry

et al. 2019

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Almost all massive stars explode as supernovae and form a black hole or neutron star. The remnant mass and the impact of the chemical yield on subsequent star formation and galactic evolution strongly depend on the internal physics of the progenitor star, which is currently not well understood. The theoretical uncertainties of stellar interiors accumulate with stellar age, which is particularly pertinent for the blue supergiant phase. Stellar oscillations represent a unique method of probing stellar interiors, yet inference for blue supergiants is hampered by a dearth of observed pulsation modes. Here we report the detection of diverse variability in blue supergiants using the K2 and TESS space missions. The discovery of pulsation modes or an entire spectrum of low-frequency gravity waves in these stars allow us to map the evolution of hot massive stars towards the ends of their lives. Future asteroseismic modelling will provide constraints on ages, core masses, interior mixing, rotation and angular momentum transport. The discovery of variability in blue supergiants is a step towards a data-driven empirical calibration of theoretical evolution models for the most massive stars in the Universe.Stars born with masses larger than approximately eight times the mass of the Sun play a significant role in the evolution of galaxies. They are the chemical factories that produce and expel heavy elements through their wind and when they end their lives as supernovae and form a black hole or neutron star 1-3 . However, the chemical yields that enrich the interstellar medium and the remnant mass strongly depend on the progenitor star's interior properties 4 . The detectable progenitors of supernovae include blue supergiant stars, which are hot massive stars in a shell-hydrogen or core-helium burning stage of stellar evolution. Stellar evolution models of these post-main sequence stars contain by far the largest uncertainties in stellar astrophysics, as observational constraints on interior mixing, rotation and angular momentum transport are missing. These phenomena are further compounded when coupled with mass loss, binarity and magnetic fields 1-3 . Across astrophysics, from star formation to galactic evolution, it is imperative to calibrate theoretical models of massive stars using observations because they determine the evolution of the cosmos.A unique methodology for probing stellar interiors is asteroseismology 5 , which -similarly to seismology of earthquakes -uses oscillations to derive constraints on the structure of stars.The study of stellar interiors of low-mass stars like the Sun has undergone a revolution in

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Section: Discussionmentioning

confidence: 99%

Low-frequency gravity waves in blue supergiants revealed by high-precision space photometry

et al. 2019

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“…Cristini et al 2017;Jones et al 2017), which affects the chemical composition profile that is left behind of the retreating hydrogen core. Furthermore, 3D simulations clearly show that at the interface of the convective and radiative region internal gravity waves are generated, that propagate to the surface (Cristini et al 2017;Edelmann et al 2019). How much these waves mix the composition needs to be determined but they definitely affect the radiative region above the convective core.…”

Section: Discussionmentioning

confidence: 99%

Relative importance of convective uncertainties in massive stars

Kaiser

Hirschi

Arnett

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT In this work, we investigate the impact of uncertainties due to convective boundary mixing (CBM), commonly called ‘overshoot’, namely the boundary location and the amount of mixing at the convective boundary, on stellar structure and evolution. For this we calculated two grids of stellar evolution models with the MESA code, each with the Ledoux and the Schwarzschild boundary criterion, and vary the amount of CBM. We calculate each grid with the initial masses of 15, 20, and $25\, \rm {M}_\odot$. We present the stellar structure of the models during the hydrogen and helium burning phases. In the latter, we examine the impact on the nucleosynthesis. We find a broadening of the main sequence with more CBM, which is more in agreement with observations. Furthermore, during the core hydrogen burning phase there is a convergence of the convective boundary location due to CBM. The uncertainties of the intermediate convective zone remove this convergence. The behaviour of this convective zone strongly affects the surface evolution of the model, i.e. how fast it evolves redwards. The amount of CBM impacts the size of the convective cores and the nucleosynthesis, e.g. the 12C to 16O ratio and the weak s-process. Lastly, we determine the uncertainty that the range of parameter values investigated introduces and we find differences of up to $70{{\ \rm per\ cent}}$ for the core masses and the total mass of the star.

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“…A recent discovery made using the CoRoT, K2, and TESS missions was that the vast majority of early-type stars have significant low-frequency variability in photometry (Bowman et al, 2019a,b). Such stochastic variability is not predicted from the κ-mechanism, but is expected from convectively-driven internal gravity waves (IGWs) excited by core convection (Rogers et al, 2013;Rogers, 2015;Edelmann et al, 2019;Horst et al, 2020). 2D and 3D hydrodynamical simulations predict that IGWs reach the surface with significant amplitudes and provide detectable perturbations in temperature and velocity (Edelmann et al, 2019), and that IGWs are also extremely efficient at transporting angular momentum and chemical elements (Rogers, 2015;Rogers and McElwaine, 2017).…”

Section: Diverse Photometric Variability In Massive Starsmentioning

confidence: 99%

“…2D and 3D hydrodynamical simulations predict that IGWs reach the surface with significant amplitudes and provide detectable perturbations in temperature and velocity (Edelmann et al, 2019), and that IGWs are also extremely efficient at transporting angular momentum and chemical elements (Rogers, 2015;Rogers and McElwaine, 2017). A snapshot of a 3D simulation of IGWs propagating within a 3-M ⊙ main-sequence star from Edelmann et al (2019) is shown in Figure 6.…”

Section: Diverse Photometric Variability In Massive Starsmentioning

confidence: 99%

“…There are currently four known excitation mechanisms that can trigger variability in early-type stars: (i) coherent p and g modes excited by the κ-mechanism Gautschy and Saio, 1993;Szewczuk and Daszyńska-Daszkiewicz, 2017); (ii) IGWs generated by turbulent core convection (Edelmann et al, 2019); (iii) IGWs generated by thin sub-surface convection zones (Cantiello et al, 2009); and (iv) waves generated from tides in binary systems (Fuller, 2017). Whereas, essentially all of the asteroseismic results discussed in section 4 are based on heat-driven modes, the other variability mechanisms in massive stars remain somewhat under-utilized despite having great probing power of stellar interiors.…”

Section: Diverse Photometric Variability In Massive Starsmentioning

confidence: 99%

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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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Three-dimensional Simulations of Massive Stars. I. Wave Generation and Propagation

Cited by 99 publications

References 59 publications

Low-frequency gravity waves in blue supergiants revealed by high-precision space photometry

Low-frequency gravity waves in blue supergiants revealed by high-precision space photometry

Relative importance of convective uncertainties in massive stars

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

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