Simulations of stellar convection, pulsation and semiconvection

Muthsam, H.; Kupka, F.; Mundprecht, Eva; Zaussinger, Florian; Grimm‐Strele, Hannes; Happenhofer, Natalie

doi:10.1017/s1743921311017595

Cited by 5 publications

(7 citation statements)

References 10 publications

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“…The ANTARES code was originally developed at the University of Vienna for the simulation of surface convec-tion (Muthsam et al, 2007(Muthsam et al, , 2010a; Lemmerer et al, 2013). Recently, the code was also applied to many other astrophysical problems (Kupka et al, 2009;Muthsam et al, 2010b;Kupka et al, 2012;Happenhofer et al, 2013;Zaussinger and Spruit, 2013;Mundprecht et al, 2013). In some of these applications problems arose due to the use of closed boundary conditions (Kupka et al, 2009;Mundprecht et al, 2013).…”

Section: Introductionmentioning

confidence: 99%

Realistic simulations of stellar surface convection with ANTARES: I. Boundary conditions and model relaxation

et al. 2015

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Section: Introductionmentioning

confidence: 99%

Realistic simulations of stellar surface convection with ANTARES: I. Boundary conditions and model relaxation

et al. 2015

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“…15 and 16 of [58], where h ≈ 9.8 km, whence Re eff ≈ 677. A change only occurs at even higher Re eff and was first shown in [55] who demonstrated the transition to a highly turbulent flow once the resolution is increased from 7.4 km (and thus Re eff ≈ 984) to 3.7 km (with Re eff ≈ 2479) and can be inspected by comparing Fig. 1 with Fig.…”

Section: D Simulations Of Overshootingmentioning

confidence: 75%

“…Figure 1. Numerical simulation of convection at the solar surface, presented originally in [55]. The isosurface where T = 6000 K is shown by a dark yellow shade.…”

Section: Modelling Of Convectionmentioning

confidence: 99%

Thermal Convection in Stars and in Their Atmosphere

Kupka¹

2020

Preprint

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Thermal convection is one of the main mechanisms of heat transport and mixing in stars in general and also in the photospheric layers which emit the radiation that we observe with astronomical instruments. The present lecture notes first introduce the role of convection in astrophysics and explain the basic physics of convection. This is followed by an overview on the modelling of convection. Challenges and pitfalls in numerical simulation based modelling are discussed subsequently. Finally, a particular application for the previously introduced concepts is described in more detail: the study of convective overshooting into stably stratified layers around convection zones in stars.

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“… 2007 ) to Cepheid pulsation (Muthsam et al. 2011 ), the code has not received much attention in the solar physics community so far. While, for the time being, the code is restricted to the modeling of the quiet Sun, an MHD upgrade is foreseen in the near future that will allow us to study the modifications to the dynamics and to the energy transport due to the photospheric magnetic field and to extend its applicability to magnetoactive regions at the solar surface.…”

Section: Introductionmentioning

confidence: 99%

Structure of the solar photosphere studied from the radiation hydrodynamics code ANTARES

Leitner

Lemmerer

Hanslmeier

et al. 2017

Astrophys Space Sci

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The ANTARES radiation hydrodynamics code is capable of simulating the solar granulation in detail unequaled by direct observation. We introduce a state-of-the-art numerical tool to the solar physics community and demonstrate its applicability to model the solar granulation. The code is based on the weighted essentially non-oscillatory finite volume method and by its implementation of local mesh refinement is also capable of simulating turbulent fluids. While the ANTARES code already provides promising insights into small-scale dynamical processes occurring in the quiet-Sun photosphere, it will soon be capable of modeling the latter in the scope of radiation magnetohydrodynamics. In this first preliminary study we focus on the vertical photospheric stratification by examining a 3-D model photosphere with an evolution time much larger than the dynamical timescales of the solar granulation and of particular large horizontal extent corresponding to on the solar surface to smooth out horizontal spatial inhomogeneities separately for up- and downflows. The highly resolved Cartesian grid thereby covers of the upper convection zone and the adjacent photosphere. Correlation analysis, both local and two-point, provides a suitable means to probe the photospheric structure and thereby to identify several layers of characteristic dynamics: The thermal convection zone is found to reach some ten kilometers above the solar surface, while convectively overshooting gas penetrates even higher into the low photosphere. An wide transition layer separates the convective from the oscillatory layers in the higher photosphere.

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Simulations of stellar convection, pulsation and semiconvection

Cited by 5 publications

References 10 publications

Realistic simulations of stellar surface convection with ANTARES: I. Boundary conditions and model relaxation

Realistic simulations of stellar surface convection with ANTARES: I. Boundary conditions and model relaxation

Thermal Convection in Stars and in Their Atmosphere

Structure of the solar photosphere studied from the radiation hydrodynamics code ANTARES

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