Moving and reactive boundary conditions in moving-mesh hydrodynamics

Prust, Logan J.

doi:10.1093/mnras/staa1031

Cited by 6 publications

(3 citation statements)

References 41 publications

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“…Different parameters (efficiency of jet launching, inclination angle of the jet) are explored. In some cases, a neutron-star could drive a jet that breaks through the material piled up around it (López-Cámara et al 2019, 2020. A white dwarf companion star, however needs a very high efficiency to successfully launch a jet and for main sequence stars accretion is found to be too weak so that the jet does not break out of a RG star envelope but is choked (López-Cámara et al 2022).…”

Section: Simulations Of the Companion-envelope Interactionmentioning

confidence: 99%

“…A rigorous assessment of the relevance of these effects for CEE is still missing, but some aspects of accretion onto the stellar cores, the potential formation of a disk and jet-like outflows have been explored in more detail (e.g. Chamandy et al 2018;Hillel et al 2022;López-Cámara et al 2019, 2020MacLeod and Ramirez-Ruiz 2015a, b;Moreno Méndez et al 2017;Schreier et al 2019Schreier et al , 2021Schreier et al , 2023Shiber et al 2019;Soker 2016b;Zou et al 2022).…”

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confidence: 99%

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Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques

Roepke

Marco

2023

Living Rev Comput Astrophys

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When the primary star in a close binary system evolves into a giant and engulfs its companion, its core and the companion temporarily orbit each other inside a common envelope. Drag forces transfer orbital energy and angular momentum to the envelope material. Depending on the efficiency of this process, the envelope may be ejected leaving behind a tight remnant binary system of two stellar cores, or the cores merge retaining part of the envelope material. The exact outcome of common-envelope evolution is critical for in the formation of X-ray binaries, supernova progenitors, the progenitors of compact-object mergers that emit detectable gravitational waves, and many other objects of fundamental astrophysical relevance. The wide ranges of spatial and temporal timescales that characterize common-envelope interactions and the lack of spatial symmetries present a substantial challenge to generating consistent models. Therefore, these critical phases are one of the largest sources for uncertainty in classical treatments of binary stellar evolution. Three-dimensional hydrodynamic simulations of at least part of the common-envelope interaction are the key to gain predictive power in modeling common-envelope evolution. We review the development of theoretical concepts and numerical approaches for such three-dimensional hydrodynamic simulations. The inherent multi-physics, multi-scale challenges have resulted in a wide variety of approximations and numerical techniques to be exercised on the problem. We summarize the simulations published to date and their main results. Given the recent rapid progress, a sound understanding of the physics of common-envelope interactions is within reach and thus there is hope that one of the remaining fundamental problems of stellar astrophysics may be solved before long.

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Section: Simulations Of the Companion-envelope Interactionmentioning

confidence: 99%

mentioning

confidence: 99%

Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques

Roepke

Marco

2023

Living Rev Comput Astrophys

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“…11 There are many researches on the distributed parameter system of moving boundaries, such as the Stefan problem 12,13 that has been raised since the 19th century. In addition, there are the invasion of viruses or cancer cells in biology, 14 problems in the field of fluid mechanics, 15 and Czochralski crystal growth process. 16,17 For the research on the control problems of distributed parameter systems with moving boundaries, robust control, 18 feedback control, 19,20 and optimal control 21 are some of the most important control methods.…”

Section: Introductionmentioning

confidence: 99%

Closed loop variable gain ILC for a class of nonlinear parabolic distributed parameter systems with moving boundaries

Dai

Zhang

et al. 2021

Optim Control Appl Methods

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This article researched the output tracking problem of a class of nonlinear parabolic distributed parameter systems with moving boundaries. Considering the large deviation of the initial state reset of the system, a closed-loop variable gain accelerated iterative learning control algorithm is designed. And sufficient condition for the convergence of the tracking error is given. Through rigorous theoretical analysis guaranteed that the tracking error of the system converges to zero in the positive direction of the iteration axis in the sense of the L 2 norm.Finally, the effectiveness of the designed algorithm is verified by a numerical simulation.

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General relativistic hydrodynamics on a moving-mesh I: static space–times

Chang

Etienne

2020

Monthly Notices of the Royal Astronomical Society

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We present the moving-mesh general relativistic hydrodynamics solver for static space–times as implemented in the code, MANGA. Our implementation builds on the architectures of MANGA and the numerical relativity python package NRPy+. We review the general algorithm to solve these equations and, in particular, detail the time-stepping; Riemann solution across moving faces; conversion between primitive and conservative variables; validation and correction of hydrodynamic variables; and mapping of the metric to a Voronoi moving-mesh grid. We present test results for the numerical integration of an unmagnetized Tolman–Oppenheimer–Volkoff star for 24 dynamical times. We demonstrate that at a resolution of 106 mesh generating points, the star is stable and its central density drifts downwards by 2 per cent over this time-scale. At a lower resolution, the central density drift increases in a manner consistent with the adopted second-order spatial reconstruction scheme. These results agree well with the exact solutions, and we find the error behaviour to be similar to Eulerian codes with second-order spatial reconstruction. We also demonstrate that the new code recovers the fundamental mode frequency for the same TOV star but with its initial pressure depleted by 10 per cent.

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Moving and reactive boundary conditions in moving-mesh hydrodynamics

Cited by 6 publications

References 41 publications

Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques

Simulations of common-envelope evolution in binary stellar systems: physical models and numerical techniques

Closed loop variable gain ILC for a class of nonlinear parabolic distributed parameter systems with moving boundaries

General relativistic hydrodynamics on a moving-mesh I: static space–times

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