Статья

Modules for Experiments in Stellar Astrophysics ( ): Convective Boundaries, Element Diffusion, and Massive Star Explosions

Bill PaxtonKavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USAJosiah SchwabDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAEvan B. BauerDepartment of Physics, University of California, Santa Barbara, CA 93106, USALars BildstenKavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USAС. И. БлинниковKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, JapanPaul C. DuffellDepartment of Astronomy and Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USAR. FarmerAnton Pannenkoek Institute for Astronomy, University of Amsterdam, NL-1090 GE Amsterdam, The NetherlandsJared A. GoldbergDepartment of Physics, University of California, Santa Barbara, CA 93106, USAPablo MarchantDepartment of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USAE. I. SorokinaNIC Kurchatov Institute—Institute for Theoretical and Experimental Physics (ITEP), 117218 Moscow, RussiaAnne ThoulSpace sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 Août 19C, Bat. B5C, 4000 Liège, BelgiumR. H. D. TownsendDepartment of Astronomy, University of Wisconsin-Madison, Madison, WI 53706, USAF. X. TimmesSchool of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA

2018en

ABI

Аннотация

Abstract We update the capabilities of the software instrument Modules for Experiments in Stellar Astrophysics ( MESA ) and enhance its ease of use and availability. Our new approach to locating convective boundaries is consistent with the physics of convection, and yields reliable values of the convective-core mass during both hydrogen- and helium-burning phases. Stars with become white dwarfs and cool to the point where the electrons are degenerate and the ions are strongly coupled, a realm now available to study with MESA due to improved treatments of element diffusion, latent heat release, and blending of equations of state. Studies of the final fates of massive stars are extended in MESA by our addition of an approximate Riemann solver that captures shocks and conserves energy to high accuracy during dynamic epochs. We also introduce a 1D capability for modeling the effects of Rayleigh–Taylor instabilities that, in combination with the coupling to a public version of the radiation transfer instrument, creates new avenues for exploring Type II supernova properties. These capabilities are exhibited with exploratory models of pair-instability supernovae, pulsational pair-instability supernovae, and the formation of stellar-mass black holes. The applicability of MESA is now widened by the capability to import multidimensional hydrodynamic models into MESA . We close by introducing software modules for handling floating point exceptions and stellar model optimization, as well as four new software tools— , -Docker, , and mesastar.org—to enhance MESA ’s education and research impact.

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Идентификаторы

DOI: 10.3847/1538-4365/aaa5a8

Цитирования и источники

Цитирований: 11Использованных источников: 0

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