Zobrazeno 1 - 10
of 47
pro vyhledávání: '"Radiative magnetohydrodynamics"'
Publikováno v:
The Astrophysical Journal Letters, Vol 969, Iss 2, p L34 (2024)
Magnetic tornadoes, characterized as impulsive Alfvén waves initiated by photospheric vortices in intergranular lanes, are considered efficient energy channels to the corona. Despite their acknowledged importance for solar coronal heating, their obs
Externí odkaz:
https://doaj.org/article/3a40722b971f4423a9348e5c7847e13c
Publikováno v:
The Astrophysical Journal Letters, Vol 965, Iss 2, p L29 (2024)
Active galactic nuclei (AGN) light curves observed with different wave bands show that the variability in longer wavelength bands lags the variability in shorter wavelength bands. Measuring these lags, or reverberation mapping, is used to measure the
Externí odkaz:
https://doaj.org/article/1fc21377e1c9470785ec17bed781053f
Dependence of Spicule Properties on the Magnetic Field—Results from Magnetohydrodynamics Simulations
Publikováno v:
The Astrophysical Journal, Vol 973, Iss 1, p 49 (2024)
Solar spicules are plasma jets observed in the interface region between the visible solar surface and the corona. At any given time, there is a forest of spicules originating in the chromosphere of the Sun. While various models attempt to elucidate t
Externí odkaz:
https://doaj.org/article/8a4474ac8b0345ff817cb670bcd7d38a
Autor:
Yuta Asahina, Ken Ohsuga
Publikováno v:
The Astrophysical Journal, Vol 973, Iss 1, p 45 (2024)
We perform a three-dimensional general relativistic radiation magnetohydrodynamics simulation of a tilted super-Eddington accretion disk around a spinning black hole (BH). The disk, which tilts and twists as it approaches the BH, precesses while main
Externí odkaz:
https://doaj.org/article/90967f2d914945529e4dbc3bf7fccddc
Publikováno v:
The Astrophysical Journal, Vol 972, Iss 1, p 18 (2024)
In our study, we examine a 2D radiation, relativistic, magnetohydrodynamics accretion flow around a spinning supermassive black hole. We begin by setting an initial equilibrium torus around the black hole, with an embedded initial magnetic field insi
Externí odkaz:
https://doaj.org/article/26c30a5e0ae74772aff8eea8f6e9639b
Publikováno v:
The Astrophysical Journal, Vol 970, Iss 1, p 24 (2024)
We describe the Stagger code for simulations of magnetohydrodynamic (MHD) systems. This is a modular code with a variety of physics modules that will let the user run simulations of deep stellar atmospheres, sunspot formation, stellar chromospheres a
Externí odkaz:
https://doaj.org/article/1ab0dedd271e4bb2bbca5b4f65d3facf
Publikováno v:
The Astrophysical Journal, Vol 970, Iss 1, p 3 (2024)
The dispersion relation of the magnetized Kelvin–Helmholtz (KH) instability driven by shear flow with zero thickness of the shear layer is derived theoretically based on a set of magnetohydrodynamic equations in the presence of a transverse magneti
Externí odkaz:
https://doaj.org/article/ba8b9f43649a4dc3bb94a6ee59d2f73d
Autor:
Taichi Igarashi, Hiroyuki R. Takahashi, Tomohisa Kawashima, Ken Ohsuga, Yosuke Matsumoto, Ryoji Matsumoto
Publikováno v:
The Astrophysical Journal, Vol 968, Iss 2, p 121 (2024)
Strong soft X-ray emission called soft X-ray excess is often observed in luminous active galactic nuclei (AGN). It has been suggested that the soft X-rays are emitted from a warm ( T = 10 ^6 ∼ 10 ^7 K) region that is optically thick for the Thomson
Externí odkaz:
https://doaj.org/article/de23d71abb0542e4aad68286f49a9d30
Publikováno v:
The Astrophysical Journal, Vol 968, Iss 1, p 29 (2024)
Turbulence is crucial for protoplanetary disk dynamics, and vertical shear instability (VSI) is a promising mechanism in outer disk regions to generate turbulence. We use the Athena++ radiation module to study VSI in full and transition disks, accoun
Externí odkaz:
https://doaj.org/article/46a027d815534eec90d80afdecc5e638
Autor:
Gennaro D’Angelo, Peter Bodenheimer
Publikováno v:
The Astrophysical Journal, Vol 967, Iss 2, p 124 (2024)
We compute the accretion efficiency of small solids, with radii 1 cm ≤ R _s ≤ 10 m, on planets embedded in gaseous disks. Planets have masses 3 ≤ M _p ≤ 20 Earth masses ( M _⊕ ) and orbit within 10 au of a solar mass star. Disk thermodynami
Externí odkaz:
https://doaj.org/article/7fdf4f11fbe64efea41e82813fbd7726