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Physica Scripta, 1984
The mass loss phenomenon in hot luminous stars is discussed and models for the structure of the wind, two component models and shock models are described. The constraints on models by X-ray observations are analysed. Hot stars return considerable amounts of matter and energy to the interstellar medium; the importance of this flow of energy and matter ...
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The mass loss phenomenon in hot luminous stars is discussed and models for the structure of the wind, two component models and shock models are described. The constraints on models by X-ray observations are analysed. Hot stars return considerable amounts of matter and energy to the interstellar medium; the importance of this flow of energy and matter ...
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Cosmic-ray-driven galactic wind
Il Nuovo Cimento B Series 11, 1991A simple one-dimensional Cartesian solution of the magnetohydrodynamic equations describing the global motion of interstellar matter including the effects of cosmic-ray and magnetic-field pressure is presented. First an adiabatic equation of state for the thermal background plasma and a loss-free cosmic-ray gas in the strong-scattering limit is ...
H. Fichtner +5 more
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2012
Kontext: Untersuchung der Charakteristika von galaktischen Winden bei Simulation von multiplen Supernovaexplosionen. Weiters wird der Einfluss von Diffusion untersucht. Ziele: Zeitlich versetzten Supernova-Explosionen führt zur Ausbildung von multiplen Schockwellen.
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Kontext: Untersuchung der Charakteristika von galaktischen Winden bei Simulation von multiplen Supernovaexplosionen. Weiters wird der Einfluss von Diffusion untersucht. Ziele: Zeitlich versetzten Supernova-Explosionen führt zur Ausbildung von multiplen Schockwellen.
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Galactic winds from primeval galaxies
Astrophysics and Space Science, 2007Ultra-high resolution hydrodynamic simulations using 10243 grid points are performed of early supernova burst in a forming galaxy, with properties similar to those inferred for Lyman α emitters (LAEs) and Lyman Break Galaxies (LBGs). We show that, at the earliest stages of less than 300 Myr, continual supernova explosions produce multitudinous hot ...
Masao Mori, Masayuki Umemura
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Nature Astronomy, 2020
A Galactic wind blowing from the Milky Way nucleus has swept up a few hundred clouds of atomic gas. New observations reveal dense molecular cores in two of these clouds, indicating a high loss rate of interstellar gas from the Galactic centre.
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A Galactic wind blowing from the Milky Way nucleus has swept up a few hundred clouds of atomic gas. New observations reveal dense molecular cores in two of these clouds, indicating a high loss rate of interstellar gas from the Galactic centre.
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The physics of galactic winds driven by cosmic rays – II. Isothermal streaming solutions
Monthly Notices of the Royal Astronomical Society, 2021Eliot Quataert +2 more
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Powerful Outflows and Feedback from Active Galactic Nuclei
Annual Review of Astronomy and Astrophysics, 2015Andrew King
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Particle Acceleration in Galactic Winds
2006Galactic winds are driven by pressure gradients of the thermal gas, the energetic particles and the magnetic waves. In the case of time-dependent inner boundary conditions (e.g. super bubbles, star burst regions) shock waves are generated within the wind thereby also re-accelerating the cosmic rays and modifying the flow structure.
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