Book Chapter10.1007/978-94-009-3861-8_7
The High-Energy Component of the ISM—Cosmic-Ray Phenomena
Hans Bloemen
- 01 Jan 1987
- Vol. 134, pp 143-168
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TL;DR: The role of cosmic rays among the magnetic-field, gaseous, and stellar components in a possible large-scale hydrostatic equilibrium of the Galaxy is discussed in this paper.
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Abstract: Salient properties of cosmic rays and their interactions with the other interstellar components are summarized It is concentrated on observational constraints, both from direct detections of the energetic particles near the earth and from indirect detections by low-frequency radio-continuum and high-energy γ-ray observations, with the emphasis on recent γ-ray results In addition, γ-ray constraints on the molecular hydrogen content of the Galaxy are described The role of cosmic rays among the magnetic-field, gaseous, and stellar components in a possible large-scale hydrostatic equilibrium of the Galaxy is discussed
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Citations
The dynamical state of the interstellar gas and fields. VII.
E. N. Parker
- 01 Dec 1968
TL;DR: In this article, the authors discuss the attractive and disruptive forces in conversion of interstellar gas into stars, discussing self gravitation, galactic magnetic field and cosmic ray pressure, as well as the effects of star formation.
511
The galactic gamma-ray distribution: Implications for galactic structure and the radial cosmic ray gradient
Alice K. Harding,Floyd W. Stecker +1 more
- 01 Nov 1984
TL;DR: The radial distribution of gamma ray emissivity in the Galaxy was derived from flux longitude profiles, using both the final SAS-2 results and the recently corrected COS-B results and analyzing the northern and southern galactic regions separately as discussed by the authors.
14
•Dissertation
Magnetic Field Evolution in Isolated and Interacting Spiral Galaxies
Hanna Kotarba
- 15 Jun 2011
TL;DR: In this article, the existence and evolution of magnetic disks in spiral galaxies is studied with the help of high-resolution state-of-the-art numerical simulations, and the implications of an interaction-driven amplification for the magnetic evolution during the phase of hierarchical structure formation in the Universe are discussed.
11
Cosmic ray antiprotons in closed galaxy model
R. Protheroe
- 01 Jun 1981
TL;DR: The flux of secondary antiprotons expected for the leaky-box model was calculated as well as that for the closed galaxy model of Peters and Westergard (1977).
3
References
A theory of the interstellar medium - Three components regulated by supernova explosions in an inhomogeneous substrate
TL;DR: In this paper, a self-consistent model of the interstellar medium was developed to account for the observed pressure of interstellar clouds, the galactic soft X-ray background, the O VI absorption line observations, the ionization and heating of much of the galaxy, and the motions of the clouds.
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Particle Acceleration by Astrophysical Shocks
TL;DR: In this article, a new mechanism is proposed for acceleration of a power-law distribution of cosmic rays with approximately the observed slope, where high-energy particles in the vicinity of a shock are scattered by Alfven waves carried by the converging fluid flow leading to a first-order acceleration process in which the escape time is automatically comparable to the acceleration time.
2.1K
An introduction to the theory of diffusive shock acceleration of energetic particles in tenuous plasmas
TL;DR: In this article, the central idea of diffusive shock acceleration is presented from microscopic and macroscopic viewpoints; applied to reactionless test particles in a steady plane shock, the mechanism is shown to produce a power law spectrum in momentum with a slope which, to lowest order in the ratio of plasma to particle speed, depends only on the compression in the shock.
1.8K
The relationship between carbon monoxide abundance and visual extinction in interstellar clouds.
TL;DR: In this paper, the relationship of column density to extinction was established, and new determinations for (C-13)O column densities were given for a range of visual extinctions extended to beyond 20 mag.
1.2K