The structure and stability of shock waves in a multiphase interstellar medium

1974 ◽  
Vol 193 ◽  
pp. 561 ◽  
Author(s):  
S. L. Mufson
Keyword(s):  
Shock Waves ◽  
Interstellar Medium ◽  
Structure And Stability

On the model of the solar wind-interstellar medium interaction with two shock waves

1976 ◽  
Vol 41 (2) ◽  
pp. 481-490 ◽  
Author(s):  
V. B. Baranov ◽  
K. V. Krasnobaev ◽  
M. S. Ruderman
Keyword(s):  
Solar Wind ◽  
Shock Waves ◽  
Interstellar Medium

scholarly journals The evolution of dust in the local and high-redshift universe

2015 ◽  
Vol 11 (A29B) ◽  
pp. 182-183
Author(s):  
Eli Dwek ◽  
Richard G. Arendt ◽  
Johannes Staguhn ◽  
Tea Temim
Keyword(s):  
Shock Waves ◽  
Interstellar Medium ◽  
Size Distribution ◽  
High Redshift ◽  
Magellanic Clouds ◽  
Core Collapse ◽  
Agb Stars ◽  
Dust Production ◽  
Great Debate ◽  
High Redshift Universe

AbstractDust is a ubiquities component of the interstellar medium (ISM) of galaxies, and manifests itself in many different ways. Yet, its origin, composition, and size distribution are still a matter of great debate. Most of the thermally condensed dust is produced in the explosively expelled ejecta of core collapse supernovae (CCSNe) and in the quiescent winds of AGB stars. Following its injection into the ISM it is destroyed by supernova (SN) shock waves. Knowing the relative rates of these processes is crucial for understanding the nature and evolution of dust in galaxies. In the following we will review three aspects of the evolution of dust in galaxies: the evolution of dust in the ejecta of SN1987A; the rates of dust production and destruction rates in the Magellanic Clouds (MCs), and the evolution of dust in CLASH 2882, a gravitationally-lensed galaxy at z=1.

scholarly journals Cosmic-Ray Injection into Shock-Waves

1981 ◽  
Vol 94 ◽  
pp. 361-362 ◽  
Author(s):  
Catherine J. Cesarsky ◽  
Jean-Pierre Bibring
Keyword(s):  
Cosmic Rays ◽  
Shock Waves ◽  
Interstellar Medium ◽  
Ionization Potential ◽  
Absorption Line ◽  
Cosmic Ray ◽  
Galactic Cosmic Rays ◽  
Reactive Elements ◽  
Refractory Elements ◽  
First Ionization Potential

When corrected for the effects of propagation in the interstellar medium (i.s.m.), the observed composition of galactic cosmic rays can give us some clues as to the origin of these particles. It is noteworthy that the main pecularities of the cosmic ray source composition (CRS), as compared to normal i.s.m. abundances, bear some resemblance to that of i.s. grains, as inferred from i.s. absorption line measurements (e.g. York 1976): (1) the refractory elements Al, Si, Mg, Ni, Fe and Ca, which in i.s. clouds are almost completely locked into grains, are present with normal abundance ratios in the CRS. (2) normalized to Si, the volatile and reactive elements C, N, O, S and Zn are underabundant in CRS by factors of 2.5 to 6; these elements are only partially depleted in the i.s.m. (3) at a given rigidity the ratios H/Si and He/Si are lower than in the i.s.m. by a factor of ~ 25; while H and He atoms are virtually absent in i.s. grains. (1) implies that cosmic rays originate in astrophysical sites where the grains have either not condensated as yet, or where they have been (at least partially) destroyed. Then, to account for (2) and (3), one might consider that an unspecified mechanism selects the particles to be accelerated, possibly according to their first ionization potential (Cassé 1979 and references there-in).

scholarly journals The cycling of carbon into and out of dust

2014 ◽  
Vol 168 ◽  
pp. 313-326 ◽  
Author(s):  
Anthony P. Jones ◽  
Nathalie Ysard ◽  
Melanie Köhler ◽  
Lapo Fanciullo ◽  
Marco Bocchio ◽  
...  
Keyword(s):  
Optical Properties ◽  
Cosmic Rays ◽  
Shock Waves ◽  
Interstellar Medium ◽  
Gas Phase ◽  
Molecular Clouds ◽  
Observational Evidence ◽  
Electron Collisions ◽  
Uv Photons ◽  
Dust Evolution

Observational evidence seems to indicate that the depletion of interstellar carbon into dust shows rather wide variations and that carbon undergoes rather rapid recycling in the interstellar medium (ISM). Small hydrocarbon grains are processed in photo-dissociation regions by UV photons, by ion and electron collisions in interstellar shock waves and by cosmic rays. A significant fraction of hydrocarbon dust must therefore be re-formed by accretion in the dense, molecular ISM. A new dust model (Jones et al., Astron. Astrophys., 2013, 558, A62) shows that variations in the dust observables in the diffuse interstellar medium (nH ≤ 103 cm−3), can be explained by systematic and environmentally-driven changes in the small hydrocarbon grain population. Here we explore the consequences of gas-phase carbon accretion onto the surfaces of grains in the transition regions between the diffuse ISM and molecular clouds (e.g., Jones, Astron. Astrophys., 2013, 555, A39). We find that significant carbonaceous dust re-processing and/or mantle accretion can occur in the outer regions of molecular clouds and that this dust will have significantly different optical properties from the dust in the adjacent diffuse ISM. We conclude that the (re-)processing and cycling of carbon into and out of dust is perhaps the key to advancing our understanding of dust evolution in the ISM.

Ion reflection by shock waves and pulse generation by cross-field ion beams

2017 ◽  
Vol 83 (1) ◽  
Author(s):  
Yukiharu Ohsawa
Keyword(s):  
Magnetic Field ◽  
Shock Waves ◽  
Interstellar Medium ◽  
Spatial Scales ◽  
Ion Beams ◽  
Pulse Generation ◽  
The Other ◽  
Shock Formation ◽  
Density Control ◽  
Particle Simulations

Comparisons are made of two different particle simulations: one for the study of plasma-based accelerators (Gueroult & Fisch, Phys. Plasmas, vol. 23, 2016, 032113) and the other for the study of shock formation in the interstellar medium (Yamauchi & Ohsawa, Phys. Plasmas, vol. 14, 2007, 053110). In the former, shock waves used for plasma density control create ion beams by reflection. In the latter, a fast and dense beam of exploding ions penetrates a surrounding plasma. In both simulations, magnetic bumps are generated from the motion of ion beams perpendicular to a magnetic field. Despite the apparent differences of their purposes, configurations and spatial scales, the two simulations show strong similarities in the generation processes and effects of the bumps, suggesting that these are not rare plasma phenomena. The bump created by the exploding ions develops into backward and forward magnetosonic pulses.

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