A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust
Identifieur interne : 000016 ( Istex/Corpus ); précédent : 000015; suivant : 000017A Cosmic-ray Composition Controlled by Volatility and a/q Ratio. snr Shock Acceleration of gas and Dust
Auteurs : Jean-Paul Meyer ; Luke O'C. Drury ; Donald C. EllisonSource :
- Space Science Reviews [ 0038-6308 ] ; 1998.
English descriptors
- Teeft :
- Abundance, Abundance relative, Acceleration efficiency, Apparent correlation, Astron, Astrophys, Binns, Cambridge university press, Cass, Chemical compound, Clue element, Companion paper, Condensation temperature, Conf, Coronal, Coronal composition, Coronal material, Cosmic abundance, Cosmic ray, Datum, Different volatility, Dominant solid compound, Dust grain, Element condensation temperature, Element overabundance, Element relative, Element volatility, Ellison, Energetic particle, Enhancement, Entire grain, Error bar, Excess relative, Ferrando, First ionization potential, Gcrs, Gcrs abundance, Gcrs composition, Gcrs overabundance, Gcrs ratio, General correlation, General pattern, General trend, Grain destruction product, Grain material, Grain silicate, Grevesse, Heavier specie, Heavy element, Higher temperature, Intermediate class, Interstellar circumstellar, Interstellar propagation, Large error, Large spread, Lighter one, Mass dependence, Mass effect, Mass fractionation, Meyer, Monotonic function, More refractory element, More volatile one, Much less, Noble gas, Nucleosynthesis, Nucleosynthesis calculation, Other element, Other hand, Other type, Overabundance, Possible source, Preferential acceleration, Proc, Reames, Refractory, Refractory element, Refractory element relative, Relevant parameter, Same gcrs, Secondary element, Separate site, Shock speed, Shock wave, Show intermediate overabundance, Significant fraction, Single site, Single step, Singular behavior, Slow chemical reprocessing, Solar abundance ratio, Solar composition, Solar corona, Solar energetic particle, Solar value, Solar wind, Solid dot, Solid square, Source abundance, Source abundance relative, Source ratio, Spallation error, Stellar, Systematic error, Time solar, Up limit, Various element, Various type, Vernois, Volatile, Volatile element, Volatile one, Volatility, Waddington, Weak enhancement, Webber, Wind material, World scientific.
Abstract
Abstract: The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).
Url:
DOI: 10.1023/A:1005081721214
Links to Exploration step
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<p>The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).</p>
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<Para>The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).</Para>
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<abstract lang="en">Abstract: The composition of Galactic Cosmic Ray Sources (GCRS) shows the following features: (i) an enhancement of the refractory elements relative to the volatile ones, and (ii) an enhancement of the heavier volatile elements relative to the lighter ones; this mass dependence should reflect a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is only a very weak enhancement of heavier species, or none at all. We consider it fortuitous that the GCRS composition resembles that of the solar corona, which is biased according to first ionization potential. In a companion paper by Ellison et al. (1998, this issue), this GCRS composition is interpreted in terms of a supernova shock wave acceleration of interstellar and/or circumstellar (e.g., 22Ne-rich Wolf-Rayet wind) gas phase and especially dust grain material. These two papers summarize and complement the content of two papers that recently appeared in Astrophys. J. (Meyer et al., 1997; Ellison et al., 1997).</abstract>
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