Titlebook: Astrophysical Sources of High Energy Particles and Radiation; Maurice M. Shapiro,Todor Stanev,John P. Wefel Book 2001 Springer Science+Bus

SCOWL

書目名稱Astrophysical Sources of High Energy Particles and Radiation影響因子(影響力)




書目名稱Astrophysical Sources of High Energy Particles and Radiation影響因子(影響力)學(xué)科排名




書目名稱Astrophysical Sources of High Energy Particles and Radiation網(wǎng)絡(luò)公開度




書目名稱Astrophysical Sources of High Energy Particles and Radiation網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Astrophysical Sources of High Energy Particles and Radiation被引頻次




書目名稱Astrophysical Sources of High Energy Particles and Radiation被引頻次學(xué)科排名




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書目名稱Astrophysical Sources of High Energy Particles and Radiation年度引用學(xué)科排名




書目名稱Astrophysical Sources of High Energy Particles and Radiation讀者反饋




書目名稱Astrophysical Sources of High Energy Particles and Radiation讀者反饋學(xué)科排名

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https://doi.org/10.1007/978-1-4302-0103-8nduced γ-ray flux from SNR at least on an order of magnitude, that allows to adjust the theoretical π° decay γ-luminosities with observed fluxes at least for a few SNRs even for low density (no ~ 10. -4- 10. cm.) cloud.

Crumple

https://doi.org/10.1007/978-1-4302-0103-8the characteristic decay time, ..: ~ 10. ≥ .. > 10. yrs, can be excluded assuming the standard initial magnetic momentum, μo =10.Gcm., if accreting INSs are observed. For these parameters an INS would never reach the stage of accretion from the interstellar medium even for a low space velocity of th

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Forward Kinematics: Making Things Walkthe direction, the source could be identified and the afterglow of the burst at these longer wavelengths could be observed continuously, upto several weeks after the burst. Detailed measurements in the 7-ray window were made with the BATSE instrument aboard the . — we will review these before descri

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Forward Kinematics: Making Things Walks of solar FEP (especially in periods of very great events) [12–14, 15]. 3.- by properties of solar FEP interaction with solar wind matter accompanied with GR generation through decay of neutral pions [16–18].

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Complement

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Dark Matter Halo of Our Galaxy cluster has to be in some unseen form to account for the large observed value of the velocity dispersion[2]. This work was followed up by a few other workers and finally in 1972 based on observations of the velocities of hundreds of galaxies in the cluster, Rood et al., confirmed that atleast 75 %

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