標(biāo)題: Titlebook: Astrophysical Sources of High Energy Particles and Radiation; Maurice M. Shapiro,Todor Stanev,John P. Wefel Book 2001 Springer Science+Bus [打印本頁] 作者: SCOWL 時(shí)間: 2025-3-21 18:13
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
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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
作者: A精確的 時(shí)間: 2025-3-21 21:07 作者: hallow 時(shí)間: 2025-3-22 02:55
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.作者: Crumple 時(shí)間: 2025-3-22 06:55
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作者: Type-1-Diabetes 時(shí)間: 2025-3-22 09:19
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作者: CHAR 時(shí)間: 2025-3-22 14:55
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].作者: RACE 時(shí)間: 2025-3-22 19:36 作者: Complement 時(shí)間: 2025-3-22 23:42 作者: 濃縮 時(shí)間: 2025-3-23 01:47
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 % 作者: BOOST 時(shí)間: 2025-3-23 09:12 作者: CRUDE 時(shí)間: 2025-3-23 09:59 作者: Anonymous 時(shí)間: 2025-3-23 16:18 作者: Cytokines 時(shí)間: 2025-3-23 18:38
Variable Gamma Ray Sources, 1: Interactions of Flare Energetic Particles with Solar and Stellar Winds 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].作者: 留戀 時(shí)間: 2025-3-23 23:05 作者: 煩憂 時(shí)間: 2025-3-24 03:32
Astrophysical Sources of High Energy Particles and Radiation978-94-010-0560-9Series ISSN 1568-2609 作者: Permanent 時(shí)間: 2025-3-24 09:14 作者: 突變 時(shí)間: 2025-3-24 12:01 作者: AV-node 時(shí)間: 2025-3-24 16:40 作者: FLIP 時(shí)間: 2025-3-24 21:32
Correlation and ClusteringIn this lecture we clarify the basic difference between the correlation properties for systems characterized by small or large fluctuations. The concepts of correlation length, homogeneity scale, scale invariance and criticality are discussed as well. We relate these concepts to the interpretation of galaxy clsutering.作者: 忍受 時(shí)間: 2025-3-24 23:25
https://doi.org/10.1007/978-1-4302-0103-8 rays (CRs) originates in supernova remnants (SNRs). Theoretically progress in the solution of this problem has been due to the development of the theory of diffusive shock acceleration (see, for example, reviews [1–3]). Although still incomplete, the theory is able to explain the main characteristi作者: allergen 時(shí)間: 2025-3-25 06:39
Two-way ASP.NET/Flash Communication,different values of proton-proton cross sections are used. New results obtained recently in accelerator experiments lead to the necessity of revising some of them. In this paper, we show some results obtained in a framework of a so-called geometrical model. A particular proton profile function and i作者: hematuria 時(shí)間: 2025-3-25 08:23 作者: 英寸 時(shí)間: 2025-3-25 12:15 作者: Bricklayer 時(shí)間: 2025-3-25 16:58 作者: MAOIS 時(shí)間: 2025-3-25 22:45 作者: 雪白 時(shí)間: 2025-3-26 02:44 作者: Between 時(shí)間: 2025-3-26 04:48
https://doi.org/10.1007/978-1-4302-0103-8lectrons are accelerated on SNR shocks up to the energy ~ 10. eV. We have no direct observational confirmations about proton acceleration by SNR. Different models of γ-emission from SNRs predict different emission mechanisms as dominating. Only π° decays created in proton-nucleon interactions allow 作者: 聲音刺耳 時(shí)間: 2025-3-26 11:32
https://doi.org/10.1007/978-1-4302-0103-8scuss stochastic period evolution of INSs. We briefly discuss how an INS’s spin period evolves under influence of interaction with turbulized interstellar medium..To investigate statistical properties of the INS population we calculate a . of INSs in our Galaxy. We infer a lower bound for the mean k作者: 我不明白 時(shí)間: 2025-3-26 15:30
https://doi.org/10.1007/978-1-4302-0103-8utburst amounted to ~ 1.4 * 10. erg/sec, the same order of magnitudes as the luminosity of the ’giant’ X-ray outburst of the system. Probably, the flashes were even more powerful and more transient. These superfast and superpower processes could arise in the transient accretion disk of the pulsar wi作者: resilience 時(shí)間: 2025-3-26 17:50
Two-way ASP.NET/Flash Communication,many attempts to explain them I focus here on the by now classical suggestion, that they come from powerful radio galaxies. In this review I will embed the discussion into a general framework of hadronic particle acceleration in Active galactic Nuclei.作者: 失誤 時(shí)間: 2025-3-27 00:13
https://doi.org/10.1007/978-1-4302-0103-8 formed, and how they are related to the central massive black hole (BH) and its accompanying accretion flow. Understanding this coupling, as well as the overall system energetics, is not possible without knowing the jet content (i.e., pure leptonic or hadronic). Unfortunately, this is still a matte作者: 6Applepolish 時(shí)間: 2025-3-27 04:30 作者: 固定某物 時(shí)間: 2025-3-27 06:16 作者: BUOY 時(shí)間: 2025-3-27 11:17
Forward Kinematics: Making Things Walkased instruments have shown that the universe is full of gamma-ray sources accessible to measurements. For the first time in history, present technological developments make possible to open a new window to the study of the universe in the GeV-TeV energy range. Very sensitive detectors to be launche作者: apiary 時(shí)間: 2025-3-27 15:51 作者: Mast-Cell 時(shí)間: 2025-3-27 18:33 作者: aerial 時(shí)間: 2025-3-28 00:10
Forward Kinematics: Making Things Walkwill give a development of this research with much more details. As example, we will consider in the first the situation with GR generation in the interplanetary space by solar FEP in periods of great events, determined mainly by 3 factors: 1.- by space-time distribution of solar FEP in the Heliosph作者: 范例 時(shí)間: 2025-3-28 02:27 作者: 軍械庫 時(shí)間: 2025-3-28 08:12
978-1-4020-0174-1Springer Science+Business Media Dordrecht 2001作者: CANT 時(shí)間: 2025-3-28 13:33 作者: 極少 時(shí)間: 2025-3-28 16:12
Galactic Clues About the High-Energy Processes in BL Lac (AGN) Jets formed, and how they are related to the central massive black hole (BH) and its accompanying accretion flow. Understanding this coupling, as well as the overall system energetics, is not possible without knowing the jet content (i.e., pure leptonic or hadronic). Unfortunately, this is still a matter of significant debate in the community.作者: ARBOR 時(shí)間: 2025-3-28 19:15
Theory of Cosmic Ray and High-Energy Gamma-Ray Production in Supernova Remnants rays (CRs) originates in supernova remnants (SNRs). Theoretically progress in the solution of this problem has been due to the development of the theory of diffusive shock acceleration (see, for example, reviews [1–3]). Although still incomplete, the theory is able to explain the main characteristi作者: FIN 時(shí)間: 2025-3-29 00:33 作者: 鉗子 時(shí)間: 2025-3-29 06:28
Electron Acceleration by Quasi-Parallel Shock Wavestabilities induced by protons in the transition region inside the shock plays the main role in the electron heating and their injection to the first order Fermi acceleration mechanism. The electron distribution function in the vicinity of the shock front can be calculated in our model. The model is 作者: 經(jīng)典 時(shí)間: 2025-3-29 09:02 作者: Ledger 時(shí)間: 2025-3-29 11:55
Supernovae, Superbubbles, Nonthermal Emission & Light Element Nucleosynthesis in the Galaxy with molecular clouds, superbubbles created by massive starformation regions, and high-velocity clouds. We discuss hard continuum and the 511 keV annihilation line emission from that objects. Multiwavelength spectra of extended and compact sources are used to constrain the nonthermal particle gener作者: airborne 時(shí)間: 2025-3-29 18:03
Cosmic Ray Interactions in the Galactic Center RegionIt is usually assumed that these gamma-rays arise from the interactions of cosmic ray nuclei with ambient matter. Cosmic Ray particles have been observed up to 310. eV, with many arguments suggesting, that up to about 3 10. eV they are of Galactic origin. Cosmic ray particles get injected by their s作者: LATE 時(shí)間: 2025-3-29 22:19
Dark Matter Halo of Our Galaxyd cosmology on the one hand and with nuclear and particle physics on the other. Dark matter particles are the only relicts that still servive to-day from epochs prior to the primordial helium synthesis which took place at about 400s after the big bang. The first clues pointing to the presence of hid作者: 編輯才信任 時(shí)間: 2025-3-30 03:08
A New Model for the Thermal X-Ray Composites and the Proton Origin γ-Rays from Supernova Remnantslectrons are accelerated on SNR shocks up to the energy ~ 10. eV. We have no direct observational confirmations about proton acceleration by SNR. Different models of γ-emission from SNRs predict different emission mechanisms as dominating. Only π° decays created in proton-nucleon interactions allow 作者: Extemporize 時(shí)間: 2025-3-30 06:28 作者: Iniquitous 時(shí)間: 2025-3-30 09:32
High Energy Outburst of Recurrent Transient Pulsar A0535+26utburst amounted to ~ 1.4 * 10. erg/sec, the same order of magnitudes as the luminosity of the ’giant’ X-ray outburst of the system. Probably, the flashes were even more powerful and more transient. These superfast and superpower processes could arise in the transient accretion disk of the pulsar wi作者: GOUGE 時(shí)間: 2025-3-30 16:05
High Energy Particles in Active Galactic Nucleimany attempts to explain them I focus here on the by now classical suggestion, that they come from powerful radio galaxies. In this review I will embed the discussion into a general framework of hadronic particle acceleration in Active galactic Nuclei.作者: 顯微鏡 時(shí)間: 2025-3-30 17:51
Galactic Clues About the High-Energy Processes in BL Lac (AGN) Jets formed, and how they are related to the central massive black hole (BH) and its accompanying accretion flow. Understanding this coupling, as well as the overall system energetics, is not possible without knowing the jet content (i.e., pure leptonic or hadronic). Unfortunately, this is still a matte作者: cuticle 時(shí)間: 2025-3-31 00:40 作者: erythema 時(shí)間: 2025-3-31 02:30
The Sunyaev-Zeldovich Effect and its Cosmological Significancestrophysical and cosmological significance. In recent years observations of the effect have improved tremendously; high signal-to-noise images of the effect (at low microwave frequencies) can now be obtained by ground-based interferometric arrays. In the near future, high frequency measurements of t作者: 佛刊 時(shí)間: 2025-3-31 05:19
An Overview on GeV-TeV Gamma Ray Astronomy: Past-Present-Futureased instruments have shown that the universe is full of gamma-ray sources accessible to measurements. For the first time in history, present technological developments make possible to open a new window to the study of the universe in the GeV-TeV energy range. Very sensitive detectors to be launche作者: TOM 時(shí)間: 2025-3-31 10:38
A Brief Introduction to the Study of Afterglows of Gamma Ray Burstsiscovered in the late 1960’s by American satellites (.) serendipitously. In the last 30 odd years since their discovery more than 3000 papers have been written about them (including my own unpublished work with Richard Lingenfelter even before the formal discovery) and yet it is only in the last few作者: 相容 時(shí)間: 2025-3-31 15:38 作者: Malfunction 時(shí)間: 2025-3-31 19:20 作者: 樣式 時(shí)間: 2025-4-1 01:38
Book 2001s is on physics / astrophysics andexperimental / observational techniques, scientific implications ofcurrent results, and prospects for future advances. The fieldssurveyed are in rapid development and the exploration of our highenergy universe is proceeding rapidly, with exciting new discoveries.Wha作者: Frenetic 時(shí)間: 2025-4-1 04:45 作者: 巧思 時(shí)間: 2025-4-1 08:30 作者: AWL 時(shí)間: 2025-4-1 10:58
Book 2001t unifies much of the new data is the idea of particle accelerationto enormous energies and the subsequent interactions of the particleswith the local medium. It this focus that makes the book both timelyand an important contribution to the field.作者: 忘恩負(fù)義的人 時(shí)間: 2025-4-1 16:41 作者: Aura231 時(shí)間: 2025-4-1 20:10
1568-2609 ic emphasis is on physics / astrophysics andexperimental / observational techniques, scientific implications ofcurrent results, and prospects for future advances. The fieldssurveyed are in rapid development and the exploration of our highenergy universe is proceeding rapidly, with exciting new disco
