Titlebook: Stellar Astrophysics; A Tribute to Helmut K. S. Cheng,K. C. Leung,T. P. Li Conference proceedings 2003 Springer Science+Business Media Dor

Jejunum

書目名稱Stellar Astrophysics影響因子(影響力)




書目名稱Stellar Astrophysics影響因子(影響力)學(xué)科排名




書目名稱Stellar Astrophysics網(wǎng)絡(luò)公開度




書目名稱Stellar Astrophysics網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Stellar Astrophysics被引頻次




書目名稱Stellar Astrophysics被引頻次學(xué)科排名




書目名稱Stellar Astrophysics年度引用




書目名稱Stellar Astrophysics年度引用學(xué)科排名




書目名稱Stellar Astrophysics讀者反饋




書目名稱Stellar Astrophysics讀者反饋學(xué)科排名

學(xué)術(shù)討論會(huì)

Gamma-Ray Pulsars in Gould Belt and Unidentified Gamma-Ray Sources in Medium Latitudes can exist even their age > 10. yr old. We use Monte Carlo techniques to simulate the statistical properties of rotation-powered pulsars in the Gould Belt. If the pulsar birth rate in Gould Belt is 3 × 10..., the gamma-ray pulsars in this region, which can be detected by EGRET, will must be dominate

misanthrope

Magnetars and Pulsars: A Missing Link fields, i.e., magnetars, marking them a distinguished species from the conventional species of spindown-powered isolated neutron stars, i.e., radio pulsars. The current arguments in favor of the magnetar interpretation of SGR/AXP phenomenology will be outlined, and the two energy sources in magneta

西瓜

流利圓滑

假裝是我

Inflated

PURG

Phase Transition in Rotating Hybrid Starsmoment of inertia, and even results in an era of spin-up of the pulsar (Glendenning, Pei, & Weber 1997, hereafter GPW) . We have found that the equation of states of the crust of neutron star and the accuracy of the numerical models which can be used to determinate the stellar rotating properties ar

Lipohypertrophy

Accretion Disk Oscillations and QPOs in X-Ray Binariesation modes in a relativistic accretion disk. Here we studied the non-damping feature of some oscillation modes by considering the radial perturbations and viscosity effects. We found that the non-damping fundamental modes can be amplified significantly in the inner disk when the viscosity parameter

charisma

Bare Strange Quark Stars: Formation and Emissionmperature after the supernova detonation flame, and a crust can also hardly form except for a super-Eddington accretion. The magnetosphere of a bare strange star is composed mainly of e. pair plasma, where both inner and outer vacuum gaps work for radio as well as high energy nonthermal emission. A