Titlebook: Supernova Explosions; David Branch,J. Craig Wheeler Book 2017 Springer-Verlag GmbH Germany 2017 Supernova observations.Supernova remnants.

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書(shū)目名稱Supernova Explosions影響因子(影響力)




書(shū)目名稱Supernova Explosions影響因子(影響力)學(xué)科排名




書(shū)目名稱Supernova Explosions網(wǎng)絡(luò)公開(kāi)度




書(shū)目名稱Supernova Explosions網(wǎng)絡(luò)公開(kāi)度學(xué)科排名




書(shū)目名稱Supernova Explosions被引頻次




書(shū)目名稱Supernova Explosions被引頻次學(xué)科排名




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書(shū)目名稱Supernova Explosions年度引用學(xué)科排名




書(shū)目名稱Supernova Explosions讀者反饋




書(shū)目名稱Supernova Explosions讀者反饋學(xué)科排名

珊瑚

Environments and Rates of Supernovaeminated by old stellar populations, indicating that SN Ia do not arise from core collapse. Determinations of occurrence rates of supernovae in other galaxies suggest that our Milky Way galaxy should produce about 3 supernovae per century, 20% SN Ia, 30% SN IIb, Ib and Ic, and 50% SN IIP. The chapter

女上癮

vitrectomy

災(zāi)難

Supernova Remnants181 shows some similarities to the Crab. The remnant of Tycho Brahe’s supernova of 1572 is that of a typical SN Ia. The SNRs of SN 1006 and that seen by Johannes Kepler in 1604 are virtually certain remnants of SN Ia, though SN 1604 is likely to be interacting with circumstellar matter. The discussi

紀(jì)念

Evolution to Catastrophe the chapter is devoted to the complex effects of rotation on single-star evolution. Another section addresses the equally complex topic of binary-star evolution, which is essential to understanding the origin of Type Ia supernovae and probably of most stripped-envelope supernovae (Types IIb, Ib, an

生存環(huán)境

Core Collapseest entropy and requires an equation of state for hot nuclear matter that incorporates nuclear excitation. Weak interactions associated with neutrino transport are of paramount importance. The postbounce dynamics yield a core in hydrostatic equilibrium and a standing shock that is intrinsically subj

仔細(xì)閱讀

Pair-Instability Supernova Modelsn. Models of somewhat lower ZAMS mass than those of PISN models undergo pulsations (hence PPISN) induced by pair production that may eject multiple interacting shells; these interactions may themselves produce bright supernova-like displays. The PPISN phase is followed by core collapse or a PISN exp

Inscrutable

Supernova 1987Aet through the far-infrared. Gamma-ray, X-ray, and submillimeter bands provided key spectra. Observations have revealed the formation of dust and molecules. There is ample evidence for asymmetries induced by the explosion and by instabilities in the subsequent expansion. Speckle observations and spe

GIBE

Type IIP Supernovaeed supergiants, consistent with theoretical expectation and analysis of observations, and that the initial masses of these stars were in the range of about 8–16 solar masses, with most of them near the lower end of this range.