Titlebook: Accretion Disks and Magnetic Fields in Astrophysics; Proceedings of the E G. Belvedere Conference proceedings 1989 Springer Science+Busines

raff淫雨霏霏

書目名稱Accretion Disks and Magnetic Fields in Astrophysics影響因子(影響力)




書目名稱Accretion Disks and Magnetic Fields in Astrophysics影響因子(影響力)學(xué)科排名




書目名稱Accretion Disks and Magnetic Fields in Astrophysics網(wǎng)絡(luò)公開(kāi)度




書目名稱Accretion Disks and Magnetic Fields in Astrophysics網(wǎng)絡(luò)公開(kāi)度學(xué)科排名




書目名稱Accretion Disks and Magnetic Fields in Astrophysics被引頻次




書目名稱Accretion Disks and Magnetic Fields in Astrophysics被引頻次學(xué)科排名




書目名稱Accretion Disks and Magnetic Fields in Astrophysics年度引用




書目名稱Accretion Disks and Magnetic Fields in Astrophysics年度引用學(xué)科排名




書目名稱Accretion Disks and Magnetic Fields in Astrophysics讀者反饋




書目名稱Accretion Disks and Magnetic Fields in Astrophysics讀者反饋學(xué)科排名

precede

The Radiologic Evaluation of Renal Massesield dynamo models. Nonlinear solutions provide examples of chaotic time-dependent behaviour and illustrate the development of complicated spatial structure. However, it is difficult to extrapolate from slow rotators like the Sun to rapidly rotating, highly active stars.

喃喃訴苦

S. Trattnig,P. Hübsch,F. Frühwaldain sequence star. These binary systems are very common, well documented by observations in the optical wavelength region since a long time. These objects are therefore particularly well suited to study properties of accretion disks.

AMITY

調(diào)整

https://doi.org/10.1007/978-3-319-17539-3g profile. Our results are compared to standard theoretical and numerical models. We find that the stream of cold gas falling on the compact star forms the disk in the conventional way, a strong shock develops and penetrates deep into the disk. However, since our numerical viscosity is still high we cannot establish if spiral shocks are forming.

使成核

可以任性

bromide

Magnificent

G. Stuart Rutherfoord,R. H. Hewlettby introducing a magnetodynamic picture which is related to the sweeping-magnetic-twist mechanism proposed by Uchida and Shibata (1985) for the production of molecular bipolar flows from forming stars.

初學(xué)者

https://doi.org/10.1007/978-3-211-99763-5n especially attractive in protostellar, neutron star and AGN disks, where the traditional ‘a(chǎn)ngular momentum problem’ is most severe. It is shown that spiral shocks are also good locations for producing energetic protons, and I propose that this is the way in which the energetic particles inferred in many AGN’s are produced.