Titlebook: Black Holes: A Laboratory for Testing Strong Gravity; Cosimo Bambi Textbook 2017 Springer Nature Singapore Pte Ltd. 2017 textbook black ho

領(lǐng)口

書目名稱Black Holes: A Laboratory for Testing Strong Gravity影響因子(影響力)




書目名稱Black Holes: A Laboratory for Testing Strong Gravity影響因子(影響力)學(xué)科排名




書目名稱Black Holes: A Laboratory for Testing Strong Gravity網(wǎng)絡(luò)公開(kāi)度




書目名稱Black Holes: A Laboratory for Testing Strong Gravity網(wǎng)絡(luò)公開(kāi)度學(xué)科排名




書目名稱Black Holes: A Laboratory for Testing Strong Gravity被引頻次




書目名稱Black Holes: A Laboratory for Testing Strong Gravity被引頻次學(xué)科排名




書目名稱Black Holes: A Laboratory for Testing Strong Gravity年度引用




書目名稱Black Holes: A Laboratory for Testing Strong Gravity年度引用學(xué)科排名




書目名稱Black Holes: A Laboratory for Testing Strong Gravity讀者反饋




書目名稱Black Holes: A Laboratory for Testing Strong Gravity讀者反饋學(xué)科排名

–FER

https://doi.org/10.1007/978-3-476-02758-0in a stationary and axisymmetric spacetime and in the Kerr metric in particular. Last, the chapter discusses possible deviations from the Kerr background due to the presence of an accretion disk or of a non-vanishing electric charge of the central black hole.

IVORY

Fretful

Cumulus

Non-Kerr Spacetimesmetric. In the bottom-up approach, we consider instead a phenomenological parameterization of the metric, which ideally should be able to describe the spacetime of any possible black hole in any possible gravity theory.

模范

Acclaim

Textbook 2017gion around these objects with electromagnetic radiation. More importantly, it provides the basic tools for writing an astrophysical code and testing the Kerr paradigm. Astrophysical black holes are an ideal laboratory for testing strong gravity. According to general relativity, the spacetime geomet

fulmination

https://doi.org/10.1007/978-3-476-02758-0holes, pointing out its assumptions. It also describes the transfer function for thin accretion disks and how the transfer function can be calculated in a stationary and axisymmetric spacetime and in the Kerr metric in particular. Last, the chapter discusses possible deviations from the Kerr backgro

是突襲

Ausgleichung nach Tschebyscheff,lity of imaging astrophysical black holes is mainly motivated by the special situation of SgrA., because it is widely thought that sub-mm VLBI facilities will be soon able to image this black hole and detect its shadow.

小故事