| LDR | | 01945nmm uu200397 4500 |
| 001 | | 000000333900 |
| 005 | | 20240805174741 |
| 008 | | 181129s2018 |||||||||||||||||c||eng d |
| 020 | |
▼a 9780438095311 |
| 035 | |
▼a (MiAaPQ)AAI10826477 |
| 035 | |
▼a (MiAaPQ)columbia:14746 |
| 040 | |
▼a MiAaPQ
▼c MiAaPQ
▼d 248032 |
| 082 | 0 |
▼a 520 |
| 100 | 1 |
▼a Generozov, Aleksey. |
| 245 | 10 |
▼a Stellar and Gas Dynamics in Galactic Nuclei. |
| 260 | |
▼a [S.l.] :
▼b Columbia University.,
▼c 2018 |
| 260 | 1 |
▼a Ann Arbor :
▼b ProQuest Dissertations & Theses,
▼c 2018 |
| 300 | |
▼a 247 p. |
| 500 | |
▼a Source: Dissertation Abstracts International, Volume: 79-11(E), Section: B. |
| 500 | |
▼a Advisers: Brian Metzger |
| 502 | 1 |
▼a Thesis (Ph.D.)--Columbia University, 2018. |
| 520 | |
▼a Galactic nuclei are important for studies of galaxy evolution, stellar dynamics and general relativity. Many have Supermassive Black Holes (SMBHs) (with one million to one billion times the mass of the sun) that affect the large scale properties |
| 520 | |
▼a In Chapters 2 and 3, we develop an analytic model for the gas environment around quiescent SMBHs. In the absence of large scale inflows, winds from the local stellar population will supply most of the gas. The gas density on parsec scales depend |
| 520 | |
▼a In Chapter 4 we construct observationally motivated models for the distributions of stars and stellar remnants in our Galactic Center. We then calculate rates of various collisional stellar interactions, including the tidal capture of stars by s |
| 590 | |
▼a School code: 0054. |
| 650 | 4 |
▼a Astronomy. |
| 690 | |
▼a 0606 |
| 710 | 20 |
▼a Columbia University.
▼b Astronomy. |
| 773 | 0 |
▼t Dissertation Abstracts International
▼g 79-11B(E). |
| 773 | |
▼t Dissertation Abstract International |
| 790 | |
▼a 0054 |
| 791 | |
▼a Ph.D. |
| 792 | |
▼a 2018 |
| 793 | |
▼a English |
| 856 | 40 |
▼u http://www.riss.kr/pdu/ddodLink.do?id=T14998893
▼n KERIS |
| 980 | |
▼a 201812
▼f 2019 |
| 990 | |
▼a 관리자 |