| LDR | | 02021nam u200397 4500 |
| 001 | | 000000422120 |
| 005 | | 20190215165854 |
| 008 | | 181129s2018 |||||||||||||||||c||eng d |
| 020 | |
▼a 9780438095311 |
| 035 | |
▼a (MiAaPQ)AAI10826477 |
| 035 | |
▼a (MiAaPQ)columbia:14746 |
| 040 | |
▼a MiAaPQ
▼c MiAaPQ
▼d 247004 |
| 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
▼z 이 자료의 원문은 한국교육학술정보원에서 제공합니다. |
| 980 | |
▼a 201812
▼f 2019 |
| 990 | |
▼a ***1012033 |