| LDR | | 02026nam u200397 4500 |
| 001 | | 000000419425 |
| 005 | | 20190215163651 |
| 008 | | 181129s2018 |||||||||||||||||c||eng d |
| 020 | |
▼a 9780438180833 |
| 035 | |
▼a (MiAaPQ)AAI10839516 |
| 035 | |
▼a (MiAaPQ)columbia:14821 |
| 040 | |
▼a MiAaPQ
▼c MiAaPQ
▼d 247004 |
| 082 | 0 |
▼a 520 |
| 100 | 1 |
▼a Zheng, Yong. |
| 245 | 14 |
▼a The Cycle of Gaseous Baryons between the Disk and Halo. |
| 260 | |
▼a [S.l.]:
▼b Columbia University.,
▼c 2018. |
| 260 | 1 |
▼a Ann Arbor:
▼b ProQuest Dissertations & Theses,
▼c 2018. |
| 300 | |
▼a 285 p. |
| 500 | |
▼a Source: Dissertation Abstracts International, Volume: 79-12(E), Section: B. |
| 500 | |
▼a Adviser: Mary E. Putman. |
| 502 | 1 |
▼a Thesis (Ph.D.)--Columbia University, 2018. |
| 520 | |
▼a The gaseous halo surrounding a galaxy disk is often referred to as the circum-galactic medium (CGM). The boundary of the CGM is loosely defined as the virial radius of the galaxy. Recent observations and simulations have shown that the CGM is ma |
| 520 | |
▼a Observations of the MW's CGM are unavoidably contaminated by foreground gas since we reside in the MW's disk. Conventionally, a velocity cut at |upsilonLSR| ~ 100 km s --1 is used as a proxy for distance, with low-velocity (| upsilonLSR| < 100 k |
| 520 | |
▼a I further study how baryons are cycled between the disk and CGM by observing gas accretion in M33. Using HST/COS to observe seven UV-bright stars in M33's disk, I find that there is a layer of metal-enriched inflow moving towards M33 at a rate o |
| 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 79-12B(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=T14999683
▼n KERIS
▼z 이 자료의 원문은 한국교육학술정보원에서 제공합니다. |
| 980 | |
▼a 201812
▼f 2019 |
| 990 | |
▼a ***1012033 |