원자외선 관측을 통한 Loop I Superbubble 에서의 hot gas 특성 = Properties of the hot gas in Loop I superbubble as observed by far-ultraviolet telescopes

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dc.contributor.advisorMin, Kyoung-Wook-
dc.contributor.advisor민경욱-
dc.contributor.authorPark, Jae-Woo-
dc.contributor.author박재우-
dc.date.accessioned2011-12-14T07:28:17Z-
dc.date.available2011-12-14T07:28:17Z-
dc.date.issued2009-
dc.identifier.urihttp://library.kaist.ac.kr/search/detail/view.do?bibCtrlNo=309044&flag=dissertation-
dc.identifier.urihttp://hdl.handle.net/10203/47623-
dc.description학위논문(박사) - 한국과학기술원 : 물리학과, 2009.2, [ x, 103 p. ]-
dc.description.abstractA superbubble is generally produced by collective stellar winds and several consecutive supernova events, which produce a large amount of energy ($10^{52-53}$ ergs) in an interstellar medium. The hot gas induced in this process loses its energy through radiative cooling, dominant far-ultraviolet (FUV) emission, and interaction with a cooler ambient. In this thesis, we focus on the FUV properties of two well-known superbubbles, Loop I (L1) and Orion Eridanus (OES). A spectral image of L1 made with C IV emission shows a shell-like feature collocated with the X-ray NPS. This is located just inside the L1 radio ridges. The result is in good agreement with a model of recent supernova explosion in an inhomogeneous medium, possibly disturbed by previous multiple supernova explosions. For comparison, we also briefly discuss the FUV emission properties in OES. The spatial variations in the FUV line show a peak at the bubble edge around the arc B. This enhancement region indicates the thermal interface where the hot gas inside the bubble can interact with the cooler ambient at that position. Further analysis of the shock with the line flux and ratio shows that the edge may indicates a quiescent thermal interface. Together with the emission map, the C IV and Si IV absorption lines reinforce the physical origin of these two interesting objects. For example, the broad line widths towards the L1 targets seem to indicate the existence of turbulent mixing of the hot gas in this region. The observed ratio of N(C IV)/N(Si IV) supports the turbulent nature of the ISM toward inner part of L1. Conversely, the line widths are narrower for the OES targets by a factor of 2 or more compared with those of the L1 targets and N(C IV)/N(Si IV) is also lower, indicating that the hot gas of OES is produced by much less turbulent mechanisms. The turbulent nature of L1, which is expected from the absorption results can lead to the following conclusion: Because L1 is the place where a super...eng
dc.languageeng-
dc.publisher한국과학기술원-
dc.subjectFar Ultraviolet-
dc.subjectSuperbubble-
dc.subjectSupernova Remnant-
dc.subjectLoop 1-
dc.subjectSTSAT-1-
dc.subject원자외선-
dc.subject슈퍼버블-
dc.subject초신성 잔해-
dc.subject루프 1-
dc.subject과학기술위성 1호-
dc.title원자외선 관측을 통한 Loop I Superbubble 에서의 hot gas 특성 = Properties of the hot gas in Loop I superbubble as observed by far-ultraviolet telescopes-
dc.typeThesis(Ph.D)-
dc.identifier.CNRN309044/325007 -
dc.description.department한국과학기술원 : 물리학과, -
dc.identifier.uid020055068-
dc.contributor.localauthorPark, Jae-Woo-
dc.contributor.localauthor박재우-
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PH-Theses_Ph.D.(박사논문)
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