X-ray Study of Low-mass Young Stellar Objects in the ρ Ophiuchi ...

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20 CHAPTER 3. REVIEW OF THE ρ OPHIUCHI CLOUD(footnotes for Table 3.1)* The number of starless cores.† University of Arizona 1.54 m telescope.‡ The number of sources within ∼700 arcmin 2 region of the ρ Oph main body.§ The 123 cm telescope in Cala Alto/Spain and the 50 cm telescope on the Gamsberg in South West Africa. Noobservational information was given in the paper.‖ Relative Hα intensity was only given.# Pointing spectroscopic (3700–7500 Å) and photometric (UBV RI) observations on Einstein X-ray sources (Montmerleet al., 1983).References – (1) André et al. (1987), (2) Stine et al. (1988), (3) Leous et al. (1991), (4) Motte et al. (1998), (5) Johnstoneet al. (2000), (6) Young et al. (1986), (7) Wilking et al. (1989), (8) Bontemps et al. (2001), (9) Grasdalenet al. (1973), (10) Vrba et al. (1975), (11) Elias (1978), (12) Wilking & Lada (1983), (13) Barsony et al. (1989),(14) Greene & Young (1992), (15) Comerón et al. (1993), (16) Strom et al. (1995), (17) Barsony et al. (1997),(18) http://ipac.caltech.edu/2mass/, (19) Chini (1981), (20) Wilking et al. (1987), (21) Bouvier & Appenzeller(1992), (22) Montmerle et al. (1983), (23) Casanova et al. (1995), (24) Grosso et al. (2000), (25) Kamata et al.(1997), (26) This thesis and Imanishi et al. (2003).
Chapter 4InstrumentationIn this chapter, we show the basic properties of the Chandra satellite and its instruments. Moredetails are found in the Chandra Observatory Guide 1 .Fig. 4.1.— Schematic view of the Chandra satellite ( c○NASA/CXC/SAO).4.1 Overview of the Chandra X-ray ObservatoryThe Chandra X-ray Observatory (CXO: Weisskopf et al., 2002, Figure 4.1) was launched by NASA’sSpace Shuttle Columbia on July 23, 1999. The total weight and length are ∼5,000 kg and ∼10 m.The orbit is elliptical with the perigee and apogee altitudes of ∼16,800 km and ∼132,000 km,1 http://asc.harvard.edu/udocs/docs/docs.html .21
Page 3: Contents1 Introduction 12 Review of
Page 9 and 10: List of Figures2.1 The H-R diagram
Page 11 and 12: LIST OF FIGURESix6.17 Light curves
Page 13 and 14: List of Tables3.1 Multiwavelength s
Page 15 and 16: Chapter 1IntroductionStar formation
Page 17 and 18: Chapter 2Review of Low-mass Young S
Page 19 and 20: 2.1. EVOLUTION OF LOW-MASS STARS 5w
Page 21 and 22: 2.2. MOLECULAR CLOUDS 72.2 Molecula
Page 23 and 24: 2.3. X-RAY OBSERVATIONS OF LOW-MASS
Page 25 and 26: 2.3. X-RAY OBSERVATIONS OF LOW-MASS
Page 27: 2.3. X-RAY OBSERVATIONS OF LOW-MASS
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Page 46 and 47: 32 CHAPTER 5. CHANDRA OBSERVATIONS
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94 CHAPTER 6. INDIVIDUAL SOURCESPra
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96 CHAPTER 7. OVERALL FEATURE OF X-
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98 CHAPTER 7. OVERALL FEATURE OF X-
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100 CHAPTER 7. OVERALL FEATURE OF X
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Chapter 8Systematic Study of YSO Fl
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8.2. CORRELATION BETWEEN THE FLARE
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8.3. MAGNETIC RECONNECTION MODEL 11
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8.5. EFFECT OF THE QUIESCENT X-RAYS
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8.6. EVOLUTION OF YSOS AND THEIR FL
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Chapter 9ConclusionWe summarize the
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Appendix AFlare Light CurvesFig. A.
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Fig.A.2 (Continued)121
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Fig. A.4.— Same as Figure A.1, bu
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126 APPENDIX B. PHYSICAL PARAMETERS
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128 APPENDIX B. PHYSICAL PARAMETERS
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Appendix CModeling of the FlareIn t
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C.2. PREDICTED CORRELATIONS BETWEEN
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BibliographyAgeorges, N., Eckart, A
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BIBLIOGRAPHY 137Feigelson, E. D., &
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BIBLIOGRAPHY 139Johnstone, D., Wils
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BIBLIOGRAPHY 141Rutledge, R. E., Ba
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BIBLIOGRAPHY 143Yokoyama, T. & Shib
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