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

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60 CHAPTER 6. INDIVIDUAL SOURCESrespectively (Inoue, 1985). If we regard that most of the observed column density (5.2×10 22 cm −2 )originates from the circumstellar matter and use the iron abundance of 0.3 solar, we predict themaximum equivalent width to be ∼15 eV, which is significantly lower than the observed value of∼200 eV. We therefore require non-spherical geometry; a larger amount of matter should be presentout of the line-of-sight. A possible scenario is that YLW16A has a face-on geometry (Sekimoto etal., 1997) and the disk is responsible for the fluorescent 6.4 keV line. Since we see no time delay(reflection timescale) with 10 4 s between the flare on-set and 6.4 keV iron line appearance, thedistance of the star and the reflecting region should be less than 20 AU, which is typical of thedistance between the stellar surface and the inner edge of the disk (Feigelson & Montmerle, 1999).Fig. 6.2.— (left): (top) Light curve of BF-64 = YLW16A and (middle and bottom) time profile ofthe best-fit temperature and the emission measure. (right): Spectrum of YLW16A in phases 7–9.The upper panel shows data points (crosses) and the best-fit model (solid line), while the lowerpanel shows residuals from the best-fit model. Line structure exists at ∼6.4 keV and ∼6.7 keV.
6.1. PROTOSTARS 61Table 6.1: Best-fit parameters of BF64 = YLW16APhase * kT log(EM) N H†EW ‡ Flux § L X‖(keV) (cm −3 ) (10 22 cm −2 ) (eV)1 . . . . . 3.2(2.3–4.8) 53.3(53.1–53.4) 5.2(5.0–5.4)
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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
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Chapter 2Review of Low-mass Young S
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2.1. EVOLUTION OF LOW-MASS STARS 5w
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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
Page 30 and 31: 16 CHAPTER 3. REVIEW OF THE ρ OPHI
Page 36 and 37: 22 CHAPTER 4. INSTRUMENTATIONrespec
Page 38 and 39: 24 CHAPTER 4. INSTRUMENTATIONangle
Page 40 and 41: 26 CHAPTER 4. INSTRUMENTATIONThe AC
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Page 44 and 45: 30 CHAPTER 4. INSTRUMENTATIONTable
Page 46 and 47: 32 CHAPTER 5. CHANDRA OBSERVATIONS
Page 72 and 73: 58 CHAPTER 6. INDIVIDUAL SOURCEShig
Page 76 and 77: 62 CHAPTER 6. INDIVIDUAL SOURCES6.2
Page 78 and 79: 64 CHAPTER 6. INDIVIDUAL SOURCESfla
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Page 110 and 111: 96 CHAPTER 7. OVERALL FEATURE OF X-
Page 112 and 113: 98 CHAPTER 7. OVERALL FEATURE OF X-
Page 114 and 115: 100 CHAPTER 7. OVERALL FEATURE OF X
Page 121 and 122: Chapter 8Systematic Study of YSO Fl
Page 123 and 124: 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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