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

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76 CHAPTER 6. INDIVIDUAL SOURCESoccultation. However, its detailed physical condition is still in discussion. More details about S1are discussed in Hamaguchi et al. (2002).Table 6.4: Best-fit parameters of S1Model * < kT > /Γ †‡ Abundance † † N † H E †§ edge τ †‖ < L X > # χ 2 /d.o.f.(keV/–) (solar) (10 53 cm −3 ) (10 22 cm −2 ) (keV)– obs-A –Mekal(Q) 1.9 0.20 ** 2.6 2.2 ** · · · · · · 2.2 138.6/126(1.7–2.1) (0.05–0.39) (2.2–3.2) (2.1–2.4)(F) 2.7 · · · 2.3 · · · · · · · · · 2.3 · · ·(2.1–3.0) (1.9–2.9)Mekal*Edge(Q) 2.2 0.16 ** 2.3 2.1 ** 3.9 ** 0.47 ** 2.0 126.8/124(2.1–2.4) (0.03–0.33) (2.2–2.3) (2.0–2.2) (3.8–4.0) (0.29–0.66)(F) 3.4 · · · 2.0 · · · · · · · · · 2.3 · · ·(2.9–4.1) (1.9–2.3)Power(Q) 3.3 ** · · · · · · 2.8 ** · · · · · · 5.8 142.2/128(3.1–3.5) (2.6–3.0)(F) · · · · · · · · · · · · · · · · · · 6.6 · · ·Power*Edge(Q) 2.9 ** · · · · · · 2.6 ** 3.9 ** 0.56 ** 4.1 127.3/126(2.6–3.0) (2.2–2.7) (3.8–4.1) (0.37–0.76)(F) · · · · · · · · · · · · · · · · · · 4.8 · · ·– obs-BF –Mekal 1.6 0.0 4.1 1.9 · · · · · · 2.6 117.6/105(1.5–1.9) (
6.3. OTHER T TAURI STARS 77quasi-periodic flares from YLW15A (Tsuboi et al., 2000). We hence make and fit the time slicedspectra of A-79 as shown in Figure 6.14, however no significant sign of increase of kT is found atthe second flare but it keeps almost constant of 3–4 keV (phases 3–5 in Figure 6.14), which is asharp contrast to the case of YLW15A (Figure 2 in Tsuboi et al., 2000).6.3.7 BF-10 – WL22The X-ray spectrum of a class II BF-10 = WL22 exhibitsclear line structure at ∼3.2 and ∼3.9 keV (Figure 6.15).The line energies correspond to He-like Ca and Ar. Wehence relax the abundances of these elements to be freeand fit it by the MEKAL model. The best-fit < kT >and N H are 2.1 keV and 12×10 22 cm −2 , respectively (Table5.2), while the abundances of Ar and Ca are 2.7 +8.3−2.7and 5.0 +7.9−4.1 solar. Thus Ca is extremely overabundant,although the mechanism is an open question.Fig. 6.15.— Spectrum of BF10 = WL22. Theupper panel shows data points (crosses) and thebest-fit MEKAL model (solid line), while thelower panel shows residuals from the best-fitmodel. The line structure at ∼3.2 keV and ∼3.9keV is due to He-like Ar and Ca.Fig. 6.14.— (top) Light curve and(middle and bottom) time evolution ofkT and EM of A-79 = GY195.
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Contents1 Introduction 12 Review of
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List of Figures2.1 The H-R diagram
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LIST OF FIGURESix6.17 Light curves
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List of Tables3.1 Multiwavelength s
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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
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2.3. X-RAY OBSERVATIONS OF LOW-MASS
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16 CHAPTER 3. REVIEW OF THE ρ OPHI
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22 CHAPTER 4. INSTRUMENTATIONrespec
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24 CHAPTER 4. INSTRUMENTATIONangle
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Page 44 and 45: 30 CHAPTER 4. INSTRUMENTATIONTable
Page 46 and 47: 32 CHAPTER 5. CHANDRA OBSERVATIONS
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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
Page 125 and 126: 8.3. MAGNETIC RECONNECTION MODEL 11
Page 127 and 128: 8.5. EFFECT OF THE QUIESCENT X-RAYS
Page 129 and 130: 8.6. EVOLUTION OF YSOS AND THEIR FL
Page 131 and 132: Chapter 9ConclusionWe summarize the
Page 133 and 134: Appendix AFlare Light CurvesFig. A.
Page 135 and 136: Fig.A.2 (Continued)121
Page 137: 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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X-ray Study of Low-mass Young Stellar Objects in the ρ Ophiuchi ...

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