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

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56 CHAPTER 5. CHANDRA OBSERVATIONS OF THE ρ OPHIUCHI CLOUDTable 5.4 (Continued)No. t p τ r τ d Q Comment(ks) (ks) (ks) (Cts ks −1 )BF-36 30 4.4(1.7–9.4) ... ‡ 0.8(0.6–0.9)BF-92 20 0.5 * 2.6(1.1–4.4) 1.9 ** We can not determine errors because of the limited statistics and/or strong coupling of the otherparameters.† Fitting is obtained for light curves in 2. ′′ 5–12. ′′ 5 (A-2) and 2. ′′ 5–7. ′′ 5 (BF-64) radius circles in orderto avoid the pileup effect.‡ No fitting is possible because of the limited statistics and/or the boundary of the observations.§ We relax the flare peak time (t p ) to be free in order to obtain as good results as possible.‖ This should be the upper limit because the fitting does not include the time bin with zero counts.
Chapter 6Individual SourcesIn this chapter, we show details of some interesting sources.6.1 Protostars6.1.1 A-49 – GY91Fig. 6.1.— ACIS image around A-49 = GY91 in 0.5–9.0 keV, smoothed with a Gaussian of σ = 4 pixels.The solid rectangle represents the region for the X-raydata of jet-like emission (see text). Many cloud cores(not given in this figure) are aligned along the directiongiven by the dashed line (see Figure 3.1).Figure 6.1 shows the ACIS image of a class I source GY91 (A-49). Besides significant X-rays from the central source, we can see weak diffuse jet-like emission to the north-east (the solidrectangle in Figure 6.1) perpendicular to the cloud core alignment; many cloud cores are alignedalong the dashed line in Figure 6.1 (see also Figure 3.1). This X-ray “jet” is likely due to an outflowfrom GY91, although the significance level is still low (∼2.3 σ). We make the spectrum from therectangle region and fit it by the MEKAL model. Then we constrain the plasma temperature to be57
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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
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
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Page 30 and 31: 16 CHAPTER 3. REVIEW OF THE ρ OPHI
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Page 40 and 41: 26 CHAPTER 4. INSTRUMENTATIONThe AC
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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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