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

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46 CHAPTER 5. CHANDRA OBSERVATIONS OF THE ρ OPHIUCHI CLOUD(footnotes for Table 5.2)* Background-subtracted X-ray counts in 0.5–2.0 keV, 2.0–9.0 keV, and 0.5–9.0 keV for soft-band, hard-band, and theother sources, respectively. (m) denotes sources with marginal detections (the confidence level < 99.9 %, see §5.2).Although the confidence levels of A-48 and A-H2 are significant enough, we regard them as marginal sources becauseof the larger source size (A-48) and severe contamination from A-2 (A-H2).† Right ascension and declination for all sources are 16h and −24 ◦ .‡ Parentheses indicate the 90 % confidence limits.§ Observed flux (10 −14 ergs s −1 cm −2 ) and absorption-corrected X-ray luminosity (10 29 ergs s −1 ; “< L X >” in thetext) in 0.5–9.0 keV.‖ Reduced-χ 2 for the spectral fittings. Parentheses indicate the degrees of freedom.# We determine spectral parameters with fixed temperatures of 1 keV and 5 keV (see text). For sources which onlyshow the parameters for kT = 1 or 5 keV, no good fitting is obtained for the other temperature.** We assume the same abundances as the “F2” phase in Table 6.3. The quiescent spectrum is not obtained becausethe decay phases of the two flares occupy all of the light curve.†† The pileup effect is not corrected.‡‡ No spectral fit is done due to the limited statistics.§§ Abundances are free parameters (§6.3.2, §6.3.3, and §6.3.7).‖‖ We make the flare spectra with a bit larger timescale in order to obtain as good statistics as possible. Errors of for A-29 in the quiescent are not determined because of the limited statistics.## The spectra show the possible absorption edge of neutral Ca or warm Ar. The non-thermal model also wellreproduces the spectra (§6.3.5, see also Hamaguchi et al. 2002).*** We assume the same temperature because of the limited statistics.† † † These show non-thermal spectra (§6.6.3).‡ ‡ ‡ These show two temperature model with an unusual abundance pattern (§6.2).§§§ Foreground star. The distance is 60 pc (Festin, 1998).‖‖‖ The best-fit value of < kT > is not determined (larger than 10 keV), hence we assume 10 keV temperature forthe estimation of the other parameters.### N H and reduced-χ 2 are estimated by the simultaneous fittings with the identical sources in obs-A.
5.7. THE CATALOGUE OF X-RAY SOURCES IN ρ OPH 475.7.2 Identifications of the X-ray sourcesTable 5.3:: Identifications of the X-ray sourcesNo. Offset * Radio † —- X-ray —- ‡ Other names § Class ‖( ′′ ) P SP C HRI ASCA IKTA-1 ... ... ... ... ... ... ... ...A-2 0.33 R8, S7 13 A11 3 ... DoAr21, ROXs8, YLW26, GSS23, IIIElias14, SKS1-5, ISO10A-3 0.40 ... ... ... ... ... ISO13 IIA-4 7.54(R) R9? ... ... ... ... ... ...A-5 0.60 ... 15? A13 ... ... ISO14 IIIA-6 0.23 ... 16 ... ... ... GSS26, CRBR5, SKS1-6, ISO17 IIA-7 ... ... ... ... ... ... ... ...A-8 ... ... ... ... ... ... ... ...A-9 ... ... ... ... ... ... ... ...A-10 ... ... ... ... ... ... ... ...A-11 ... ... ... ... ... ... ... ...A-12 0.47 ... ... ... ... ... CRBR9, SKS1-7, ISO18 III cA-13 ... ... ... ... ... ... ... ...A-14 0.11 Lp1 18 A14 ... ... ROXs11, GSS29, Elias18, CRBR10, IISKS1-8, ISO19A-15 0.44 ... 17 A15 ... ... DoAr24, ROXs10A, GSS28, Elias19, IICRBR11, SKS1-9, ISO20A-16 1.08 ... ... ... ... ... 2MASSI J1626172−241238 ?A-17 ... ... ... ... ... ... ... ...A-18 ... ... ... ... ... ... ... ...A-19 0.38 ... 19 ... ... ... YLW31, VSSG1, Elias20, ISO24 IIA-20 0.03 L2 ... A17 ... ... GY12, VSSG12, ISO34 IIIA-21 ... ... ... ... ... ... ... ...A-22 0.19 ... 24(22?) A18 4 ... ROXs10B, GY20, GSS31, Elias22, IICRBR29, SKS1-15, ISO36A-23 0.23 L3 ... ... ... ... GY21, CRBR30, SKS1-16, ISO37 IIA-24 0.14 ... 25 A19 C3 ... S2, GY23, GSS32, Elias23, CRBR32, IISKS1-17, ISO39A-25 0.15 ... 26 A20 ... ... YLW32, Elias24, ISO40 IIA-26 0.09 ... ... ... ... ... GY31, CRBR34, SKS3-15 ? ‖‖A-27 0.12 ... ... ... ... ... GY29, CRBR35, SKS1-18, ISO41 IIA-28 0.55 ... ... ... ... ... 2MASSI J1626257−241427 ?A-29 ... ... ... ... ... ... ... ...A-30 0.05 ... C15 ... ... ... GY37, VSSG29, CRBR37, ISO42 BD c (III c )A-31 2.66(R) L6? ... ... ... ... ... ...A-32 0.92 ... ... ... ... ... ISO44 III cA-33 0.06 L8 27 ... ... ... SKS1-19, ISO45 IIIA-34 0.72 L9 ... ... ... ... GY51, VSSG27, CRBR38, SKS1-20, IIISO46A-35 ... ... ... ... ... ... ... ...A-36 1.14 ... ... ... ... ... YLW35, GY54, IRS14, ISO47 III cA-37 1.42(R) L10 ... ... ... ... ... ...A-38 0.24 ... ... ... ... ... GY59, CRBR39, SKS1-21 BD cA-39 ... ... ... ... ... ... ... ...A-40 ... ... ... ... ... ... ... ...
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
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
Page 42 and 43: ¨28 CHAPTER 4. INSTRUMENTATIONspli
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
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Page 76 and 77: 62 CHAPTER 6. INDIVIDUAL SOURCES6.2
Page 78 and 79: 64 CHAPTER 6. INDIVIDUAL SOURCESfla
Page 80 and 81: 66 CHAPTER 6. INDIVIDUAL SOURCESTab
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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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Page 118 and 119:
Page 121 and 122:
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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