Alma Mater Studiorum Universit`a degli Studi di Bologna ... - Inaf

More documents

Recommendations

Info

88 5. Ordered magnetic fields around radio galaxies 0206+35 Figure 5.4: Plots of E-vector position angleΨagainstλ 2 at representative points of the 1.2 arcsec RM map of 0206+35. Fits to the relationΨ(λ)=Ψ 0 + RMλ 2 are shown. The values of RM are given in the individual panels. In order to constrain RM structure on spatial scales below the beamwidth, I estimated the depolarization as described in Section 5.2. The fitted k values are listed in Table 5.5. I stress that these values refer only to areas with isotropic fluctuations, and cannot usefully be compared with the integrated depolarizations quoted in in Fig. 5.2. For M 84, using the Burn law k analysis and assuming that variation of Faraday rotation across the 1.65-arcsec beam causes the residual depolarization, I find thatΛ min < ∼ 0.1 kpc for any reasonable RM power spectrum. 5.6 Rotation-measure bands from compression It is clear from the fact that the observed RM bands are perpendicular to the lobe axes that they must be associated with an interaction between an expanding radio source and the gas immediately surrounding it. One inevitable mechanism is enhancement of field and density by the shock or compression wave surrounding the source. 1 The implication of the presence of cavities in the X-ray gas distribution coincident with the radio lobes is that the sources are interacting strongly 1 An alternative mechanism is the generation of non-linear surface waves (Bicknell, Cameron & Gingold 1990). It is unlikely that this can produce large-scale bands, for the reasons given in Section 5.8.5. 88
5.6. Rotation-measure bands from compression 89 0206+35 M 84 3C 270 3C 353 Figure 5.5: Profiles of mean and rms RM and Burn law k along the radio axis. The profiles have been derived by averaging over boxes perpendicular to the radio axis of length 5 kpc for all sources except M 84, for which the box length is 2 kpc. The orange (dashed) and violet (longdashed) lines represent the Galactic RM contribution and the〈RM〉 of the lobes, respectively. All unblanked pixels are included. 89
Page 1:
Alma Mater Studiorum Università de
Page 5:
To Hypatia from Alexandria in Egypt
Page 9 and 10:
Contents Abstract i 1 Physics of ra
Page 11 and 12:
4.6.3 The outer scale of the magnet
Page 13 and 14:
Abstract The existence of diffuse m
Page 15 and 16:
2. Two-dimensional Monte Carlo simu
Page 17 and 18:
Chapter 1 Physics of radio galaxies
Page 19 and 20:
1.2. Non-thermal emission mechanism
Page 21 and 22:
1.2. Non-thermal emission mechanism
Page 23 and 24:
1.3. Radio galaxies 7 FR II sources
Page 25 and 26:
1.3. Radio galaxies 9 (a) (b) Figur
Page 27 and 28:
1.3. Radio galaxies 11 pressure, th
Page 29 and 30:
Chapter 2 The X-ray environment of
Page 31 and 32:
2.2. The thermal component 15 Figur
Page 33 and 34:
2.3. Radio source - environment int
Page 35 and 36:
2.3. Radio source - environment int
Page 37 and 38:
Chapter 3 Magnetic fields in the ho
Page 39 and 40:
3.1. Introduction 23 Figure 3.1: Ex
Page 41 and 42:
3.1. Introduction 25 to the relativ
Page 43 and 44:
3.2. Faraday Rotation 27 The RM can
Page 45 and 46:
3.2. Faraday Rotation 29 Figure 3.4
Page 47 and 48:
3.3. Depolarization 31 3.3 Depolari
Page 49 and 50:
3.5. The magnetic field profile 33
Page 51 and 52:
3.6. Tangled magnetic field 35 rad
Page 53 and 54: 3.7. The magnetic field power spect
Page 59 and 60: Chapter 4 Structure of the magneto-
Page 61 and 62: 4.1. The radio source 3C 449: gener
Page 63 and 64: 4.3. The Faraday rotation in 3C 449
Page 65 and 66: 4.3. The Faraday rotation in 3C 449
Page 67 and 68: 4.4. Depolarization 51 Figure 4.4:
Page 69 and 70: 4.4. Depolarization 53 1.25 arcsec
Page 71 and 72: 4.5. Two dimensional analysis 55 sm
Page 73 and 74: 4.5. Two dimensional analysis 57 Fi
Page 75 and 76: 4.6. Three-dimensional analysis 59
Page 83 and 84: 4.7. Summary and comparison with ot
Page 89 and 90: Chapter 5 Ordered magnetic fields a
Page 91 and 92: 5.1. The Sample 75 35 49 00 ROSAT P
Page 93 and 94: 5.1. The Sample 77 5.1.1 0206+35 02
Page 95 and 96: 5.2. Analysis of RM and depolarizat
Page 97 and 98: 5.3. Rotation measure images 81 IMA
Page 99 and 100: 5.3. Rotation measure images 83 cor
Page 101 and 102: 5.4. Depolarization 85 Therefore, a
Page 103: 5.5. Rotation measure structure fun
Page 107 and 108: 5.6. Rotation-measure bands from co
Page 109 and 110: 5.6. Rotation-measure bands from co
Page 111 and 112: 5.7. Rotation-measure bands from a
Page 113 and 114: 5.7. Rotation-measure bands from a
Page 115 and 116: 5.8. Discussion 99 5.8 Discussion 5
Page 117 and 118: 5.8. Discussion 101 line−of−sig
Page 119 and 120: 5.8. Discussion 103 flat slopes. I
Page 121 and 122: 5.9. Conclusions and outstanding qu
Page 123 and 124: 5.9. Conclusions and outstanding qu
Page 125 and 126: Chapter 6 Faraday rotation in two e
Page 127 and 128: 6.2. Two-dimensional analysis: rota
Page 135 and 136: 6.3. Two-dimensional analysis: stru
Page 137 and 138: 6.4. Preliminary conclusions 121 Ta
Page 139 and 140: 6.4. Preliminary conclusions 123
Page 141 and 142: Summary and conclusions The goal of
Page 143 and 144: 6.5. Summary 127 responsible for th
Page 145 and 146: 6.6. General conclusions 129 radio
Page 147 and 148: 6.7. Future prospects 131 and is th
Page 149: Appendix 133
Page 152 and 153: 136 Data reduction and imaging of l
Page 154 and 155:
138 Data reduction and imaging of l
Page 156 and 157:
Page 158 and 159:
Page 160 and 161:
144 BIBLIOGRAPHY Bîrzan, L., Raffe
Page 162 and 163:
146 BIBLIOGRAPHY Ensslin, T.A. & Go
Page 164 and 165:
148 BIBLIOGRAPHY Jeltema, T.E. & Pr
Page 166 and 167:
150 BIBLIOGRAPHY Owen, F.N., 1989,
Page 168 and 169:
152 BIBLIOGRAPHY 152
show all

Alma Mater Studiorum Universit`a degli Studi di Bologna ... - Inaf

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?