Contents List of Figures

More documents

Recommendations

Info

310 6 MACRO– AND MICRO–JETS DRIVEN BY BLACK HOLES Figure 147: Poloidal flow velocity along a collimated flux tube (top panel) and particle density (bottom panel) (Fendt & Greiner 2001). x = R/Rg
6.7 Formation of Micro–Jets 311 Figure 148: General relativistic simulation of a magnetized flow accreting onto a Kerr black hole (after Koide et al. 1999a). Left panel shows one quadrant of the initial model with the j = 0.95 hole at lower left, freely-falling corona, and non-rotating disk. The hole rotation axis (Z) is along the left edge. The initial magnetic field (vertical lines) is weak compared to the matter rest energy density (VA = 0.01c). Right panel shows final model at t = 130GMH/c 3 . Some of the disk and corona have been accreted into the hole, threading the ergosphere and horizon with magnetic field lines that develop a significant radial component, and hence an azimuthal component as well, due to differential frame dragging. The resulting jet outflow is accelerated by J × B forces to a Lorentz factor of 2.7. [Koide et al. 2001] The authors also studied counter-rotating and co-rotating Keplerian disks with otherwise similar initial parameters (Koide et al. 1999b). The counter-rotating case behaved nearly identically to the non-rotating case: because the last stable retrograde orbit is at Rms = 9GMH/c 2 , the disk began to spiral rapidly into the ergosphere, ejecting a strong, black-hole-spin-driven MHD jet. On the other hand, for prograde orbits Rms = GMH/c 2 , so the co-rotating disk was stable, accreting on a slow secular time scale. At the end of the calculation (tmax = 94GMH/c 3 ), when the simulation had to be stopped because of numerical problems, the disk had not yet accreted into the ergosphere and had produced only a weak MHD jet. Future evolution of this case is still uncertain. The Keplerian Schwarzschild case was previously reported by Koide et al. (1998) and developed a moderate sub-relativistic MHD jet similar to the aforementioned simulations of magnetized Keplerian flows around normal stars, plus a pressure-driven splash outflow internal to the MHD jet. In the Kerr cases, significant magnetic field enhancement over the Schwarzschild
Page 1 and 2: CONTENTS 265 Contents 6 Macro- and
Page 3 and 4: 6 Macro- and Micro-Jets Driven by B
Page 5 and 6: 6.1 DRAG(o)Ns - FR I and FR II 269
Page 11 and 12: 6.2 Jets as Super(magneto)sonic Col
Page 13 and 14: 6.2 Jets as Super(magneto)sonic Col
Page 15 and 16: 6.3 Fundamental Parameters for Jets
Page 17 and 18: 6.3 Fundamental Parameters for Jets
Page 19 and 20: 6.4 A 3-Phase Model for Kiloparsec-
Page 25 and 26: 6.5 Relativistic Jet Propagation 28
Page 27 and 28: 6.6 Structure and Emission of Micro
Page 37 and 38: 6.7 Formation of Micro-Jets 301 6.7
Page 39 and 40: 6.7 Formation of Micro-Jets 303 Fig
Page 41 and 42: 6.7 Formation of Micro-Jets 305 Thi
Page 43 and 44: 6.7 Formation of Micro-Jets 307 VLB
Page 45: 6.7 Formation of Micro-Jets 309 as
Page 53 and 54: 6.7 Formation of Micro-Jets 317 the
Page 55 and 56: 7.1 The Dark Age 319 Figure 152: Da
Page 57 and 58: 7.3 The First Quasars 321 Figure 15
Page 59 and 60: 7.3 The First Quasars 323 Bromm & L
Page 61: REFERENCES 325 [17] Leahy, P. 1993,

Contents List of Figures

Create successful ePaper yourself

Delete template?

Save as template?