The Magnetorotational Instability. 16 October 2004. Large Scale Computation in Astrophysics ... Jean-Pierre De Villiers (UVa; U. Calgary) Steven A. Balbus (UVa) ...
Christensson et al. (2001, PRE 64, 056405) helical vs. nonhelical. 5. Helical decay law: ... M. Christensson, M. Hindmarsh, A. Brandenburg: 2005, AN 326, 393. 7 ...
New scheme for driving end caps scales with rotation speed ... Larger for profiles with larger flow shear and higher speed. Qualitative results from data ...
T Tauri disks in Taurus observed to viscously spread with ~ 10-2 [Hartmann et al. ... Steep profile (r) = 343 (r / 10 AU)-2.17 g cm-2 is not consistent with steady ...
Lecture 5. Population synthesis of NSs Sergei Popov (SAI MSU) Population synthesis in astrophysics Why PS is necessary? Tasks Two variants Examples Magnetorotational ...
Title: Magnetorotational mechanism: 2D Simulations of Supernova Explosions and ejections Author: max Last modified by: GENA Created Date: 2/5/2001 1:31:21 PM
Steven A. Balbus. Ecole Normale Sup rieure. Physics Department. Paris, France. IAS MRI Workshop ... The MAGNETOROTATIONAL INSTABILITY (MRI) has taught us that ...
Antony Mee (Univ. Newcastle) Nils Haugen (NTNU, Trondheim) and many more... Started in Sept. 2001 with Wolfgang Dobler. High order (6th order in space, 3rd ...
Mark Wardle Macquarie University Sydney, Australia Protoplanetary disks Magnetic diffusion MRI with diffusion Ionisation equilibrium Live and Dead zones
A Heino-Centric View of the History of Galactic Center Theory ... Spin, precession and variability of Sgr A*. Linear Polarization images near the event horizon ...
Momentum Transport D. Craig General Meeting of the Center for Magnetic Self-Organization In Laboratory and Astrophysical Plasmas August 4-6, 2004 in Madison, WI
Magnetic fields are present on planets (Earth) ... map of the region illuminated by Hydra A, the. most luminous AGN in Hydra cluster (Taylor & Perley 1993) 4 ...
SHEARING SHEET. local model of a differentially rotating disc ... entirely absent (ky 0) in the shearing sheet. do not describe parallel shear flow instability ...
Title: Star formation - the accretion (luminosity) problem Author: Lee Hartmann Last modified by: Lee Hartmann Created Date: 6/6/1999 2:12:30 PM Document presentation ...
(Radiation: as a 3-step process) How to manage the contributions of 20 people ... MHD (Haugen), passive scalar (K pyl ), cosmic rays (Snod, Mee) Stratified layers ...
High order (6th order in space, 3rd order in time) Cache & memory efficient ... High resolution direct simulation. 5123 resolution. singular! 2563 (direct, new) ...
Understanding the physics of accretion-ejection flows. is central to the understanding of ... Jet acceleration and collimation. Emission from shocks in YSO jets ...
This work was partly supported by the 'Rikkyo University. Special Found ... generation of vorticity. dynamo by rotation of galaxy. within galaxy formation time ...
Magneto-hydrodynamic turbulence: from the ISM to discs. Axel ... Depends on Rm of vortical flow component. Bimodal: Rm=35 (w/o shocks), 70 (w/ shocks) ...
Equipartition field in the minimum solar nebula. Evidence for 0.1 1 G fields in the solar nebula at 1AU ... minimum solar nebula. assume isothermal in z-direction ...
Title: Close-by young isolated neutron stars (and black holes) Author: polar Last modified by: sergepolar Created Date: 4/1/2005 6:24:30 AM Document presentation format
Common superhumps shown by Whitehurst and several others to be the result of ... Bonnet-Bidaud, Motch, & Mouchet (1985) first to suggest the 5.2-hr period in TV ...
Relativistic accretion disks/tori. More energy may come from the disk than the hole ... Dissipation inevitable if V c/ln(qmax/qmin) ~ 0.1c; otherwise not. cf PWN ...
Magnetic diffusion regimes. ions, electrons and neutrals decoupled. ions and electrons decoupled ... distinct diffusion regimes: Ohmic (resistive) Hall ...
Black Hole rotation vertical field: Blandford-Znajek Poynting flux jet ... Black hole accretion process require us to describe the behaviour of matter ...
The interaction of a giant planet with a disc with MHD turbulence II: The interaction of the planet with the disc Papaloizou & Nelson 2003, MNRAS 339 (4), 993
1961-2 Hoyle, Fowler - radio sources are powered by ... 1964 Zel'dovich & Novikov, Salpeter et al - black holes. 1965 Dent - variability. More history ...
Gamma Ray Bursts? 1 ix 05. GLAST GC Meeting. 3. Traditional Disks are: ... X. Can you measure the toroidal field pattern? Even Parity. Odd Parity. Mixed Parity ...
... in 2D dissipation rate. after saturation is sensitive to numerical dissipation: Code Test ... Numerical dissipation is ~1.5 times smaller with. CTU & 3rd ...
Growth of Massive Black Holes in Active Galactic Nuclei Roger Blandford KIPAC, Stanford Assumptions and Notation Astrophysical holes depend upon mass and spin Charge ...
How are starbursts, low surface brightness galaxies different? Timescales ... value depends on corrections for dust obscuration, surface-brightness dimming ...
Accretion Power in Astrophysics Andrew King Theoretical Astrophysics Group, University of Leicester, UK Accreting Black Holes in a Nearby Galaxy (M101) Accreting ...
have rotation rates such that Vrot ~ 0.3-2 x Vrot (Jupiter) after. contraction down to the mean ... Snapshots of sims with different. Tcool, all after ~ 10 Torb ...
Essentially ALL protostellar cloud magnetic flux must be lost during star ... collimation. Alfven surface. Accretion leads to ejection. dM/dt (wind) = 0.1 dM/dt (acc) ...
A Crab-like field of 1012 Gauss and a Crab-like rotation. of 33 ms are dynamically unimportant. ... m = 1 single spiral arm mode. Outward transport of angular ...
FU Ori. FUor's are YSO's with significant circumstellar material. ... Observed frequency of FU Ori eruptions (last 50 years) is several times greater ...