Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..275..383f&link_type=abstract
Jets at all Scales, Proceedings of the International Astronomical Union, IAU Symposium, Volume 275, p. 383-391
Astronomy and Astrophysics
Astronomy
Accretion, Accretion Disks, Stars: Magnetic Fields, Stars: Mass Loss, Stars: Winds, Outflows, Ism: Herbig-Haro Objects, Galaxies: Jets
Scientific paper
Jet formation MHD simulations are presented considering a variety of model setups. The first approach investigates the interrelation between the disk magnetisation profile and jet collimation. Our results suggest (and quantify) that outflows launched from a very concentrated region at the inner disk tend to be weakly collimated. In the second approach, jet formation is investigated from a magnetic field configuration consisting of a stellar dipole superposed by a strong disk field. We find that the central dipole considerably de-collimates the disk wind. In addition, reconnection flares are launched in the interaction region of disk and stellar magnetic field, subsequently changing the outflow mass flux by factors of two. The time interval between flare ejection is about 1000 Keplerian periods - surprisingly similar to the observed time lag between jet knots. The third approach considers radiative pressure effects on jet collimation - an environment which is interesting mainly for outflows from massive young stars (but also for relativistic jets). Finally we present relativistic MHD simulations of jet formation from accretion disks extenting the previous non-relativistic approaches.
Fendt Christian
Nezami Somayeh Sheikh
Porth Oliver
Vaidya Bhargav
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