Large scale simulation of a very light jet
- computed with NIRVANA
- final size:> 200 jet radii
- resolution: 20 points per beam radius
- King cluster atmosphere
- bipolar simulation
- initial density contrast 1/10,000 (jet/IGM)
- no magnetic field
- 2.5D axysymmetrtic
- Density films: (970 frames)
[gif, 100MB] [MPEG IM, 5MB] - Density films: (97 frames)
[gif, 10MB] [jpg, 0.9MB] [h363+, 0.9MB] [ISO MPEG4, 0.9MB] [pre MPEG4 v3, 0.9MB] [pre MPEG4 v2, 0.8MB] [real, 0.9MB] [gif, 1MB] [MPEG1, 0.9MB] [MPEG IM, 0.5MB] - papers:
HPCSE'03 (computational)
ApSS 04 (astrophysical, short)
A&A( small) - talks:
Workshop: Formation and Early Evolution of Galaxies (Irsee, Germany) [abstract] [slides]
Leiden Workshop on Emission Line Halos 20th June 2003 [slides]
Virtual Jets 2003 (Dogliani, Italy) [slides] [proceedings]
![[gif, 100MB]](dfilms/mghk_axy_large0.gif){kind=link}
![[gif, 10MB]](dfilmsmall/mghk_axy_large.ds0.gif){kind=link}
Line of sight integrated X-ray emission (left) compared to Chandra X-ray contours of the radio galaxy Cygnus A with radio colors (right). The bow shock is located where elliptical contours change into spherical ones, which is well measured for Cygnus A (Smith et al. 2002).
