High resolution simulations of the filamentation in heavy jets
In 1983,
Norman et al. (sect. 5, 2nd paragraph)
have shown that dense jets shed filaments. Together with
Sebastian Jester,
I have studied the process in some detail. We propose to explain the
jet structure in 3C 273 in that way. This would have important consequences:
The jet has to be in a sparce environment and to be seen at low inclination.
This is an exceptional source, because most of the extragalactic jets are very light compared to their environment. Only because of its great length, this jet could reach regions that are even less dense.
Observations of 3C 273:
This is a radio image with optical (top) and X-ray (bottom) insets. The optical is enlarged on the right. The extensions that we identify with filaments are labeled "In" and "S". The feature near the tip of the jet is thought to be a galaxy.
This is an exceptional source, because most of the extragalactic jets are very light compared to their environment. Only because of its great length, this jet could reach regions that are even less dense.
- computed with NIRVANA
- final size: up to 120 jet radii
- resolution: up to 80 points per beam radius
- King cluster atmosphere
- unipolar simulations (reflection and open at injection side)
- density contrast 0.5 to 699 (jet/IGM)
- no magnetic field
- 2.5D axysymmetrtic
- Density films (full grid): [gif, 32MB] [mpeg, 0.8MB]
- Density films: (head) [gif, 77MB] [mpeg, 1.4MB]
![[gif, 32MB]](fhj.lgden.all.gif){kind=link}
![[gif, 77MB]](fhj.lgden.head.gif){kind=link}
Observations of 3C 273:
This is a radio image with optical (top) and X-ray (bottom) insets. The optical is enlarged on the right. The extensions that we identify with filaments are labeled "In" and "S". The feature near the tip of the jet is thought to be a galaxy.