Astronomy and Astrophysics – Astrophysics
Scientific paper
2007-11-26
Astronomy and Astrophysics
Astrophysics
4 Pages, 3 figures + online material ; Accepted for publication in A&A Letters. Higher resolution version may be downloaded he
Scientific paper
10.1051/0004-6361:20078915
Emission-lines in the form of filamentary structures is common in bright clusters characterized by short cooling times. In the Perseus cluster, cold molecular gas, tightly linked to the H$\alpha$ filaments, has been recently revealed by CO observations. In order to understand the origin of these filamentary structures, we have investigated the evolution of the hot ICM gas perturbed by the AGN central activity in a Perseus like cluster. Using very-high resolution TreeSPH simulations combined with a multiphase model and a model of plasma bubbles, we have been able to follow the density and temperature evolution of the disturbed ICM gas around the bubbles. Our simulations show that a fraction of the $1-2 \rm{keV}$ gas present at the center of clusters is trapped and entrained by the rising buoyant bubble to higher radius where the AGN heating is less efficient. The radiative cooling makes it cool in a few tens of Myr below $10^4 \rm{K}$, forming cold filamentary structures in the wake and in the rim of the bubbles.
Combes François
Revaz Yves
Salomé Philippe
No associations
LandOfFree
Formation of cold filaments in cooling flow clusters does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Formation of cold filaments in cooling flow clusters, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Formation of cold filaments in cooling flow clusters will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-170983