Computer Science
Scientific paper
Jun 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005mpge.conf...31e&link_type=abstract
The Magnetized Plasma in Galaxy Evolution, Proceedings of the conference held in Kraków, Poland, Sept. 27th - Oct. 1st, 2004, Ed
Computer Science
Scientific paper
Diffuse thermal X-ray emission due to the hot gas component of the ISM is seen not only in the disks but also up to large distances above the planes of edge-on starburst galaxies. These outflows do not only have an influence on the evolution of the galaxy but are potentially significant also in enriching and heating of the intergalactic medium. A widely accepted model is that supernovae (and stellar winds) in the disks of star-forming galaxies create, via blow-out and venting of hot gas, a tenuous hot extraplanar ISM gas component. The soft thermal X-ray emission observed is either this metal-enriched preexisting halo medium, which has been swept up and shock-heated by the starburst driven wind, or wind material compressed near the walls of the outflow by reverse shocks within the wind. Observations of starburst galaxies with the current generation of X-ray telescopes (XMM-Newton and Chandra) are demonstrating that the soft thermal X-ray halo emission is highly structured and spatially correlated with Hα emission, as expected in case of an interaction of the galactic wind with a cooler ambient medium. The role of the halo magnetic field configuration in the dynamics of the hot X-ray emitting gas has not yet been addressed in detail but a correlation of X-ray halo features and vertical magnetic field lines might exist.
No associations
LandOfFree
The Coronal Gas Phase of the ISM 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 The Coronal Gas Phase of the ISM, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Coronal Gas Phase of the ISM will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1421135