NDLI: Theory and Models of the Disk-Halo Connection — Modelling the Disk-Halo Interaction in Galaxies

Content Provider	EDP Sciences
Author	D. Breitschwerdt M.A. de Avillez V. Baumgartner V.A. Dogiel
Abstract	We review the evolution of the interstellar medium in disk galaxies, and show, both analytically and by numerical 3D hydrodynamic simulations, that the disk-halo connection is an essential ingredient in understanding the evolution of star forming galaxies. Depending on the star formation rate of the underlying gaseous disk, a galactic fountain is established. If the star formation rate is sufficiently high and/or cosmic rays are well coupled to the thermal plasma, a galactic wind will be formed and lead to a secular mass loss of the galaxy. Such a wind leaves a unique imprint on the soft X-ray spectra in edge-on galaxies, with delayed recombination being one of its distinctive features. We argue that synthetic spectra, obtained from self-consistent dynamical and thermal modeling of a galactic outflow, should be treated on an equal footing as observed spectra. We show that it is thus possible to successfully fit the spectrum of the starburst galaxy NGC 3079
Ending Page	342
Starting Page	333
Page Count	10
File Format	HTM / HTML PDF
ISSN	16334760
Alternate Webpage(s)	https://www.eas-journal.org/articles/eas/abs/2012/04/eas1256055/eas1256055.html
e-ISSN	16381963
Journal	EAS Publications Series
Volume Number	56
DOI	10.1051/eas/1256055
Language	English
Publisher	EDP Sciences
Publisher Date	2012-01-01
Access Restriction	Subscribed
Rights Holder	© EAS, EDP Sciences, 2012
Content Type	Text
Resource Type	Article
Subject	Engineering Astronomy and Astrophysics Space and Planetary Science

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4	Project PI / Joint PI	Principal Investigator and Joint Principal Investigators of the project	Dr. B. Sutradhar bsutra@ndl.gov.in Prof. Saswat Chakrabarti will be added soon
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