Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-27T02:02:55.654Z Has data issue: false hasContentIssue false
  • English
  • Français

The role of SN-driven turbulence on the formation of outflows, inflows and cooling flows: from Galaxies to Clusters of Galaxies

Published online by Cambridge University Press:  21 October 2010

E. M. de Gouveia Dal Pino ,
D. Falceta-Gonçalves ,
J. S. Gallagher ,
C. Melioli ,
A. D'Ercole  and
F. Brighenti
E. M. de Gouveia Dal Pino
Affiliation:
IAG, Universidade de São Paulo, Rua do Matão 1226, Sãao Paulo 05508-900, Brazil, [email protected]
D. Falceta-Gonçalves
Affiliation:
NAC, Universidade Cruzeiro do Sul, Rua Galvão Bueno 868, São Paulo 01506-000, Brazil
J. S. Gallagher
Affiliation:
Astronomy Department, University of Wisconsin, Madison, WI, USA
C. Melioli
Affiliation:
University of Bologna, Italy
A. D'Ercole
Affiliation:
University of Bologna, Italy
F. Brighenti
Affiliation:
University of Bologna, Italy
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Star forming galaxies often exhibit hot halos with structures that resemble chimneys and fountains extending for several kpc above the galaxy. Observations indicate that they are probably produced by supernovae (SNe) which blow superbubbles that carve holes in the disk. Through these holes, high speed material is injected and expands buoyantly up to a maximum height and then returns to the disk pulled by the galaxy gravity. This circulating gas in a fountain tends to condense out forming high-velocity clouds and filaments. Starburst galaxies also show evidence that the spectacular winds that arise from their disk are fed by SNe explosions. Similarly, at galaxy cluster scales, most massive clusters exhibit rich filamentary structure of ionized gas which is distributed all around the central galaxy. We discuss here the role that SNe bubbles play in driving outflows and filamentary structures both at galaxy and galaxy-cluster scales. With the help of HD and MHD numerical simulations, we show in particular that SN-driven turbulence may play a key role at helping a central AGN halting and ”isotropize” the cooling flow in the central regions of a galaxy cluster.

Keywords

supernovaeoutflowsgalaxiesgalaxy clusters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 452 - 453
Copyright
Copyright © International Astronomical Union 2010

References

de Gouvei ADal Pino, E. M., Melioli, C., D'Ercole, A., Brighenti, F. C., & Raga, A. 2009, Adv. Spa. Res., in press, arXiv:0803.3853v1Google Scholar
Falceta-Gonçalves, D., de Gouvei ADal Pino, E. M., Gallagher, J. S., & Lazarian, A., 2009, ApJ Lett., in pressGoogle Scholar
Hanasz, M., Otmianowska-Mazur, K., Kowal, G., & Lesch, H. 2009, A&A, 498, 335Google Scholar
Melioli, C., Brighenti, F. C., D'Ercole, A., & de Gouvei ADal Pino, E. M. 2008, MNRAS, 388, 573CrossRefGoogle Scholar
Melioli, C., Brighenti, F. C., D'Ercole, A., & de Gouvei ADal Pino, E. M. 2009, MNRAS, 399, 1089CrossRefGoogle Scholar