Galaxy evolution-Star formation connection: from PC to KPC scales
| Full text | |
| Author(s): |
Falceta-Goncalves, D.
[1, 2]
;
Bonnell, I.
[1]
;
Kowal, G.
[2]
;
Lepine, J. R. D.
[3]
;
Braga, C. A. S.
[3]
Total Authors: 5
|
| Affiliation: | [1] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife - Scotland
[2] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, BR-03828000 Sao Paulo - Brazil
[3] Univ Sao Paulo, Inst Astron Geofis & Cincias Atmosfer, BR-05508090 Sao Paulo - Brazil
Total Affiliations: 3
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 446, n. 1, p. 973-989, JAN 2015. |
| Web of Science Citations: | 14 |
| Abstract | |
Turbulence is ubiquitous in the interstellar medium (ISM) of the Milky Way and other spiral galaxies. The energy source for this turbulence has been much debated with many possible origins proposed. The universality of turbulence, its reported large-scale driving, and that it occurs also in starless molecular clouds, challenges models invoking any stellar source. A more general process is needed to explain the observations. In this work, we study the role of galactic spiral arms. This is accomplished by means of three-dimensional hydrodynamical simulations which follow the dynamical evolution of interstellar diffuse clouds (similar to 100 cm(-3)) interacting with the gravitational potential field of the spiral pattern. We find that the tidal effects of the arm's potential on the cloud result in internal vorticity, fragmentation and hydrodynamical instabilities. The triggered turbulence results in large-scale driving, on sizes of the ISM inhomogeneities, i.e. as large as similar to 100 pc, and efficiencies in converting potential energy into turbulence in the range similar to 10-25 per cent per arm crossing. This efficiency is much higher than those found in previous models. The statistics of the turbulence in our simulations are strikingly similar to the observed power spectrum and Larson scaling relations of molecular clouds and the general ISM. The dependence found from different models indicate that the ISM turbulence is mainly related to local spiral arm properties, such as its mass density and width. This correlation seems in agreement with recent high angular resolution observations of spiral galaxies, e.g. M51 and M33. (AU) | |
| FAPESP's process: | 13/04073-2 - Magnetic reconnection and related processes in collisional and collisionless astrophysical plasmas: from solar flares to extragalactic sources |
| Grantee: | Grzegorz Kowal |
| Support type: | Research Grants - Young Investigators Grants |
| FAPESP's process: | 11/12909-8 - Magnetic fields, turbulence and plasma effects in the intergalactic medium |
| Grantee: | Diego Antonio Falceta Gonçalves |
| Support type: | Regular Research Grants |
| FAPESP's process: | 13/18815-0 - Magnetic reconnection and related processes in collisional and collisionless astrophysical plasmas: from solar flares to extragalactic sources |
| Grantee: | Grzegorz Kowal |
| Support type: | Scholarships in Brazil - Young Researchers |