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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 308784.0, MPI für Astronomie / Publikationen_mpia
The supernova rate-velocity dispersion relation in the interstellar medium
Authors:Dib, S.; Bell, E.; Burkert, A.
Date of Publication (YYYY-MM-DD):2006
Journal Abbrev.:The Astrophysical Journal
Volume:638
Start Page:797
End Page:810
Audience:Not Specified
Abstract / Description:We investigate the relationship between the velocity dispersion of the gas and the supernova (SN) rate and feedback efficiency with three-dimensional numerical simulations of SN-driven turbulence in the interstellar medium (ISM). Our simulations aim to explore the constancy of the velocity dispersion profiles in the outer parts of galactic disks at ~6-8 km s-1 and the transition to the starburst regime, i.e., high star formation rates (SFRs) associated with high velocity dispersions. With our fiducial value of the SN feedback efficiency (i.e., epsilo=0.25, corresponding to an injected energy per SN of 0.25×1051 ergs), our results show that (1) SN driving leads to constant velocity dispersions of sigma~6 km s-1 for the total gas and sigmaHI~3 km s-1 for the H I gas, independent of the SN rate, for values of the rate between 0.01 and 0.5 the Galactic value (etaG) (2) the position of the transition to the starburst regime (i.e., location of sharp increase in the velocity dispersion) at around SFR/area~=5×10-3 to 10-2 Msolar yr-1 kpc-2 observed in the simulations is in good agreement with the transition to the starburst regime in the observations (e.g., NGC 628 and NGC 6949); (3) for the high SN rates, no H I gas is present in the simulations box; however, for the total gas velocity dispersion, there is good agreement between the models and the observations; (4) at the intermediate SN rates (eta/etaG~0.5-1), taking into account the thermal broadening of the H I line helps reach a good agreement in that regime between the models and the observations; and (5) for eta/etaG<0.5, sigma and sigmaHI fall below the observed values by a factor of ~2. However, a set of simulations with different values of ∊ indicates that, for larger values of the SN feedback efficiencies, velocity dispersions of the H I gas of the order of 5-6 km s-1 can be obtained, in closer agreement with the observations. The fact that for eta/etaG<0.5, the H I gas velocity dispersions are a factor of ~2 smaller than the observed values could result from the fact that we might have underestimated the SN feedback efficiency. On the other hand, it might also be an indication that other physical processes couple to the stellar feedback in order to produce the observed level of turbulence in galactic disks.
Free Keywords:Galaxies: ISM; Galaxies: Kinematics and Dynamics; Instabilities; ISM: Kinematics and Dynamics; ISM: Supernova Remnants; Turbulence
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi...
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