| Issue |
A&A
Volume 407, Number 3, September I 2003
|
|
|---|---|---|
| Page(s) | 913 - 917 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361:20031019 | |
| Published online | 17 November 2003 | |
Applicability of a Schmidt law to star formation in ring galaxies
Institute of Physics, Stachki 194, Rostov-on-Don, Russia, and Isaac Newton Institute of Chile, Rostov-on-Don Branch, Russia
Corresponding author: eduard_vorobev@mail.ru
Received:
26
March
2003
Accepted:
19
June
2003
The gas hydrodynamics modeling of the Cartwheel ring galaxy is performed
with the purpose to reproduce the measured intensity and radial
distribution of 
emission in the Cartwheel's disk.
The star formation efficiency of 
is derived for
an assumed Schmidt law with power index 
and a full
thickness of the Cartwheel's gas disk of 
pc, respectively.
Simulations with a Schmidt law of star formation yield a higher surface brightness
(
)
in the Cartwheel's inner ring as compared to the observed values.
The Toomre criterion for star formation fails to account for the observed
sharp drop of massive star formation (MSF) in the inner ring.
Numerical simulations indicate that a large shear near/at the position of the inner ring
can raise the gas threshold for star formation and suppress MSF in
the Cartwheel's inner regions.
Hence, the Schmidt law has to be supplemented with a shear criterion for
star formation in order to reproduce the observed radial distribution of
in the Cartwheel's inner regions.
Key words: galaxies: individual: the Cartwheel / galaxies: starburst
© ESO, 2003
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