981 research outputs found
Recommended from our members
Evolution Of Galaxies .4. Highly Flattened Disks
NSF GP-18335, GP-32051Astronom
Recommended from our members
Advanced Evolution Of Massive Stars .4. Secondary Nucleosynthesis During Helium Burning
NSF GP-32051, GP-23282Astronom
Recommended from our members
Evolution Of Galaxies .2. Chemical Evolution Coefficients
NSF GP-18355, GP-32051Astronom
The ring around SN1987A
Stars in the 9-40 solar mass range play a prominent role in the hydrodynamical and chemical evolution of galaxies. Their stellar winds and supernova explosions are believed to create the hot component of the interstellar medium (ISM). In some galactic disks, the kiloparsec sized super bubbles formed around clusters of massive stars may blow out of the disk plane and release hot, metal enriched gas into the galaxy's halo. Additionally, the expanding shock front of a super bubble in the disk may trigger additional star formation. Furthermore, similar processes probably drive the galactic winds associated with star burst nuclei that enrich the intracluster and intergalactic mediums. Nonetheless, the explosion of a blue super giant in the Large Magellanic Cloud (LMC), SN1987A, illuminated the incompleteness of our understanding of massive stars. Evolutionary models of massive stars do not synthesize the observed super giant populations in either the Milky Way or LMC. Our modeling of the formation of SN1987A's ring will improve our knowledge of both the post-main-sequence evolution of massive stars and their coupling to the ISM in galaxies
Turbulent Mixing in Stars: Theoretical Hurdles
A program is outlined, and first results described, in which fully
three-dimensional, time dependent simulations of hydrodynamic turbulence are
used as a basis for theoretical investigation of the physics of turbulence in
stars. The inadequacy of the treatment of turbulent convection as a diffusive
process is discussed. A generalization to rotation and magnetohydrodynamics is
indicated, as are connection to simulations of 3D stellar atmospheres.Comment: 5 pages, 1 figure, IAU Symposium 265, 200
- …