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Shapes of star-gas waves in spiral galaxies
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Lubow, Stephen H. |
| Copyright Year | 1988 |
| Description | Density-wave profile shapes are influenced by several effects. By solving viscous fluid equations, the nonlinear effects of the gas and its gravitational interaction with the stars can be analyzed. The stars are treated through a linear theory developed by Lin and coworkers. Short wavelength gravitational forces are important in determining the gas density profile shape. With the inclusion of disk finite thickness effects, the gas gravitational field remains important, but is significantly reduced at short wavelengths. Softening of the gas equation of state results in an enhanced response and a smoothing of the gas density profile. A Newtonian stress relation is marginally acceptable for HI gas clouds, but not acceptable for giant molecular clouds. |
| File Size | 363481 |
| Page Count | 7 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_19900006543 |
| Archival Resource Key | ark:/13960/t86h9fw9t |
| Language | English |
| Publisher Date | 1988-02-01 |
| Access Restriction | Open |
| Subject Keyword | Astronomy Gas Density Thickness Equations of State Gravitational Effects Smoothing Molecular Clouds Shock Fronts Gravitational Fields Nonlinearity Shapes Spiral Galaxies Viscous Fluids Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Article |
