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The solar envelope
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Burlaga, L. F. |
| Copyright Year | 1971 |
| Description | Processes which occur within the region between approximately 2 solar radii and 25 solar radii, which is called the solar envelope and the effect on the solar wind as seen at 1 AU are discussed. In the envelope the wind speed becomes supersonic and super-Alfvenic, the magnetic energy density is larger than the flow energy density, and the magnetic energy density is much larger than the thermal energy density. Large azimuthal gradients in the bulk speed are expected in the envelope, but the stream interactions near the outer edge of the envelope are probably relatively small. Cosmic ray observations suggest the presence of hydromagnetic waves in the envelope. The collisionless damping of such waves could heat protons out to approximately 25 solar radii and thereby cause an increase in V and T sub p consistent with the observed T sub p -V relation. A mechanism which couples protons and electrons would also heat and accelerate the wind. Alfven waves can accelerate the wind in the envelope without necessarily causing heating of protons; the Lorentz force might have a similar effect. |
| File Size | 1370723 |
| Page Count | 52 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_19720003184 |
| Archival Resource Key | ark:/13960/t50g8dt55 |
| Language | English |
| Publisher Date | 1971-10-01 |
| Access Restriction | Open |
| Subject Keyword | Space Radiation Magnetohydrodynamic Waves Solar Activity Effects Solar Energy Magnetic Effects Solar Physics Solar Radiation Solar Wind Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Technical Report |
