Solar-like oscillations in late spectral class stars [electronic resource].
- Published
- Los Alamos, N.M. : Los Alamos National Laboratory, 1988.
Oak Ridge, Tenn. : Distributed by the Office of Scientific and Technical Information, U.S. Dept. of Energy. - Physical Description
- Pages: 6 : digital, PDF file
- Additional Creators
- Los Alamos National Laboratory and United States. Department of Energy. Office of Scientific and Technical Information
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- Restrictions on Access
- Free-to-read Unrestricted online access
- Summary
- We investigate the minimum mass star that can exhibit solar-like nonradial p-mode oscillations. Solar models have almost equal pulsational driving and damping due to standard radiative effects. Coupling with surface convective elements occasionally tips the balance by strongly driving for a few days modes with convection timescales at the top of the convection zone. Then both convective and radiative damping decrease the mode amplitude at an observed decay rate, until the next convective reexcitation. Population I stellar models at 0.30, 0.45, and 0.75 Msub solar have been constructed to see if they have a near equality of radiative driving and damping also. If so, then stars down to late spectral class could possibly display solar-like oscillations. We find that the near equality of radiative driving and damping occurs down to about 0.5sub solar. Possibly 100 to 300 second oscillations can be observed through most of the K spectral class, if magnetic activity does not overwhelm these small amplitude nonradial pulsations. 24 refs., 6 figs., 6 tabs.
- Report Numbers
- E 1.99:la-ur-88-3219
E 1.99: conf-8809146-2
conf-8809146-2
la-ur-88-3219 - Subject(s)
- Other Subject(s)
- Note
- Published through SciTech Connect.
01/01/1988.
"la-ur-88-3219"
" conf-8809146-2"
"DE89000321"
Seismology of the sun and sun-like stars, Puerto de la Cruz, Spain, 26 Sep 1988.
Cox, A.N.; Cahn, J.H. - Funding Information
- W-7405-ENG-36
View MARC record | catkey: 13826224