Effects of convective velocities on solar pressure mode frequencies.
Abstract
There are persistent discrepancies between observations and theoretical calculations of solar p-mode frequencies, νobs, νcalc, in spite of improvements in the theory (e.g. equation of state). In this short communication, the authors propose to approximate roughly the difference (observation-calculation) versus frequency as: δν = νobs-νcalc ≈ -Kν2, where the constant K is of the order of 1 second, and independent of degree l. It has been already suggested by T. Brown that "Solar p-mode eigenfrequencies are decreased by turbulent convection". The authors want to revisit this suggestion and reformulate it in the following manner: is this physical effect responsible for some of the difference ν0-νcalc? After a brief discussion of the mechanism, the authors present an order of magnitude evaluation which shows that, indeed, it is worthwhile to pursue the idea further: this will be done in improving the description of the coupling between convection and oscillations.
- Publication:
-
Seismology of the Sun and Sun-Like Stars
- Pub Date:
- December 1988
- Bibcode:
- 1988ESASP.286..671D
- Keywords:
-
- Acoustic Measurement;
- Helioseismology;
- P Waves;
- Solar Atmosphere;
- Solar Oscillations;
- Numerical Analysis;
- Solar Physics;
- Sound Waves;
- Stellar Models;
- Solar Physics;
- Solar Oscillations: Solar Convective Zone