Other
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992acasn..33..258c&link_type=abstract
Acta Astronomica Sinica (ISSN 0001-5245), vol. 33, no. 3, p. 258-266.
Other
1
Convection Currents, P Waves, Solar Atmosphere, Stellar Envelopes, Eigenvectors, Solar Magnetic Field, Solar Oscillations, Stellar Models
Scientific paper
Adiabatic p-mode eigenfrequencies for five solar convective envelope models are computed. For models with smaller convection parameter c1, the frequency differences divide into two distinct groups, one for e of 60 or less and another for e greater than 60. In the first group the difference decreases as the frequency increases, with the distribution in an inclined narrow strip. This indicates that the main error sources are located in the outermost 5 percent of the solar radius, with some nonadiabatic effects and the uncertainty in the equation of state being the possible source. In the second group, the theoretical eigenfrequencies are systematically smaller than the observed ones, implying that another error source is located at the bottom of the solar convection zone and the overshooting region below. It may be best explained by a magnetic field of 1000-10,000 gauss in the lower part of the solar convection zone.
Cheng Qi-Liang
Xiong Da-Run
No associations
LandOfFree
The middle-high degree adiabatic p-mode eigenfrequencies of the solar envelope models does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The middle-high degree adiabatic p-mode eigenfrequencies of the solar envelope models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The middle-high degree adiabatic p-mode eigenfrequencies of the solar envelope models will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1765166