Computer Science
Scientific paper
Dec 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286..525s&link_type=abstract
In ESA, Seismology of the Sun and Sun-Like Stars p 525-528 (SEE N89-25819 19-92)
Computer Science
1
Convection, Solar Activity Effects, Solar Atmosphere, Solar Oscillations, Mixing Length Flow Theory, Pressure Distribution, Stellar Models
Scientific paper
Solar models are calculated with the nonlocal form of mixing length theory, applied to the lower part of the convection zone. The resulting overshoot layer has a depth of 16 Mm; this is 30 percent of the local pressure scale height. The parameters, alpha = (mixing length/pressure scale height) and the initial He-abundance Y0 are obtained by calculating a full model sequence in time to alpha = 1.505 and Y0 = 0.25637. The total convection zone has the depth d = 197 Mm at a temperature T = 2.166 MK compared to d = 181 Mm and T = 1.927 MK in the local case. This fact may have implications on the observed low Li-abundance. The influence of the overshoot layer on low-l modes shows an increase in the frequencies of the order of 1 micro Hz, thus lowering the difference to the observed frequencies. For intermediate-l modes where the reflection boundary is just below the overshoot region the effect is strongest, up to 4 microHz. High-l modes are slightly lowered by the overshoot effect. Nevertheless in all frequency ranges a discrepancy of several microHz remains.
Skaley D.
Stix Michael
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