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By Palle P.L., Esteban C. (eds.)

ISBN-10: 1107029449

ISBN-13: 9781107029446

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The only parameter that was changed from model to model, and therefore the only factor that could alter the observed shifts, was the maximum latitude of the activity, λmax . The minimum latitude was fixed for all models at λmin = 5 degrees. 51) ⎩ 0 otherwise. In the scenario above, the total surface magnetic flux is proportional to λmax − λmin , and therefore varied by over an order of magnitude for the range of computations made (10 ≤ λmax ≤ 70 degrees). Chaplin et al. (2007a) also made a second sequence of models in which the total flux was conserved for all values of λmax .

To describe the observed shifts as functions of time), hence circumventing the need to have complementary activity data. How large might the frequency bias be for other stars? The magnitude of the bias is governed to first order by the size of the acoustic asphericity, arising from the magnetic activity, and the angle of inclination of the star. , 2008, on correlations between different parameters). 8 shows the predicted bias from the first-order effects. Here, we assumed an acoustic asphericity similar to that observed on the Sun, as experienced by l = 1 and l = 2 modes at the center of the solar p-mode spectrum.

Pall´e, P. , and Jim´enez-Reyes, S. J. 2009. The onset of solar cycle 24: what global acoustic modes are telling us. ), L1–L4. , N. R. 2010 (June). What’s so peculiar about the cycle 23/24 solar minimum? Pages 3–13 of: S. R. Cranmer, J. T. Hoeksema, and J. L. Kohl (ed), SOHO-23: Understanding a Peculiar Solar Minimum. Astronomical Society of the Pacific Conference Series, vol. 428. Tapping, K. , and Detracey, B. 1990. 7 CM flux. Sol. , 127(June), 321–32. , and Wehrli, C. 1997. First Results from the SPM of the VIRGO/SOHO Experiment.

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Asteroseismology by Palle P.L., Esteban C. (eds.)


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