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On the Velocity and Intensity Asymmetries of Solar P-Mode Lines

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Abstract

We show that to explain the opposite line asymmetries shown by the velocity and intensity spectra, it is necessary to solve the full non-adiabatic problem which is at least of the fourth order.

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References

  • Duvall, T.L., Jr., Jefferies, S.M., Harvey, J.W., Osaki, Y. and Pomerantz, M.A.: 1993, ‘Asymmetries of solar oscillation line profiles', ApJ 410, 829.

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  • Gabriel, M.: 1992, ‘On the solar p-mode spectrum excited by convection', A&A 265, 771.

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  • Gabriel, M.: 1993, ‘On the location of the excitation of solar p-modes', A&A 274, 935.

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  1. Institut d'Astrophysique, 5 Av. de Cointe, B-4000, Liège, Belgium

    M. Gabriel

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  1. M. Gabriel
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Gabriel, M. On the Velocity and Intensity Asymmetries of Solar P-Mode Lines. Space Science Reviews 85, 113–116 (1998). https://doi.org/10.1023/A:1005196921546

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  • DOI: https://doi.org/10.1023/A:1005196921546

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