Phases of the 5-Min Photospheric Oscillations above Granules and Intergranular Lanes

  • E. V. Khomenko
Conference paper
Part of the Astrophysics and Space Science Library book series (ASSL, volume 259)


The currently accepted excitation mechanism of solar oscillations is the stochastic excitation by turbulent convection with the acoustic energy output that scales as a high power of the Mach number of the convection (Goldreich and Kumar, 1988; Goldreich et al., 1994, and references therein). Acoustic events of large amplitudes might be observed with the help of high-resolution techniques as enhancements of the oscillatory amplitude localized in time and space (Brown, 1991). The analyses of observations performed by Rimmele et al. (1995) and Espagnet et al (1996) revealed that the amplitude amplification occurs mainly above the darkest intergranular lanes. This was attributed to the enhanced turbulence of downflows. But later Hoekzema et al. (1998) found no difference between oscillations above the granules and intergranular lanes. In this work we re-examine the links between the 5-minute oscillations and granulation using observations of the Fe I 5324 Å line obtained with high spatial and temporal resolution. In contradiction to the previous studies we show that oscillations above the brightest granules as well as above the darkest intergranular lanes occur with the smaller amount of radiative energy losses. This causes the amplitude amplification with the contrast of granulation.


Phase Shift Mach Number Velocity Oscillation Turbulent Convection Intensity Oscillation 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.


  1. Brown, T.M.: 1991, ApJ 371, 396–401.ADSCrossRefGoogle Scholar
  2. Deubner, P.L.: 1990, in I.O. Stenflo (ed.), Solar photosphere: Structure, Convection and Magnetic Fields, Kluwer Academic Publishers, Dordrecht, 217–228.CrossRefGoogle Scholar
  3. Espagnet, O., Muller, R., Roudier, T., Mein, P., Mein, N., and Malherbe, J.M.: 1996,A&A 313, 297–305.ADSGoogle Scholar
  4. Goldreich, P. and Kumar, P.: 1988, ApJ 326, 462–468.ADSCrossRefGoogle Scholar
  5. Goldreich, P., Murray, N., and Kumar, P.: 1994, ApJ 424, 466–479.ADSCrossRefGoogle Scholar
  6. Hoekzema, N.M., Rutten, R.J., Brandt, P.N., and Shine, R.A.: 1998, A&A 329, 276–290.ADSGoogle Scholar
  7. Kostik, R. and Shchukina, N.: 1999, Sov. Astron. Letters 25, No. 9, in press.Google Scholar
  8. Kostik, R.I., Shchukina, N.G., and Khomenko, E.V.: 1999, in Proceedings of the 9th European Meeting on Solar Physics: Magnetic Fields and Solar Processes, in press.Google Scholar
  9. Rimmele, T.R., Goode, P.R., Harold, E., and Stebbins, R.T.: 1995, Ap J 444, L119–L122.ADSCrossRefGoogle Scholar
  10. Shchukina, N.G. and Trujillo Bueno, J.: 1998, Kinematika i Fizika Nebesnich Tel 14,No. 4, 242.Google Scholar
  11. Tanenbaum, A.S., Wilcox, J.M., and Frasier, E.N.: 1969, Solar Phys. 9, 328–342.ADSCrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media Dordrecht 2001

Authors and Affiliations

  • E. V. Khomenko
    • 1
  1. 1.Main Astronomical ObservatoryNational Academy of SciencesKiev 22Ukraine

Personalised recommendations