Oscillatory motions in sunspots
β Scribed by J. M. Beckers; R. B. Schultz
- Publisher
- Springer
- Year
- 1972
- Tongue
- English
- Weight
- 601 KB
- Volume
- 27
- Category
- Article
- ISSN
- 0038-0938
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β¦ Synopsis
We observe vertical velocity oscillations in some sunspot umbrae with periods of about 180 s and peak to peak amplitudes up to 1 km s -1. These oscillations are not visible in either the line depth, line width or the continuum intensity. No correlation seems to exist between the occurence of these oscillations and the presence of the chromospheric umbral flashes (Solar Phys. 7, 351, 1069). In the spot penumbra there is an indication of a long period oscillation, the period increasing from about 300 s in the inner penumbra to nearly 1000 s at the penumbra-photosphere boundary. An attempt has been made to interpret these oscillations in terms of gravity or acoustic waves, travelling along the magnetic field lines, taking into account the variation of scale height and magnetic field direction across the sunspot.
π SIMILAR VOLUMES
The Evershed motion is postulated as a steady, laminar flow of material along a limiting field line which separates the umbral magnetic field from the penumbral. Assuming that the Evershed flow starts from the spot-base with a velocity which is adequate to carry the convective flux at that level, th
Different types of oscillatory motions were detected in the late phases of eruption of a prominence. We found oscillations of the prominence axis and diameter with periods of 4.3 and 9.1 min, corresponding to the eigenmodes m = 4 and m = 8 with a damping factor 4.6 x 10 -3 s -1. A period about 4.5
It is confirmed that the penumbral bright grains are moving towards the sunspots umbra. We find different prope r motions of 0.08 to 0.33 km s -1 for different penumbrae and different reduction methods. The lifetimes of these bright grains are about 1.5 to 3 hr depending on the position in the penum
We have measured the motion of facular points and granules in the same region near a decaying sunspot. It is found that both features move away across the moat surrounding the sunspot. The mean speed of facular points is larger than that of granules: 0.65 km s -~ and 0.4 km s -1, respectively. These