Motions in solar magnetic tubes. II - The oscillations

Details Motions in solar magnetic tubes. II - The oscillations Motions in solar magnetic tubes. II - The oscillations

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...59...49g&link_type=abstract

Solar Physics, vol. 59, Sept. 1978, p. 49-64.

Physics

34

Chromosphere, Magnetic Disturbances, Photosphere, Solar Atmosphere, Solar Magnetic Field, Gas Dynamics, H Alpha Line, Oscillations, Solar Spectra, Stellar Structure, Velocity Measurement, Zeeman Effect

Scientific paper

The method of Giovanelli and Brown (1977) is used to study oscillating longitudinal gas velocities inside solar magnetic elements. Oscillations have been found inside all elements observed, the amplitudes increasing with height from typically plus or minus 0.27 km/sec in Fe I 5166 A to plus or minus 0.75 km/sec in H alpha. Simultaneous observations in pairs of lines show that a given disturbance occurs later with height, so that disturbances propagate outwards. The period is typically 5 min in all lines originating near or below Mg b1, but is about 3 min in H alpha.

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