Motions in solar magnetic tubes. II: The oscillations.
Abstract
The method of Giovanelli and Brown (1977) has been used with a variety of spectral lines 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 ±0.27 km s−1 in Fe I 5166 Å (a line of low origin) to ±0.75 km s−1 in Hα. 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 Hα.
- Publication:
-
Solar Physics
- Pub Date:
- September 1978
- DOI:
- 10.1007/BF00154931
- Bibcode:
- 1978SoPh...59...49G
- Keywords:
-
- Chromosphere;
- Magnetic Disturbances;
- Photosphere;
- Solar Atmosphere;
- Solar Magnetic Field;
- Gas Dynamics;
- H Alpha Line;
- Oscillations;
- Solar Spectra;
- Stellar Structure;
- Velocity Measurement;
- Zeeman Effect;
- Solar Physics;
- Atmosphere;
- Shock Wave;
- Spectral Line;
- Phase Difference;
- Common Mechanism;
- Oscillations:Sun;
- Solar Magnetic Regions: Motions