Abstract
Solar spicules are known as one of the most prevalent small-scale dynamical phenomena in the solar chromosphere, and are likely to make a considerable contribution to coronal mass supply. In order to understand the dynamical behavior of spicules, we analyzed high resolution filtergrams in Hα line center and wings taken at an enhanced network region near disk center (Suematsu et al. 1995), and found: (1) About 80% of the spicules, many of which were multiple events, could be traced through up and down phase; there were some spicules which were seen in the upward phase but barely visible in the downward phase, and vice versa. (2) Both proper motions and line-of-sight Doppler signals indicate that the spicules are phenomena of true material motion; the motions of the tops of some spicules are well represented by an inclined ballistic trajectory with an initial ejection velocity of about 40 km/sec. (3) Most of bright points in the Hα blue wing tend to appear at the base of spicules at their peak extension and in the falling phase; they are barely seen in the Hα red wing.
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References
Beckers, J.M. 1964, Ph.D. Thesis, Utrecht.
Suematsu, Y., Wang, H, and Zirin, H., 1995, Astrophys. J., 450, 411
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© 1996 Kluwer Academic Publishers
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Suematsu, Y. (1996). High Resolution Observation of Solar Spicules and their Kinematic Modelling. In: Uchida, Y., Kosugi, T., Hudson, H.S. (eds) Magnetodynamic Phenomena in the Solar Atmosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0315-9_86
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DOI: https://doi.org/10.1007/978-94-009-0315-9_86
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-6627-3
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