Astronomy and Astrophysics – Astronomy
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.0702s&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #07.02; Bulletin of the American Astronomical Society, Vol. 24, p.738
Astronomy and Astrophysics
Astronomy
Scientific paper
We present the dynamical evolution of spicules seen on the solar disk and the relationship between the spicule formation and Hα bright point at its footpoint. We used filtergrams in Hα -0.65 Angstroms, 0.0, and +0.65 Angstroms, (passband = 0.25 Angstroms) obtained at BBSO on Sep. 16, 1991, with the OSL CCD camera. The observations were made in a region of enhanced network for one and half hours. The resolution was 0.4 arcsec/pixel. The time resolution for the filtergrams of same wavelength was about 20 sec. These filtergrams were carefully registered with a cross-correlation technique, in order to follow the time evolution of fine structures. We investigated both proper motions and line-of-sight Doppler velocities of spicules; the latter were obtained from the subtraction of Hα -0.65 from +0.65 filtergrams. About 2/3 of the spicules could be traced through up and down phases. For most short-lived spicules, both their apparent motions and Doppler velocities indicate that the motion of a spicule is real and it follows nearly a ballistic trajectory. For some long-lived spicules, we can see periodic rising motion. In these cases, we can see the lower part of the spicule showing downward motion even in the rising phase. The bright points, which are prominent in Hα blue wing, tend to appear or reach their maximum intensity at about the maximum phase of spicules, and to be accompanied with downward motions. It is likely that the Hα bright point does not initiate the spicule formation but rather it appears as a by-products of the spicule formation. These results seem to suggest that the spicules are generated by an impulsive upward force on the chromosphere such as a shock wave propagating upward, and its seed perturbation might take place at a layer deeper than the chromosphere, or might be a kinematic process with less heating if it occurs in the chromosphere.
Suematsu Yoshinori
Wang Hai-Hong
Zirin Harold
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