Abstract:
Solar prominences are structures of importance because of their role in polar field reversal.
We study the long-term variation of the time latitude distribution of solar prominences in this article. To
accomplish this, we primarily used the digitized disc-blocked Ca K spectroheliograms as recorded from
Kodaikanal Solar Observatory for the period of 1906–2002. For improving the data statistics we included
full disc H
images from Meudon and Kanzelhohe Observatory, which are available after 1980. We
developed an automated technique to identify the latitudinal locations of prominences in daily images
from all three data sets. Derived time-latitude distribution clearly depicted poleward migration of
prominence structures for 10 cycles (15–24). Unlike previous studies, we separated the rate of poleward
migration during onset and near pole, using piece-wise linear fits. In most cases, we found acceleration
in poleward migration with the change occurring near ±70
latitudes. The derived migration rates for
such large number of solar cycles can provide important inputs toward understanding polar field
buildup process.
