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Filaments and coronal holes, two principal features observed in the solarcorona are sources of space weather variations. Filament formation is closelyassociated with polarity inversion lines (PIL) on the solar photosphere whichseparate positive and negative polarities of the surface magnetic field. Theorigin of coronal holes is governed by large-scale unipolar magnetic patches onthe photosphere from where open magnetic field lines extend to the heliosphere.We study properties of filaments, PILs and coronal holes in solar cycles 20,21, 22 and 23 utilizing the McIntosh archive. We detect a prominent cyclicbehavior of filament length, PIL length, and coronal hole area with significantcorrespondence with the solar magnetic cycle. The spatio-temporal evolution ofthe geometric centers of filaments shows a butterfly-like structure anddistinguishable pole-ward migration of long filaments during cycle maxima. Weidentify this rush to the poles of filaments to be co-temporal with theinitiation of polar field reversal as gleaned from Mount Wilson and WilcoxSolar Observatory polar field observations and quantitatively establish theirtemporal correspondence. We analyze the filament tilt angle distribution toconstrain their possible origins. Majority of the filaments exhibit negativeand positive tilt angles in the northern and the southern hemispheres,respectively -- strongly suggesting that their formation is governed by theoverall large-scale magnetic field distribution on the solar photosphere andnot by the small-scale intra-active region magnetic field configurations. Wealso investigate the hemispheric asymmetry in filaments, PILs, and coronalholes. We find that the hemispheric asymmetry in filaments and PILs arepositively correlated -- whereas coronal hole asymmetry is uncorrelated -- withsunspot area asymmetry.

The Association of Filaments, Polarity Inversion Lines, and Coronal Hole Properties with the Sunspot Cycle: An Analysis of the McIntosh Database