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(Abridged) Classical Be stars occasionally transition from having a gaseouscircumstellar disk (''Be phase'') to a state in which all observationalevidence for the presence of these disks disappears (''normal B-star phase'').We present one of the most comprehensive spectropolarimetric views to date ofsuch a transition for two Be stars, pi Aquarii and 60 Cygni. 60 Cyg's disk lossepisode was characterized by a monotonic decrease in emission strength over atime-scale of 1000 days, consistent with the viscous time-scale of the disk,assuming alpha is 0.14. pi Aqr's disk loss was episodic in nature and occurredover a time-scale of 2440 days. An observed time lag between the behavior ofthe polarization and H-alpha in both stars indicates the disk clearingproceeded in an ''inside-out'' manner. We determine the position angle of theintrinsic polarization to be 166.7 +/- 0.1 degrees for pi Aqr and 107.7 +/- 0.4degrees for 60 Cyg, and model the observed polarization during the quiescentdiskless phase of each star to determine the interstellar polarization alongthe line of sight. Minor outbursts observed during the quiescent phase of eachstar shared similar lifetimes as those previously reported for mu Cen,suggesting that the outbursts represent the injection and subsequent viscousdissipation of individual blobs of material into the inner circumstellarenvironments of these stars. We also observe deviations from the mean intrinsicpolarization position angle during polarization outbursts in each star,indicating deviations from axisymmetry. We propose that these deviations mightbe indicative of the injection (and subsequent circularization) of new blobsinto the inner disk, either in the plane of the bulk of the disk material or ina slightly inclined (non-coplanar) orbit.

Disk Loss and Disk Renewal Phases in Classical Be Stars I: Analysis of Long-Term Spectropolarimetric Data