Sdo/AIa Detection of Solar Prominence Formation Within a Coronal Cavity

We report the first analyses of SDO /AIA observations of the formation of a quiescent polar crown prominence in a coronal cavity. The He ii 304 Å (log T max ∼ 4.8 K) data show both the gradual disappearance of the prominence due to vertical drainage and lateral transport of plasma followed by the formation of a new prominence 12 hr later. The formation is preceded by the appearance of a bright emission "cloud" in the central region of the coronal cavity. The peak brightness of the cloud progressively shifts in time from the Fe xiv 211 Å channel, through the Fe xii 193 Å channel, to the Fe ix 171 Å channel (log T max ∼ 6.2, 6.1, 5.8 K, respectively) while simultaneously decreasing in altitude. Filter ratio analysis estimates the initial temperature of the cloud to be approximately log T ∼ 6.25 K with evidence of cooling over time. The subsequent growth of the prominence is accompanied by darkening of the cavity in the 211 Å channel. The observations imply prominence formation via in situ condensation of hot plasma from the coronal cavity, in support of our previously proposed process of magnetothermal convection in coronal magnetic flux ropes.