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We analyze solar quiescent prominence bubble characteristics and instabilitydynamics using Hinode/Solar Optical Telescope (SOT) data. We measure bubbleexpansion rate, prominence downflows, and the profile of the boundary layerbrightness and thickness as a function of time. The largest bubble analyzedrises into the prominence with a speed of about 1.3 km/s until it isdestabilized by a localized shear flow on the boundary. Boundary layerthickness grows gradually as prominence downflows deposit plasma onto thebubble with characteristic speeds of 20 - 35 km/s. Lateral downflows initiatefrom the thickened boundary layer with characteristic speeds of 25 - 50 km/s,"draining" the layer of plasma. Strong shear flow across one bubble boundaryleads to an apparent coupled Kelvin-Helmholtz Rayleigh-Taylor (KH-RT)instability. We measure shear flow speeds above the bubble of 10 km/s and inferinterior bubble flow speeds on the order of 100 km/s. Comparing the measuredgrowth rate of the instability to analytic expressions, we infer a magneticflux density across the bubble boundary of ~10^{-3} T (10 gauss) at an angle of~70 degrees to the prominence plane. The results are consistent with thehypothesis that prominence bubbles are caused by magnetic flux that emergesbelow a prominence, setting up the conditions for RT, or combined KH-RT,instability flows that transport flux, helicity, and hot plasma upward into theoverlying coronal magnetic flux rope.

astrophysical journal/the astrophysical journal

Quiescent prominence dynamics observed with the Hinode Solar Optical  Telescope . II. Prominence Bubble Boundary Layer Characteristics and the  Onset of a Coupled Kelvin-Helmholtz Rayleigh-Taylor Instability