Introduction {#intro}
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Quiescent prominences are large clouds of relatively cool plasma supported against gravity by their magnetic field. It is known that the temperature of quiescent prominences is approximately 8000K [@TH1995] and density $\sim 10^{11}$cm$^{-3}$ [@HIR1986] which is a decrease and increase of approximately two orders of magnitude respectively from the surrounding corona. Using this value for the temperature the pressure scale height can be calculated as $\Lambda \sim 300$km, which is approximately $2$ orders of magnitude less than the characteristic height of a quiescent prominence [$\sim 25$Mm @TH1995]. There are many reviews that describe the current understanding of the nature of quiescent prominences [see, for example, @TH1995; @LAB2010; @MAC2010].

Observations by the Solar Optical Telescope [SOT; @TSU2008] on the Hinode satellite [@KOS2007] have shown that on very small scales quiescent prominences are highly dynamic and unstable phenomena. [@BERG2008] and [@BERG2010] reported dark upflows that propagate from large ($\sim 10$Mm in size) bubbles that formed at the base of some quiescent prominences, through a height of approximately $10$Mm before dispersing into the background prominence material. An example of these plumes is shown in Figure \[prom\]. Observations by [@BERG2011] show that the bubble and plumes have a minimum temperature of 