Abstract Solar prominences are the most prominent large-scale structures observed above the solar limb in emission in chromospheric lines but in absorption in coronal lines. At the bottom of prominences often appears a bubble, with plumes occasionally rising from the prominence–bubble interface. The plumes may potentially play an important role in the mass supply and thermodynamic evolution of prominences, but their nature and generation mechanism are elusive. Here we use the high-resolution H α observations obtained by the New Vacuum Solar Telescope to investigate a quiescent prominence with bubbles and plumes on 2022 November 8. Within an interval of about 2 hr, enhanced spicular activity disturbs the prominence–bubble interface, producing bursts of small-scale plumes rising through the prominence. Characterized by clustered spicules jetting at higher speeds (sometimes exceeding the typical chromospheric Alfvén speed) and longer lifetime (over 15 minutes), the enhanced spicular activity differs markedly from regular spicules. We hence conjecture that the enhanced spicular activity may drive shock waves, which trigger the magnetic Richtmyer–Meshkov instability at the prominence–bubble interface, leading to the formation of small-scale plumes. These observations provide evidence that the enhanced spicular activity plays a potentially important role in the dynamic evolution of bubbles and plumes, thereby participating in the mass supply of solar prominences.
Wang et al. (Tue,) studied this question.