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Coronal plumes are bright magnetic funnels found in quiet regions (QRs) andcoronal holes (CHs). They extend high into the solar corona and last from hoursto days. The heating processes of plumes involve dynamics of the magnetic fieldat their base, but the processes themselves remain mysterious. Recentobservations suggest that plume heating is a consequence of magnetic fluxcancellation and/or convergence at the plume base. These studies suggest thatthe base flux in plumes is of mixed polarity, either obvious or hidden in SDOHMI data, but do not quantify it. To investigate the magnetic origins of plumeheating, we select ten unipolar network flux concentrations, four in CHs, fourin QRs, and two that do not form a plume, and track plume luminosity in SDO AIA171 A images along with the base flux in SDO HMI magnetograms, over each fluxconcentrations lifetime. We find that plume heating is triggered whenconvergence of the base flux surpasses a field strength of 200 to 600 G. Theluminosity of both QR and CH plumes respond similarly to the field in the plumebase, suggesting that the two have a common formation mechanism. Our examplesof non-plume-forming flux concentrations, reaching field strengths of 200 G fora similar number of pixels as for a couple of our plumes, suggest that acritical field might be necessary to form a plume but is not sufficient for it,thus, advocating for other mechanisms, e.g. flux cancellation due to hiddenopposite-polarity field, at play.

Critical magnetic field strengths for solar coronal plumes in quiet regions and coronal holes?