ALMA Observations of Solar Spicules in a Polar Coronal Hole

We report observations of solar spicules at millimeter wavelengths (mm- λ ) using the Atacama Large Millimeter/submillimeter Array (ALMA). These are supplemented by observations in optical, ultraviolet (UV), and extreme ultraviolet (EUV) wavelengths. The observations were made on 2018 December 25 of the northern polar coronal hole. ALMA obtained time-resolved imaging observations at wavelengths of 3 mm (100 GHz; 2 s cadence) and 1.25 mm (239 GHz; ≈2 minutes cadence) with an angular resolution of 2 $\mathop{.}\limits^{\unicode{x02033}}$ 2 × 1 $\mathop{.}\limits^{\unicode{x02033}}$ 3 and 1 $\mathop{.}\limits^{\unicode{x02033}}$ 5 × 0 $\mathop{.}\limits^{\unicode{x02033}}$ 7, respectively. Spicules observed at mm- λ are easily seen low in the chromosphere whereas spicules in UV bands are seen to extend higher. The spicules observed at mm- λ are seen in absorption against coronal EUV emission, allowing us to estimate the column depth of neutral hydrogen. Spicular emission at mm- λ , due to thermal free–free radiation, allows us to estimate the electron number density as a function of height. We find that spicule densities, inferred from the mm- λ data are uniquely insensitive to assumptions regarding the temperature of plasma in spicules. We suggest that the upward mass flux carried by spicules is unlikely to play a significant role in the mass budget of the solar corona and solar wind, and the transport of hot material into the corona by spicules may not play a significant role in coronal heating. However, the possibility that electric currents, fast kink and torsional waves, or other wave modes carried by spicules may play a role in transporting energy into the solar corona cannot be excluded.