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Sunspot umbral oscillations in Mgii k

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Abstract

Time series observations of the profile of the Mgii k line λ2795.52 have been obtained in five sunspots with the Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission. The three sunspots with umbrae larger than the 3″ × 3″ pixel size show significant oscillations in integrated line intensity and line centroid, with frequencies in the range 5.29–7.55 mHz (periods of 132–190 s).

The frequencies of significant peaks in average umbral power spectra agree well with the frequencies of the three lowest-frequency transmission peaks predicted by a model of resonant transmission of acoustic waves. If radiative delays are unimportant, and the line centroid can be interpreted straightforwardly as a Doppler shift, the measured velocity-intensity phase differences indicate the superposition of upward- and downward-propagating waves in the umbral chromosphere; this is further evidence for the resonant transmission model.

A single, quiet Sun time series of k core profiles yields power spectra and a phase difference consistent with the existence of a chromospheric p-mode.

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Authors and Affiliations

  1. Solar Maximum Mission Experimenters' Operations Facility, and Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, 20771, Greenbelt, MD, U.S.A.

    Joseph B. Gurman

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  1. Joseph B. Gurman
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This work is dedicated to his memory.

The SMM data used in this work were available only because of the repair of the SMM spacecraft by the crew of Challenger on mission 41-C. The pilot for that mission and the commander of Challenger's last mission was Francis R. Scobee.

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Gurman, J.B. Sunspot umbral oscillations in Mgii k. Sol Phys 108, 61–75 (1987). https://doi.org/10.1007/BF00152077

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  • DOI: https://doi.org/10.1007/BF00152077

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