Spicules, mass transfer, oscillations, and the heating of the corona

Details Spicules, mass transfer, oscillations, and the heating of the corona Spicules, mass transfer, oscillations, and the heating of the corona

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh13c..02p&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH13C-02

Mathematics

Logic

7507 Chromosphere, 7509 Corona, 7524 Magnetic Fields, 7546 Transition Region, 7549 Ultraviolet Emissions

Scientific paper

The mass moving in chromospheric spicules is enough to replace the corona in a brief time, so understanding the dynamics of spicules is important for understanding the support and heating of the solar corona. We have undertaken a program involving simultaneous high-resolution observations in various chromospheric visible lines (H-alpha, Ca II H, and G-band, as well as Dopplergrams) using the Swedish Solar Telescope on La Palma, ultraviolet chromospheric, transition-region, and coronal lines (Fe IX/X 171 A, Lyman-alpha 1216 A, and continuum/C I/C IV 1600 A) using NASA's TRACE, and ultraviolet chromospheric and transition-region lines (Si II 1533, C IV 1548, and Ne VIII 770) using SUMER on SOHO. Our first coordinated observing run, in May 2004, yielded a variety of images that are under study, especially for the morphological statistics and dynamics of spicules. The energy transfer through the chromosphere is relevant to the overlapping investigation of coronal heating through rapid (1Hz range) oscillations of coronal loops as observed at total eclipses by Williams College expeditions. This research is supported by NASA grant number NNG04GK44G to Williams College. TRACE analysis at SAO is supported by a contract from Lockheed Martin. SOHO is a project of international cooperation between ESA and NASA.

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