High-resolution spectroscopy of active regions. I - Observing procedures

Details High-resolution spectroscopy of active regions. I - Observing procedures High-resolution spectroscopy of active regions. I - Observing procedures

Jan 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...95....3z&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 95, Jan. 1985, p. 3-14.

Physics

39

Astronomical Spectroscopy, Line Spectra, Solar Activity, Solar Spectra, Sunspots, Field Strength, Fine Structure, High Resolution, Solar Magnetic Field, Umbras

Scientific paper

An observing program designed to obtain spectra of sunspots, pores, and other features in active regions using the Vacuum Tower Telescope and Echelle Spectrograph at Sacramento Peak Observatory is described. The spectral lines used in the study were especially chosen to allow pointed studies of fine structure in the intensity distribution, and in the velocity and magnetic fields in the photospheric levels of active regions, and to relate this structure to chromospheric observations made in the Ca II H line. The capacities of the observing program are demonstrated by two examples: umbral fine structure, and an emerging active region. Although the umbral spectrograms resolve the brightness structure down to less than one arc sec, no clear-cut relations were found in the spatial variations of brightness, magnetic field strength and line-of-sight velocity across the umbral structure. In the emerging active region several processes are observed in their relationship: the rising and draining of an arch-filament system, the convective collapse of flux tubes, and the growth of a sunspot pore by coalescing fluxtubes.

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