The height variation of sunspot umbral dots

Details The height variation of sunspot umbral dots The height variation of sunspot umbral dots

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...287l...1w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 287, no. 1, p. L1-L4

Astronomy and Astrophysics

Astrophysics

12

Brightness Distribution, Iron, Line Spectra, Nickel, Silicon, Stellar Models, Sunspots, Umbras, Doppler Effect, Solar Magnetic Field, Spectrographs, Zeeman Effect

Scientific paper

The visibility of sunspot umbral dots is measured in different spectral lines that are insensitive to Zeeman spliting. At the formation height of the Fe 5576 line core, the dot to inter-dot brightness ratio amounts to about 30% of that at the continuum level. It further drops to less than 15% at the formation height of the Fe 5434 line core, that is expected to correspond to the temperature minimum. A contrast of 50% occurs at about 130 km height where the inner wings of Fe 5576 (Delta lambda - 45 mA) and the outer wings of Fe 5434 (Delta lambda = 75 mA) are formed. Simultaneously observed Ni and Si lines from very deep layers show the same brightness excess as the adjacent continuum. Neither systematic Doppler shifts nor line asymmetries are found in umbral dots with respect to their inter-dot-neighborhood.

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