Umbral Models with Enhanced Continuum Opacity

Details Umbral Models with Enhanced Continuum Opacity Umbral Models with Enhanced Continuum Opacity

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....95..229s&link_type=abstract

Astronomy and Astrophysics, Vol. 95, P. 229, 1981

Astronomy and Astrophysics

Astrophysics

7

Scientific paper

Umbral models based on the assumption of an additional continuum opacity (Zwaan, 1974; Kollatschny et al., 1979: M4) are compared with model M3 by Stellmacher and Wiehr (1975) which is based on the standard continuum opacity.
The strong Fe 4063.6 lime is observed in several sunspot umbrae. An upper limit of parasitic light is estimated on the basis of vanishing Fe+ limes in umbrae. It is shown that the wings of the so corrected Fe 4063.6 line cannot be reproduced by model M3. The recent model M4 requires an opacity enhancement q4063 = 2.5 ± 0.2; Zwaan's model needs q4063 = 2.7. The relative umbral intensity at λλ4063 is obtained to 0.026 Iphot using model M4 with q4063 = 2.5. Assuming line haze as origin for qλ the true continuum would amount to 0.065 Iphot. Measurements of umbral continuum contrasts near the peaks of the opacity curve q(λ) suggested by Gaur et al. (1979) do not show the marked contrast depressions predicted and are thus at variance with the idea that the additional opacity arises from electronic transitions of CN, CaB, MgH and TiO molecules.

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