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Figure 1:
A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperatures as a function of
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Figure 2:
A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperatures as a function of
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Figure 3:
A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperature as a function of
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Figure 4:
The geometry used for the Rybicki (1971) method of radiative transfer. The rays are distributed over the core in equal steps of 0.1 in ![]() |
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Figure 5: A comparison of the temperature structures for two solar atmospheric models, both using the ATLAS_ODF code. The solid line used the Rybicki (1971) method to compute the radiative transfer, and the dashed line used the original ATLAS9 integral equation method. |
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Figure 6:
A comparison of the temperature structures for two solar atmospheric models. The top panel displays the temperatures as a function of
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Figure 7:
A comparison of the temperature structures of two red giant atmospheric models. The top panel displays the temperatures as a function of
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Figure 8:
A comparison of the structures of two spherical red giant atmospheric models, both equivalent to
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Figure 9:
A comparison of the temperature structures of an SATLAS_ODF atmosphere (solid line) with the
structure of a model from the NG-giant grid computed with the
PHOENIX code (dashed line). The SATLAS
model has the atmospheric parameters
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Figure 10:
A comparison of the temperature structures of an
SATLAS_ODF atmosphere (solid line) with a
spherical MARCS model (dashed line).
The SATLAS model has the atmospheric parameters
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