Abstract
Semi-empirical models of solar faculae, cospatial with strong photospheric magnetic fields, have been constructed from continuum observations. The center-to-limb contrast of the various models was computed taking into account their geometrical shape. The adopted model whose horizontal size was taken to be 750 km, indicates that, in field regions, the temperature begins to rise outwards at z ≈ -125 km (above τ5000 = 1) and that the extrapolated temperature at z ≈ -400 km is about 1500 K above that of the undisturbed atmosphere; the electron density is higher by a factor of about 30.
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Chapman, G.A. On the physical conditions in the photospheric network: An improved model of solar faculae. Sol Phys 14, 315–327 (1970). https://doi.org/10.1007/BF00221317
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DOI: https://doi.org/10.1007/BF00221317