Analysis of the solar magnesium lines

Journal Article · Tue Apr 01 04:00:00 EST 1980 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157865· OSTI ID:5273743

Heasley, J N; Allen, M S

The observed quiet-Sun profiles for a number of Mg I and II lines are compared with theoretical spectra computed for two upper-photosphere lower-chromosphere models published by Ayres and Linsky. Both the Mg I and the Mg II resonance line wings, observed with the University of Hawaii Echelle Rocket Spectrographs, favor a model with a higher temperature in the upper photosphere than required to match the visible region lines lambdalambda4571 and 5172. Neither model atmosphere reproduces the observed shapes in the cores of the strong lines or the limb darkening of the 4571 A intercombination line. The wings of the ultraviolet lines in plages can be reproduced either with a mean one-component atmosphere or by a two-component model with an ad hoc filling factor.

• Research Organization: Institute for Astronomy, University of Hawaii
• OSTI ID: 5273743
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 237:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ALKALINE EARTH METALS
ATMOSPHERES
ATOMIC IONS
CHARGED PARTICLES
CHROMOSPHERE
ELEMENTS
ENERGY SPECTRA
EQUILIBRIUM
IONS
LTE
MAGNESIUM
MAGNESIUM IONS
MATHEMATICAL MODELS
MATHEMATICS
METALS
NUMERICAL ANALYSIS
PHOTOSPHERE
PLAGES
SOLAR ACTIVITY
SOLAR ATMOSPHERE
SPECTRA
STAR MODELS
TEMPERATURE DISTRIBUTION
ULTRAVIOLET SPECTRA
VISIBLE SPECTRA