Titlebook: Coronal Magnetometry; Steven Tomczyk,Jie Zhang,Timothy Bastian Book 2014 Springer Science+Business Media New York 2014 Embedded Systems.Ha

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Hyperasymptotic Perturbation Theoryn lines contain information about the magnetic field, and to access this information either a forward or an inversion method must be used. We study three coronal magnetic configurations that are applicable to polar-crown filament cavities by doing forward calculations to produce synthetic polarizati

Chivalrous

J. Litva,A. Sandhu,K. Cho,T. Lo, CoMP observations provide high-cadence image sequences of the coronal line intensity, Doppler shift, and line width simultaneously over a large field of view. By studying the Doppler shift and line width we may explore more of the physical processes of the initiation and propagation of coronal mas

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先鋒派

Vincent E. Rubatzky,Mas Yamaguchiegion were taken into account. The north–south asymmetry of the magnetic fluxes was considered as well as the imbalance between positive and negative fluxes. The north–south asymmetry displays a regular alternation of the dominant hemisphere during the solar cycle: the northern hemisphere dominated

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Allodynia

Vincent E. Rubatzky,Mas Yamaguchibased on semi-empirical models locate this point at about 500?km above the photosphere. The consistency of these models has been tested by means of millimeter to infrared observations. We show that variations of the theoretical radial temperature profile near the temperature minimum impact the brigh

cleaver

Vincent E. Rubatzky,Mas Yamaguchiressed magnetic activity spanning the second half of the 17th century. This spectral reconstruction is based on an extension of the Monte Carlo Solar Spectral Irradiance Model (MOCASSIM). The new version of the model, documented in this paper, extends its spectral range down to 150?nm, its temporal

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Nitin R. Mangalvedhe,Jeffrey H. ReedEREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R. using a tomography method. With this, we qualitatively deduced structure