Solar Physics
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The spiral configuration of sunspot magnetic fields
Solar Physics - Tập 53 - Trang 3-13 - 1977
Distributions of circularly and linearly polarized intensities are computed using an analytical magnetic field model for an isolated sunspot, and these intensity distributions are compared with observed intensities in all Stokes parameters in the λ 5250 line measured with the Marshall Space Flight Center's vector magnetograph. The qualitative agreement between measured and calculated linearly pola......
New possibilities of non-eclipse observations of the solar K-corona with liquid-mirror telescopes
Solar Physics - - 1991
Attempts to infer the density distribution in the outer part of the Sun from p-mode oscillations spectrum
Solar Physics - Tập 133 - Trang 117-125 - 1991
We devise two asymptotic inversion methods of inferring the density distribution in the outer part of the Sun from the p-mode frequency spectrum of the Sun. One of them is based on an integral equation of nonlinear inversion, while the other reduces the problem to a linear form which is derived from comparison of the observed eigenfrequencies of the true Sun and the theoretical eigenfrequencies of......
Energy balance in cool quiescent prominences
Solar Physics - Tập 19 - Trang 401-413 - 1971
The energy balance for cool quiescent prominences is examined using a 6000 km, 6000 K isothermal slab model prominence with a density gradient dictated by a modified Kippenhahn-Schlüter model. The model is irradiated from both sides by the coronal, chromospheric, and photospheric radiation fields. The radiative transfer problem is solved in detail for the Lyman continuum and Hα to determine the ne......
The effect of atomic polarization on early estimates of prominence magnetic field strengths
Solar Physics - Tập 215 - Trang 295-305 - 2003
In this paper we present our results of the application of the magnetograph formula to synthetic Stokes V profiles in prominences. We investigate both the Zeeman and atomic-polarization signatures within the V profile and question why previous attempts to determine magnetic field strength, on average, were correct, even if the magnetograph formula does not apply in general.
Observations and comments for the solar event of 24 October, 1969
Solar Physics - Tập 24 - Trang 405-410 - 1972
Observations of the flare of October 24, 1969 by Zirin et al. (1971) Solar Phys.
19, 463, are given with accompanying graphs of XUV emissions from satellites and four microwave radio emissions from Sagamore Hill Observatory. This event provides an excellent example of the development of two types of radio spectra within the same center and similar profiles for the hard X-ray burst and the 8800 MHz......
Why Do Temperature and Velocity Have Different Relationships in the Solar Wind and in Interplanetary Coronal Mass Ejections?
Solar Physics - Tập 257 - Trang 169-184 - 2009
In-situ observations of the solar wind (SW) show temperature increasing with the wind speed, whereas such a dependence is not observed in interplanetary coronal mass ejections (ICMEs). The aim of this paper is to understand the main origin of this correlation in the SW and its absence in ICMEs. For that purpose both the internal-energy and momentum equations are solved analytically with various ap......
Deka-keV X-ray emission associated with the onset of radio noise storms
Solar Physics - Tập 167 - Trang 333-348 - 1996
Radio noise storms show that suprathermal electrons (a few tens of keV) are present in the vicinity of active regions during several hours or even a few days. Where and how these electrons are energized is not yet well known. A flare-like sudden energy release in the active region is in general observed at the onset of noise storms, either as a fully developed flare or, more often, as a soft X-ray......
Sunspot Observations at the Eimmart Observatory: Revision and Supplement
Solar Physics - Tập 298 - Trang 1-26 - 2023
Digital images of sunspot drawings of the archives of Georg Christoph Eimmart stored at the National Library of Russia, St. Petersburg, are analyzed to obtain sunspot-group numbers and sunspot areas as well as heliographic positions. Overall, more than a hundred drawings were processed. The impact of drawing and reproduction uncertainties and the aims of historical observations are considered. The......
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