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......
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......
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......
Solar rotation, 1966–1978
Solar Physics - Tập 61 - Trang 219-231 - 1979
Photospheric and chromospheric spectroscopic Doppler rotation rates for the full solar disk are analyzed for the period July, 1966 to July, 1978. An approximately linear secular increase of the equatorial rate of 3.7% for these 12 years is found (in confirmation of Howard, 1976). The high latitude rates above 65 ° appear to vary with a peak-to-peak amplitude of 8%, or more, phased to the sunspot c......
Validation of the CME Geomagnetic Forecast Alerts Under the COMESEP Alert System
Solar Physics - Tập 292 - Trang 1-14 - 2017
Under the European Union 7th Framework Programme (EU FP7) project Coronal Mass Ejections and Solar Energetic Particles (COMESEP,
), an automated space weather alert system has been developed to forecast solar energetic particles (SEP) and coronal mass ejection (CME) risk levels at Earth. The COMESEP aler......
Polarity Reversal Time of the Magnetic Dipole Component of the Sun in Solar Cycle 24
Solar Physics - Tập 283 - Trang 247-252 - 2013
The Sun’s general magnetic field has shown polarity reversal three times during the last three solar cycles. We attempt to estimate the upcoming polarity reversal time of the solar magnetic dipole by using the coronal field model and synoptic data of the photospheric magnetic field. The scalar magnetic potential of the coronal magnetic field is expanded into a spherical harmonic series. The long-t......
Fine structure of a very bright active region at a wavelength of 2.8 cm
Solar Physics - Tập 37 - Trang 395-402 - 1974
The radio structure of the active region McMath 11976 has been investigated with an east-west resolution of 16″ at a wavelength of 2.8 cm. Six bright components were found with angular sizes of the order of 20″. From the position measure of these components in two following days the heights above the solar photosphere are determined. Their positions are compared with the Hα and magnetic structure ......
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