Results 141 to 150 of about 1,306 (183)

Noise in Maps of the Sun at Radio Wavelengths II: Solar Use Cases. [PDF]

Sol Phys
Bastian T, Chen B, Mondal S, Saint-Hilaire P.   +3 more
europepmc   +1 more source

Some of the next articles are maybe not open access.

Related searches:

On the polarization of the solar coronal emission lines

Solar Physics, 1973
The results of the spectrophotometrical measurements of the polarization in the coronal lines Fe xIv 5303 fit and Fe x 6374 fit are given. Polarization spectrograms were obtained by two spectrographs (prism and echelle types) during the solar eclipse in Mexico on 7 March, 1970 near the region of the second contact at the heights 0.06 to 0.12 R| above ...
Vladimir Obridko
exaly   +2 more sources

Using Strong Solar Coronal Emission Lines as Coronal Flux Proxies

Solar Physics, 1998
We investigate the possibility that strong EUV lines observed with the Goddard Solar EUV Rocket Telescope and Spectrograph (SERTS) provide good proxies for estimating the total coronal flux over shorter wavelength ranges. We use coordinated SERTS and Yohkoh observations to obtain both polynomial and power-law fits relating the broad-band soft X-ray ...
David A. Falconer, Stuart D. Jordan, Jeffrey W. Brosius, Joseph M. Davila, Roger J. Thomas, Vicenzo Andreatta, Hirohisa Hara   +6 more
openaire   +1 more source

Solar flare activity and the structure of the coronal neutral line

Solar Physics, 1995
In this study we analyse the positions of major flares from 1978 and 1979, with respect to the magnetic structure of the solar corona, as described by a potential field model. We find that major flares exhibit no strong association with the neutral line at the chromospheric level.
G. A. Stewart, S. Bravo
openaire   +1 more source

Solar rotation as measured in EUV chromospheric and coronal lines

Solar Physics, 1972
Active regions were followed across the disk on OSO 4 spectroheliograms in the Lyman continuum (LC) and in Mg x λ625. These observations indicate differential rotation with latitude, but not with height in the atmosphere. The measured equatorial sidereal rotation velocity is 14.7° ±0.2° per day in both chromospheric LC and coronal Mg x, where the ...
George W. Simon, Robert W. Noyes
openaire   +1 more source

Solar magnetic fields and the intensity of the green coronal line

Astronomy Reports, 2004
Synoptic maps of the intensity of the λ530.5 nm FeXIV green coronal line and maps of computed coronal magnetic fields for the period 1977–2001 are compared. For quantitative comparisons, the correlation coefficients r for the correlation between these two parameters at corresponding points of the synoptic maps are calculated.
O. G. Badalyan, V. N. Obridko
openaire   +1 more source

Fe XVII X-ray lines in solar coronal plasmas

Advances in Space Research, 1997
Abstract Calculated intensities of the Fe XVII X-ray lines due to transitions 2p6 − 2p53d lines (near 15 A) and 2p6 − 2p53s lines (near 17 A) are compared with measured line intensities in solar and tokamak spectra. For the solar spectra, temperature Te is obtained from the ratio of the Fe XVII 16.776 A line to a nearby Fe XVIII line.
K.J.H. Phillips, C.J. Greer, A.K. Bhatia, I.H. Coffey, R. Barnsley, F.P. Keenan   +5 more
openaire   +1 more source

On the correlation of coronal green-line intensity and solar wind velocity

Solar Physics, 1975
Cross-correlation functions have been computed between green-line intensity (Kislovodsk) and Vela solar wind velocity January–June 1967. They are calculated separately for east and west limb observations in 5° latitude increments, and the solar wind velocites are correlated at their estimated emission times by correcting for the plasma Earth-Sun ...
E. C. Roelof, S. Cuperman, A. Sternlieb
openaire   +1 more source

A polarization-intensity anticorrelation diagram for the solar coronal green line

Astronomy Letters, 2001
We analyze the complex pattern of anticorrelation between the degree of polarization p in the green λ530.3-nm line and its intensity I λ, which was revealed by coronal observations during the total solar eclipse of July 11, 1991. For coronal points located at approximately the same distance from the disk center, the anticorrelation diagram breaks up ...
O. G. Badalyan, J. Syýkora
openaire   +1 more source

Solar Corona Investigation by the Coronal Line Photometer at Lomnický Peak

International Astronomical Union Colloquium, 1994
AbstractThis paper deals with a possibility to use the ground-based method of observation in order to solve basic problems connected with the solar corona research. Namely:1.heating of the solar corona2.course of the global cycle in the corona3.rotation of the solar corona and development of active regions.There is stressed a possibility of high-time ...
M. Minarovjech, M. Rybanský
openaire   +1 more source