Results 161 to 170 of about 1,347 (224)

Magnetic star-planet interaction in the young exoplanet system DS Tucanae Ab

Santos Ld, Owen J, Duvvuri G, Loyd ROP, Vidotto A, Presa A, Bourrier V, King G, Airapetian V, Ehrenreich D, France K, Lendl M, Lothringer J, Nielsen L.   +13 more
europepmc   +1 more source

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 ...
D. A. Falconer, S. D. Jordan, J. W. Brosius, J. M. Davila, Roger J. Thomas, Vicenzo Andreatta, Hirohisa Hara   +6 more
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The identification of new forbidden coronal lines in the solar EUV spectrum

Solar Physics, 1971
Identifications are proposed for twenty of the twenty-eight coronal lines observed in the spectra obtained during a rocket flight into the path of the 7 March, 1970 solar eclipse. The methods by which the lines have been identified are discussed. Most of the lines identified are from forbidden transitions between levels in the ground 2pn and 3pn ...
Carole Jordan
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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
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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 ...
E. Mogilevsky, B. Ioshpa, V. Obridko
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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
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Solar EUV and UV Emission Line Observations Above a Polar Coronal Hole

Space Science Reviews, 1998
The roll manoeuvre of SOHO on September 3, 1997 provided the opportunity to study the northern coronal hole with SUMER slits in east-west orientation, so that polar plumes and inter-plume lanes could be observed simultaneously. A preliminary analysis of the observations shows that lines emitted by ions with the lowest formation temperatures (with the ...
Wilhelm, K., Bodmer, R.
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Improved solar coronal temperature for equal green and red line intensities

Solar Physics, 1976
An improved value of the temperature in the solar corona for equal green and red line intensities is obtained. This temperature is in better agreement with a quoted line-width value than the previous theoretical ones.
Udit Narain, Suresh Chandra
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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
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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
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