scholarly journals Slight Disappearance of Prominence Plasma to the Solar Corona

1990 ◽  
Vol 142 ◽  
pp. 347-349
Author(s):  
V. Rusin ◽  
V. Dermendjiev ◽  
M. Rybansky ◽  
G. Buyukliev
Keyword(s):  
Solar Corona ◽  
Mass Balance ◽  
Plasma Exchange ◽  
Mass Exchange ◽  
White Light ◽  
Close Relation ◽  
Plasma Flows ◽  
Corona Plasma ◽  
White Light Corona

The problem of prominences-corona relationship is relativelly old. Already in 1931 Lockyer [1] showed that there is a close relation between prominences distribution and the form of white-light corona. However, this problem is still debatable and poses a number of controversial questions. One of them is the question of the energy and mass exchange between prominences and the ambient corona. It is generally assumed that the mass balance exists between the corona and prominences, but unambiguous observational proofs for prominences-corona plasma exchange are very rare. There are little data [2-4], as well, that could be used to address the problem of slight plasma flows from prominences to the corona.

scholarly journals Coronascope II observation of the white light corona from a stratospheric balloon

1965 ◽  
Vol 23 ◽  
pp. 287-291 ◽  
Author(s):  
Gordon Newkirk ◽  
J. David Bohlin
Keyword(s):  
Solar Corona ◽  
White Light ◽  
Geomagnetic Storms ◽  
Scattered Light ◽  
Objective Lens ◽  
The West ◽  
West Limb ◽  
Stratospheric Balloon ◽  
White Light Corona

By use of an apodized occulting dish before the objective lens of a coronagraph the instrumentally scattered light can be reduced to about 10-9 B⊙. Observation of the streamers of the solar corona from 1.8 to 5.25 R⊙ outside of eclipse from a balloon at 30 km altitude are described. A solar streamer complex present at the west limb on 5 March 1964 was apparently the origin of the particles causing the recurrent geomagnetic storms of late 1963 and early 1964.

The White-Light and Emission Coronae at the July 22, 1990 Eclipse

1994 ◽  
Vol 144 ◽  
pp. 555-557
Author(s):  
V. Rušin ◽  
E. Marková
Keyword(s):  
Solar Corona ◽  
Coronal Hole ◽  
White Light ◽  
Active Regions ◽  
Coronal Line ◽  
Line Intensities ◽  
Rapid Changes ◽  
Southwest Region ◽  
White Light Corona

AbstractVarious instruments were used to study the solar corona at the July 22, 1990 eclipse. The white-light corona of July 22, 1990 is of maximum type (the Ludendorff index of the corona’s shape turns out to be a+b = 0.04). There are many streamers nearly equally distributed around the whole Sun, except of the southwest region where large coronal hole was located. The green (530.3 nm) and red (637.4 nm) coronal line intensities display many rapid changes in active regions around the eclipse day. Huge prominences were located above the E-limb. The estimated total brightness of the white-light corona (WLC) reached its value ofJK= 1.32 × 10−6.

FeXIV Line Emission Polarization of the July 11, 1991 Solar Corona

1994 ◽  
Vol 144 ◽  
pp. 541-547
Author(s):  
J. Sýkora ◽  
J. Rybák ◽  
P. Ambrož
Keyword(s):  
High Resolution ◽  
Solar Corona ◽  
Emission Line ◽  
Solar Eclipse ◽  
White Light ◽  
Preliminary Analysis ◽  
Line Emission ◽  
Total Solar Eclipse ◽  
Degree Of Polarization ◽  
High Resolution Images

AbstractHigh resolution images, obtained during July 11, 1991 total solar eclipse, allowed us to estimate the degree of solar corona polarization in the light of FeXIV 530.3 nm emission line and in the white light, as well. Very preliminary analysis reveals remarkable differences in the degree of polarization for both sets of data, particularly as for level of polarization and its distribution around the Sun’s limb.

STRUCTURE AND DYNAMICS OF THE 2009 JULY 22 ECLIPSE WHITE-LIGHT CORONA

2011 ◽  
Vol 742 (1) ◽  
pp. 29 ◽  
Author(s):  
J. M. Pasachoff ◽  
V. Rušin ◽  
M. Saniga ◽  
H. Druckmüllerová ◽  
B. A. Babcock
Keyword(s):  
White Light ◽  
Structure And Dynamics ◽  
White Light Corona

The Structure of the White-Light Corona at the 1991 Eclipse

1994 ◽  
pp. 217-221
Author(s):  
A. Sanchez-Ibarra ◽  
M. Cisneros-Molina ◽  
G. Hinojosa-Palafox ◽  
F. Cisneros-Peña ◽  
J. Guerrero De la Torre ◽  
...  
Keyword(s):  
White Light ◽  
White Light Corona

scholarly journals MHD Aspects of Coronal Transients

1980 ◽  
Vol 91 ◽  
pp. 263-277 ◽  
Author(s):  
U. Anzer
Keyword(s):  
Solar Corona ◽  
Time Scales ◽  
White Light ◽  
Solar Flares ◽  
Great Length ◽  
X Ray

If one defines coronal transients as events which occur in the solar corona on rapid time scales (≲ several hours) then one would have to include a large variety of solar phenomena: flares, sprays, erupting prominences, X-ray transients, white light transients, etc. Here we shall focus our attention on the latter two phenomena; solar flares have been discussed at great length in a recent Skylab workshop and IAU Colloqium No. 44 was devoted to the study of prominences. Coronal transients, in the narrower sense, were first seen with the instruments on board of Skylab, both in the optical and the X-ray part of the spectrum.

scholarly journals Optical Evidence for Plasma Ejections and Waves in the Solar Corona

1974 ◽  
Vol 57 ◽  
pp. 323-332 ◽  
Author(s):  
A. Bruzek
Keyword(s):  
Solar Corona ◽  
White Light ◽  
Solar Disk ◽  
Dense Plasma ◽  
Radio Bursts ◽  
X Ray ◽  
Imperfect Knowledge ◽  
Optical Evidence ◽  
Made In

Plasma ejections and waves in the solar corona are almost exclusively flare associated phenomena. Ejections of relatively cool and dense plasma are frequently observed in Hα whereas observations in coronal light (visible, EUV- and X-radiation) are still rather scarce. Occurrence of coronal waves is so far best known from their effects on the Hα chromosphere and, of course, from the production of radio bursts. Only in relatively few cases have observations been made in coronal lines and in coronal continuum by ground based as well as by satellite borne equipment. We may expect, however, that the white light coronagraph and the X-ray telescopes on board of the Skylab will detect quite a number of events in front of the solar disk and high in the solar corona and will considerably increase and improve our imperfect knowledge and understanding of coronal ejections and waves as it is presented in this review.

White-light solar corona structure observed by naked eye and processed images

2020 ◽  
Vol 495 (2) ◽  
pp. 2170-2178 ◽  
Author(s):  
Vojtech Rušin ◽  
Paul Prikryl ◽  
Emil A Prikryl
Keyword(s):  
Solar Wind ◽  
White Light ◽  
High Speed ◽  
Geomagnetic Storms ◽  
Interplanetary Space ◽  
Coronal Holes ◽  
Human Vision ◽  
Naked Eye ◽  
Wide Range ◽  
White Light Corona

ABSTRACT Light and dark adaptation and luminance contrast enhancement are well-known characteristics of human vision that allow us to observe a wide range of light intensity not fully captured in standard camera images. The naked-eye observations of total eclipses, some recorded with spectacular detail in artists’ paintings, reveal structure that is consistent with images obtained by telescopes equipped with recording media. The actual shape of the corona during a total eclipse depends not only on the phase of the solar cycle but, as can be simply demonstrated, also on the day-to-day variability and spatial distribution of coronal intensity that is determined by solar surface magnetic fields, including the locations of coronal holes that are the sources of high-speed solar wind causing geomagnetic storms. The latter were very similar for the eclipses in 1932, 1994, and 2017, which is the main reason why the naked-eye observations, as well as the processed images (1994 and 2017), of the white-light corona displayed very similar shapes. White-light corona image processing is a useful technique to enhance the contrast to observe fine-scale structure that is consistent with the physics of the solar atmosphere shaped by the magnetic field drawn out into the interplanetary space by solar wind.

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