Results 141 to 150 of about 2,148 (181)
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Interacting Active Regions in the Solar Corona
Astrophysical Journal, 1996We report an episode from the Yohkoh soft X-ray observations during which antiparallel coronal magnetic fields from two separate active regions, located in opposite hemispheres, reconnect and form new transequatorial coronal loops. Strong evidence for magnetic reconnection consists of the following: (1) Transequatorial connections not previously ...
Saku Tsuneta
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Data-driven model of the solar corona above an active region [PDF]
Astronomy and Astrophysics, 2019 Aims. We aim to reproduce the structure of the corona above a solar active region as seen in the extreme ultraviolet (EUV) using a three-dimensional magnetohydrodynamic (3D MHD) model. Methods. The 3D MHD data-driven model solves the induction equation and the mass, momentum, and energy balance.
Hardi Peter, Jorn Warnecke
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A First Spectroscopic Measurement of the Magnetic-field Strength for an Active Region of the Solar Corona [PDF]
Astrophysical Journal Letters, 2020 Abstract For all involved in astronomy, the importance of monitoring and determining astrophysical magnetic-field strengths is clear. It is also a well-known fact that the corona magnetic fields play an important part in the origin of solar flares and the variations of space weather.
Roger Hutton, Wenxian Li, Ran Si
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An Active Region Streamer of the Solar Corona
Publications of the Astronomical Society of Japan, 1967Abstract A photometric investigation is reported for a conspicuous active region streamer which originated at heliographic P. A. 280 ° of the solar corona observed at the 1962 New Guinea eclipse. The following results are derived: (1) The electron density along the axis of streamer is obtained out to 3.5 R⊙.
Kuniji Saito, Naoaki Owaki
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Development of a complex of activity in the solar corona
Solar Physics, 1977Skylab observations of the Sun in soft X-rays gave us the first possibility to study the development of a complex of activity in the solar corona during its whole lifetime of seven solar rotations. The basic components of the activity complex were permanently interconnected (including across the equator) through sets of magnetic field lines, which ...
Robert Howard, Zdeněk Švestka
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Signatures of Slow Solar Wind Streams from Active Regions in the Inner Corona [PDF]
Solar Physics, 2012 Accepted for publication in Solar Physics; 31 Pages; 13 ...
Farid Goryaev +2 more
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The Rotation of The Fe XIV Solar Corona During the Recent Solar Activity Minimum
Space Science Reviews, 1999We analyze data observed by the LASCO C1 coronagraph on board the SOHO spacecraft during the solar minimum activity from April 1996 to March 1997. Using the phase dispersion technique, we investigate the periodicity and recurrence of Fe XIV emission structures with heliospheric latitude and distance above the Sun’s surface with high spatial resolution.
Inhester, B. +4 more
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Scientific American, 1983
In the past decade what is known about the corona has been vastly enlarged by instruments on the ground and on spacecraft, manned and unmanned. The corona is observed to be in a continuous state of flux, punctuated by periodic explosive outbursts. From spectroscopic observations the temperature of the corona is estimated to be between one and two ...
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In the past decade what is known about the corona has been vastly enlarged by instruments on the ground and on spacecraft, manned and unmanned. The corona is observed to be in a continuous state of flux, punctuated by periodic explosive outbursts. From spectroscopic observations the temperature of the corona is estimated to be between one and two ...
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Publications of the Astronomical Society of Australia, 1981
When I began my studies of solar radio astronomy, Dr J. L. Pawsey, who then led the radio astronomy group in the Division of Radiophysics, CSIRO, explained to me that the internal structure of the Sun was ‘well understood’, thanks to a lack of conflicting observational data, but that for the observable layers of the Sun, the photosphere, chromosphere ...
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When I began my studies of solar radio astronomy, Dr J. L. Pawsey, who then led the radio astronomy group in the Division of Radiophysics, CSIRO, explained to me that the internal structure of the Sun was ‘well understood’, thanks to a lack of conflicting observational data, but that for the observable layers of the Sun, the photosphere, chromosphere ...
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Solar Physics, 1996
This review puts together what we have learned about coronal structures and phenomenology to synthesize a physical picture of the corona as a voluminous, thermally and electrically highly-conducting atmosphere responding dynamically to the injection of magnetic flux from below.
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This review puts together what we have learned about coronal structures and phenomenology to synthesize a physical picture of the corona as a voluminous, thermally and electrically highly-conducting atmosphere responding dynamically to the injection of magnetic flux from below.
openaire +1 more source