Results 181 to 190 of about 14,687 (203)

A theory of heating of quiet solar corona

Physics of Plasmas, 2015
A theory is proposed to discuss the creation of hot solar corona. We pay special attention to the transition region and the low corona, and consider that the sun is quiet. The proposed scenario suggests that the protons are heated by intrinsic Alfvénic turbulence, while the ambient electrons are heated by the hot protons via collisions.
C. S. Wu, P. H. Yoon, C. B. Wang
openaire   +3 more sources

Energy Distribution of Heating Processes in the Quiet Solar Corona

The Astrophysical Journal, 1998
We have determined the variations in the emission measure of the solar corona using EUV Imaging Telescope/Solar and Heliospheric Observatory observations of iron lines in a quiet region of the Sun. The emission measure is found to vary significantly in at least 85% of all the pixels within 42 minutes.
Säm Krucker, Arnold O. Benz
openaire   +3 more sources

Alfvénic waves with sufficient energy to power the quiet solar corona and fast solar wind

Nature, 2011
Energy is required to heat the outer solar atmosphere to millions of degrees (refs 1, 2) and to accelerate the solar wind to hundreds of kilometres per second (refs 2-6). Alfvén waves (travelling oscillations of ions and magnetic field) have been invoked as a possible mechanism to transport magneto-convective energy upwards along the Sun's magnetic ...
Scott W, McIntosh, Bart, De Pontieu, Mats, Carlsson, Viggo, Hansteen, Paul, Boerner, Marcel, Goossens   +5 more
openaire   +4 more sources

Heating Events in the Quiet Solar Corona

Solar Physics, 1998
Sensitive observations of the quiet Sun observed by EIT on the SOHO satellite in high-temperature iron-line emission originating in the corona are presented. The thermal radiation of the quiet corona is found to fluctutate significantly, even on the shortest time scale of 2 min and in the faintest pixels. The power spectrum of the emission measure time
Arnold O. Benz, Säm Krucker
openaire   +1 more source

The Solar Quiet Chromosphere-Corona Transition Region

Space Science Reviews, 1998
The chromosphere-corona transition region of the Sun enjoys both simplicities of character and complexities of character which result from its very thin geometrical extent. The simplicities derive from the reasonably clear view of the energy balance (both observationally and theoretically), while the complexities derive from both the proximity of the ...
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Metric-Decametric Gyrosynchrotron Radio Emission From the Quiet Solar Corona

2022
<p>The radio emission of the quiet Sun in the metric and decametric bands has not been well studied historically due to limitations of existing instruments. It is nominally dominated by thermal brehmsstrahlung of the solar corona, but may also include significant gyrosynchrotron emission, usually assumed to be weak under quiet conditions.
Kamen Kozarev, Peijin Zhang, Pietro Zucca   +2 more
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Plasma flows in the quiet solar chromosphere-corona transition region

Moscow University Physics Bulletin, 2015
This article is devoted to solving the problem of the plasma temperature distribution along a magnetic tube, one end of which is in the chromosphere, while the other is in the corona. The plasma temperature dependences of the density, pressure, and velocity of plasma are determined for various velocities of the plasma flow, which are given at the lower
O. V. Dunin-Barkovskaya, B. V. Somov
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Structure and development of quiet loops in the solar corona

Space Science Reviews, 1994
AbstractSolar coronal features seen in X-ray emission change on two different timescales: a) flare loops and transient brightenings in active regions show a rapid variability, b) quiet region loops are quasi-steady and change only slowly with time. This different time behavior has been analyzed on the basis of Yohkoh SXT observations and we report here
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Physical properties of the quiet solar chromosphere–corona transition region

Astronomy Letters, 2016
The physical properties of the quiet solar chromosphere–corona transition region are studied. Here the structure of the solar atmosphere is governed by the interaction of magnetic fields above the photosphere. Magnetic fields are concentrated into thin tubes inside which the field strength is great.
O. V. Dunin-Barkovskaya, B. V. Somov
openaire   +1 more source

Quiet corona density model for the last maximum of solar activity

Solar Physics, 1973
We have selected observations of quiet K corona in maximum activity phase (1970 and 1972) and we have computed the corresponding density models. The density is found to be two times smaller than in average maximum coronal models (Newkirk, 1967) and nearly equal to that of minimum coronas (Saito, 1970).
Y. Leblanc, J. L. Leroy, P. Pecantet
openaire   +1 more source