The Solar Corona
Thermal instabilities in the solar corona
... the solar corona exists at all especially since the above argum ent suggests th a t it is always therm ally ...the solar corona, it is necessary to have either long field lines so th at the ...
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DOUBLE ARC INSTABILITY IN THE SOLAR CORONA
... ABSTRACT The stability of the magnetic field in the solar corona is important for understanding the causes of solar eruptions. Although various scenarios have been suggested to date, the ...
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Ducted magnetoacoustic waves in the solar corona
... we shall never know, never.” Albert Einstein 7.1 Sum m ary o f T hesis This thesis has examined the guiding of magnetoacoustic waves in coronal structures such as loops and current sheets. We have investigated how ...
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Review Heating mechanisms of the solar corona
... Abstract: The solar corona is a tenuous outer atmosphere of the Sun. Its million-degree temperature was discovered spectroscopically in the 1940s, but its origin has been debated since then without complete ...
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Intermittent heating of the solar corona by MHD turbulence
... These computations allow to perform a direct comparison between observations and the results of models of coronal heating, however such comparisons can yield scientific re- turn on coronal heating problem only if they ...
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Dynamics of a multi thermal loop in the solar corona
... G. Nisticò et al.: Dynamics of a Multi-Thermal Loop in the Solar Corona Fig. 1. Snapshots of the multi-thermal loop at several times, observed with SDO/AIA at 171 Å (left) and STEREO/EUVI-A at 195 Å ...
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Observatories of the Solar Corona and Active Regions (OSCAR)
... the Solar Dynamics Observatory (SDO) which aim to study – at least some aspects of – CMEs and ...the solar corona, none of them truly tackle the hard task of providing a space-based, reliable and ...
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The temperature structure of the quiescent regions of the solar corona
... the solar corona, with a plasma beta~ 10-3 ...region corona where the field is known to be ...the corona and are often highly time varying in their soft X-ray em ission and consequentially ...
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Joule heating and anomalous resistivity in the solar corona
... tion, and a corresponding upper limit to the current of 8×10 8 Amperes. These data are used as input for a cal- culation of Joule heating of the solar corona. 2. Two models are developed to calculate the ...
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Observing the solar corona with a tunable Fabry-Perot filter
... *Corresponding author: [email protected] Received 22 July 2008; accepted 24 August 2008; posted 5 September 2008 (Doc. ID 99216); published 21 October 2008 A solid Fabry –Perot etalon with a 0:16 Å passband was used ...
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Current sheets in the solar corona : formation, fragmentation and heating
... the solar coronal heating problem, outlining the MHD equations and sequences of MHD equilibria, before going on to discuss current sheets, resistive instabilities and finally magnetic ...
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Kinematic properties of globally propagating waves in the solar corona
... 6.6 Discussions and Conclusions A semi-automated technique designed to identify, track and analyse “EIT waves” in the solar corona was applied to observations of four CBF events using data from the EUVI ...
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Microturbulent magnetoactive plasmas and polarized radiation from the solar corona
... In laboratory plasmas and thermonuclear fusion devices, plasma turbulence is manifested by anomalously high electrical resistances, anomalous diffusion of particles, excessive radiation losses, etc. Astrophysically, the ...
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Fast magnetoacoustic wave trains in magnetic funnels of the solar corona
... 3 Central Astronomical Observatory at Pulkovo of the Russian Academy of Sciences, 196140 St Petersburg, Russia Received 16 September 2013 / Accepted 28 October 2013 ABSTRACT Context. Fast magneto-acoustic waves are ...
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Propagating EUV disturbances in the solar corona : two wavelength observations
... L4 D. B. King et al.: Propagating EUV disturbances in the Solar corona: Two-wavelength observations Fig. 4. Morlet wavelet transforms of the intensity variation observed at certain fixed points in 171 Å ...
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The sun and the solar corona
... The photosphere The photosphere is the visible surface layer of the Sun where photons last interact with atoms before escaping from the Sun; the temperature of the photosphere is 5,700 K; its main constituents are given ...
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Transverse waves in the solar corona
... This first observation of a TLO in hot coronal lines underlines the new capability of SDO/AIA of performing detailed spatial observations of the hot corona, which had been impossible with instruments such as ...
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Heating plasma loops in the solar corona
... Another much favored and related dissipative process is the reconnection of sheared Ðeld lines with the aid of the tearing-mode instability, provided this occurs in a plasma Ñow strongly converging toward the neutral ...
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Helium line emissivities in the Solar Corona
... quiescent solar corona and predict the emissivities of the He and He + lines to be observed by DKIST, Solar Orbiter, and ...outer solar corona, using new dielectronic recombination ...
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Time dependent heating of the solar corona
... Hollweg (1984) showed how a coronal loop could act as a resonant cavity and that the transmission of energy into the loop was enhanced at certain resonant frequen cies. His results were in qualitative agreement with ...
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