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  • 1
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    The magnetic network location of explosive events observed in the solar transition region (1991)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: Compact short-lived explosive events have been observed in solar transition region lines with the High-Resolution Telescope and Spectrograph (HRTS) flown by the Naval Research Laboratory on a series of rockets and on Spacelab 2. Data from Spacelab 2 are coaligned with a simultaneous magnetogram and near-simultaneous He I 10,380 -A spectroheliogram obtained at the National Solar Observatory at Kitt Peak. The comparison shows that the explosive events occur in the solar magnetic network lanes at the boundaries of supergranular convective cells. However, the events occur away from the larger concentrations of magnetic flux in the network, in contradiction to the observed tendency of the more energetic solar phenomena to be associated with the stronger magnetic fields.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 370; 775-778
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Microflares observed with UVSP and HXIS (1992)
    In:  CASI
    Details
    Publication Date: 2013-08-29
    Description: A review of an analysis of SMM (Solar Maximum Mission) microflare observations is presented. The data, from the UVSP (Ultraviolet Spectrometer and Polarimeter) and HXIS (Hard X-ray Imaging Spectrometer) instruments, show that there are counterparts to UV microflares in x-ray emission characteristic of 10(exp 7) K plasma. Implications of the x-ray/UV relationship for flare distribution functions and coronal heating are discussed, and examples of similar events in SMM quiet Sun data are shown.
    Keywords: SOLAR PHYSICS
    Type: ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition; p 289-292
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    NASA TECHNICAL REPORTS
  • 3
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    The possible role of MHD waves in heating the solar corona (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-08-28
    Description: The possible role of waves in the heating of the solar corona has been investigated. A general dispersion relation has been derived for waves propagating in a homogeneous plasma subject to dissipation by viscosity and thermal conduction. The dissipation mechanisms have been incorporated self-consistently into the equations, and no assumptions about the strength of the damping have been made. Solutions of the sixth-order dispersion relation provide information on how the damping of both slow and fast mode waves depends upon the plasma density, temperature, field strength, and angle of propagation relative to the background magnetic field. We provide a detailed comparison to the standard approach, which is to solve for the wave quantities in the absence of dissipation and then to use these quantities in expressions for the heating due to viscosity and thermal conduction.
    Keywords: SOLAR PHYSICS
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 435; 1; p. 482-501
    Format: text
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    NASA TECHNICAL REPORTS
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