1 Ocak 2010 Dergi makalesi Açık Erişim

Devlen, E.; Pekunlu, E. R.

Dublin Core

<?xml version='1.0' encoding='utf-8'?>
<oai_dc:dc xmlns:dc="http://purl.org/dc/elements/1.1/" xmlns:oai_dc="http://www.openarchives.org/OAI/2.0/oai_dc/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.openarchives.org/OAI/2.0/oai_dc/ http://www.openarchives.org/OAI/2.0/oai_dc.xsd">
  <dc:creator>Devlen, E.</dc:creator>
  <dc:creator>Pekunlu, E. R.</dc:creator>
  <dc:date>2010-01-01</dc:date>
  <dc:description>The effects, hitherto not treated, of the temperature and the number density gradients, both in the parallel and the perpendicular direction to the magnetic field, of O VI ions, on the MHD wave propagation characteristics in the solar North Polar Coronal Hole are investigated. We investigate the magnetosonic wave propagation in a resistive MHD regime where only the thermal conduction is taken into account. Heat conduction across the magnetic field is treated in a non-classical approach wherein the heat is assumed to be conducted by the plasma waves emitted by ions and absorbed at a distance from the source by other ions. Anisotropic temperature and the number density distributions of O VI ions revealed the chaotic nature of MHD standing wave, especially near the plume/interplume lane borders. Attenuation length scales of the fast mode is shown not to be smoothly varying function of the radial distance from the Sun. (C) 2010 WILEY-VCH Verlag GmbH &amp; Co. KGaA, Weinheim</dc:description>
  <dc:identifier>https://aperta.ulakbim.gov.trrecord/28383</dc:identifier>
  <dc:identifier>oai:zenodo.org:28383</dc:identifier>
  <dc:rights>info:eu-repo/semantics/openAccess</dc:rights>
  <dc:rights>http://www.opendefinition.org/licenses/cc-by</dc:rights>
  <dc:source>ASTRONOMISCHE NACHRICHTEN 331(7) 716-724</dc:source>
  <dc:title>MHD waves in the solar north polar coronal hole</dc:title>
  <dc:type>info:eu-repo/semantics/article</dc:type>
  <dc:type>publication-article</dc:type>
</oai_dc:dc>