MHD Waves in Coronal Holes and Coronal Seismolgy
Abstract: Coronal holes are the dark patches in the solar corona associated with relatively cool, less dense plasma and unipolar fields. The fast component of the solar wind emanates from these regions. Several observations reveal the presence of magnetohydrodynamic (MHD) waves in coronal holes which are believed to play a key role in the acceleration of fast solar wind. The recent advent of high-resolution instruments had brought us many new insights on the properties of MHD waves in coronal holes which will be presented. The advances made in the identification of compressive slow MHD waves in both polar and equatorial coronal holes, their possible connection with the recently discovered high-speed quasi-periodic up-flows, their dissipation will be addressed. If these waves can be used for coronal seismology will be also reviewed.
Time: May 06, 2015, 2:30 pm
Venue: A601, NAOC