Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· References in the article
· Citations to the Article (11) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Solar TErrestrial Relations Observatory-A (STEREO-A) and PRoject for On-Board Autonomy 2 (PROBA2) Quadrature Observations of Reflections of Three EUV Waves from a Coronal Hole
Authors:
Kienreich, I. W.; Muhr, N.; Veronig, A. M.; Berghmans, D.; De Groof, A.; Temmer, M.; Vrsnak, B.; Seaton, D. B.
Affiliation:
AA(Kanzelhöhe Observatory/IGAM, Institute of Physics, University of Graz), AB(Kanzelhöhe Observatory/IGAM, Institute of Physics, University of Graz; Faculty of Geodesy, Hvar Observatory), AC(Kanzelhöhe Observatory/IGAM, Institute of Physics, University of Graz), AD(Royal Observatory of Belgium), AE(ESA, Science and Robotic Exploration Directorate c/o, Royal Observatory of Belgium), AF(Kanzelhöhe Observatory/IGAM, Institute of Physics, University of Graz), AG(Faculty of Geodesy, Hvar Observatory), AH(Royal Observatory of Belgium)
Publication:
Solar Physics, Volume 286, Issue 1, pp.201-219 (SoPh Homepage)
Publication Date:
08/2013
Origin:
SPRINGER
Keywords:
Shock waves, Coronal mass ejections
Abstract Copyright:
(c) 2013: Springer Science+Business Media B.V.
DOI:
10.1007/s11207-012-0023-8
Bibliographic Code:
2013SoPh..286..201K

Abstract

We investigate the interaction of three consecutive large-scale coronal waves with a polar coronal hole, simultaneously observed on-disk by the Solar TErrestrial Relations Observatory (STEREO)-A spacecraft and on the limb by the PRoject for On-Board Autonomy 2 (PROBA2) spacecraft on 27 January 2011. All three extreme ultraviolet (EUV) waves originate from the same active region, NOAA 11149, positioned at N30E15 in the STEREO-A field of view and on the limb in PROBA2. For the three primary EUV waves, we derive starting velocities in the range of ≈ 310 km s-1 for the weakest up to ≈ 500 km s-1 for the strongest event. Each large-scale wave is reflected at the border of the extended coronal hole at the southern polar region. The average velocities of the reflected waves are found to be smaller than the mean velocities of their associated direct waves. However, the kinematical study also reveals that in each case the ending velocity of the primary wave matches the initial velocity of the reflected wave. In all three events, the primary and reflected waves obey the Huygens-Fresnel principle, as the incident angle with ≈ 10° to the normal is of the same magnitude as the angle of reflection. The correlation between the speed and the strength of the primary EUV waves, the homologous appearance of both the primary and the reflected waves, and in particular the EUV wave reflections themselves suggest that the observed EUV transients are indeed nonlinear large-amplitude MHD waves.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints