2009/03/24 by M. S. Marsh, R. W. Walsh, S. P. Plunkett +1 · 3 citations
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Geomagnetism and Paleomagnetism Studies #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/697/2/1674
published as Astrophys.J.697:1674-1680,2009 · In press, ApJ June 2009 - 1 v697 issue
arxiv created 2009/03/24 · openalex publication_date 2009/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
On 2008 January 10, the twin Solar Terrestrial Relations Observatory A and B spacecraft conducted a high time cadence study of the solar corona with the Extreme-Ultraviolet Imager instruments with the aim of investigating coronal dynamics. Observations of the three-dimensional propagation of waves within active region coronal loops and a measurement of the true coronal slow mode speed are obtained. Intensity oscillations with a period of ≈12 minutes are observed to propagate outward from the base of a loop system, consistent with the slow magnetoacoustic mode. A novel analysis technique is applied to measure the wave phase velocity in the observations of the A and B spacecraft. These stereoscopic observations are used to infer the three-dimensional velocity vector of the wave propagation, with an inclination of 37° ± 6° to the local normal and a magnitude of 132 ± 9 and 132 ± 11 km s −1 , giving the first measurement of the true coronal longitudinal slow mode speed, and an inferred temperature of 0.84 ± 0.12 MK and 0.84 ± 0.15 MK.