E-Print Archive

There are 4553 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
Direct Imaging by SDO/AIA of Quasi-periodic Propagating Fast Mode Magnetosonic Waves Propagating of ~2000 km s-1 in the Low Solar Corona View all abstracts by submitter

Wei Liu   Submitted: 2011-06-15 12:22

Quasi-periodic, propagating fast mode magnetosonic waves in the corona weredifficult to observe in the past due to relatively low instrument cadences. Wereport here evidence of such waves directly imaged in EUV by the new SDO AIAinstrument. In the 2010 August 1 C3.2 flare/CME event, we find arc-shaped wavetrains of 1-5% intensity variations (lifetime ~200 s) that emanate near theflare kernel and propagate outward up to ~400 Mm along a funnel of coronalloops. Sinusoidal fits to a typical wave train indicate a phase velocity of2200 ± 130 km s-1. Similar waves propagating in opposite directions areobserved in closed loops between two flare ribbons. In the k-omega diagramof the Fourier wave power, we find a bright ridge that represents thedispersion relation and can be well fitted with a straight line passing throughthe origin. This k-omega ridge shows a broad frequency distribution withindicative power at 5.5, 14.5, and 25.1 mHz. The strongest signal at 5.5 mHz(period 181 s) temporally coincides with quasi-periodic pulsations of theflare, suggesting a common origin. The instantaneous wave energy flux of(0.1-2.6) imes 107 ergs/cm2/s estimated at the coronal base is comparableto the steady-state heating requirement of active region loops.

Authors: Wei Liu, Alan M. Title, Junwei Zhao, Leon Ofman, Carolus J. Schrijver, Markus J. Aschwanden, Bart De Pontieu, and Theodore D. Tarbell
Projects: SDO-AIA

Publication Status: Accepted by ApJ Letters (AAS/SPD Press Release, Las Cruces, June 15, http://www.lmsal.com/press/apjl2011_magnetosonic)
Last Modified: 2011-06-18 06:54
Go to main E-Print page  Solar Dynamics Observatory discovers thin high temperature strands in coronal active regions  Major electron events and coronal magnetic configurations of the related solar active regions   Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
Stability of slow magnetoacoustic and entropy waves in the solar coronal plasma with thermal misbalance
The chromosphere underneath a Coronal Bright Point
Characterising fast-time variations in the hard X-ray time profiles of solar flares using Solar Orbiter's STIX
The quiet sun at mm wavelengths as seen by ALMA
Explosive Events in the Quiet Sun Near and Beyond the Solar Limb Observed with the Interface Region Imaging Spectrograph (IRIS)
Multi-stage reconnection powering a solar coronal jet
A Statistical Analysis of Magnetic Field Changes in the Photosphere during Solar Flares Using High-cadence Vector Magnetograms and Their Association with Flare Ribbons
Numerical Study on Excitation of Turbulence and Oscillation in Above-the-loop-top Region of a Solar Flare
Oscillatory reconnection as a plasma diagnostic in the solar corona
The independence of oscillatory reconnection periodicity from the initial pulse
Oscillatory Reconnection of a 2D X-point in a hot coronal plasma
Formation Of The Lyman Continuum During Solar Flares
MHD simulation of Solar Eruption from Active Region 11429 Driven by Photospheric Velocity Field
Unfolding Drift Effects for Cosmic Rays over the Period of the Sun's Magnetic Field Reversal
Problems in Observation and Identification of Torsional Waves in the Lower Solar Atmosphere
Solar Orbiter and SDO Observations, and Bifrost MHD Simulations of Small-scale Coronal Jets
Dominance of Bursty over Steady Heating of the 48 MK Coronal Plasma in a Solar Active Region: Quantification Using Maps of Minimum, Maximum, and Average Brightness
Solar flare hard X-rays from the anchor points of an eruptive filament
Plasmoids, Flows, and Jets During Magnetic Reconnection in a Failed Solar Eruption
Connecting Chromospheric Condensation Signatures to Reconnection-driven Heating Rates in an Observed Flare

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2000-2020 Solar Physics Group - Montana State University