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
A Truly Global EUV Wave From the SOL2017-09-10 X8.2 Solar Flare-CME Eruption View all abstracts by submitter

Wei Liu   Submitted: 2018-07-25 10:19

We report SDO/AIA observations of an extraordinary global extreme ultraviolet (EUV) wave triggered by the X8.2 flare-CME eruption on 2017 September 10. This was one of the best EUV waves ever observed with modern instruments, yet likely the last one of such magnitudes of Solar Cycle 24 as the Sun heads toward the minimum. Its remarkable characteristics include: (1) The wave was observed, for the first time, to traverse the full-Sun corona over the entire visible solar disk and off-limb circumference, manifesting a truly global nature, owing to its exceptionally large amplitude, e.g., with EUV enhancements by up to 300% at 1.1 Rsun from the eruption. (2) This leads to strong transmissions (besides commonly observed reflections) in and out of both polar coronal holes, which are usually devoid of EUV waves. It has elevated wave speeds >2000 km s-1 within them, consistent with the expected higher fast-mode magnetosonic speeds. The coronal holes essentially serve as new ''radiation centers'' for the waves being refracted out of them, which then travel toward the equator and collide head-on, causing additional EUV enhancements. (3) The wave produces significant compressional heating to local plasma upon its impact, indicated by long-lasting EUV intensity changes and differential emission measure increases at higher temperatures (e.g., log T=6.2) accompanied by decreases at lower temperatures (log T=6.0). These characteristics signify the potential of such EUV waves for novel magnetic and thermal diagnostics of the solar corona {it on global scales}.

Authors: Wei Liu, Meng Jin, Cooper Downs, Leon Ofman, Mark Cheung, and Nariaki V. Nitta
Projects: SDO-AIA

Publication Status: Accepted by ApJ Letters (as of July 24, 2018)
Last Modified: 2018-07-29 21:13
Go to main E-Print page  A Truly Global EUV Wave From the SOL2017-09-10 X8.2 Solar Flare-CME Eruption  ALTERNATIVE ZEBRA-STRUCTURE MODELS IN SOLAR RADIO EMISSION  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