ResourceName
LARGE-SCALE CORONAL PROPAGATING FRONTS IN SOLAR ERUPTIONS AS OBSERVED BY THE AIA (SDO) and EUVI (STEREO-B, STEREO-A)
ReleaseDate
2026-02-02 13:10:26Z
RevisionHistory
RevisionEvent
ReleaseDate
2024-08-12 10:06:55
Note
Only known prior ReleaseDate of the metadata
RevisionEvent
ReleaseDate
2026-02-02 13:10:26Z
Note
Added MetadataRightsList. Added ResourceType and NamingAuthority. Updated to 2.7.1. Changed http to https in top-level schemaLocation attribute. Fixed version number separator in top-level schemaLocation attribute. ZCB
Description
The catalog is build on the observations (movies) of global disturbances in the solar corona with characteristic
propagating fronts as intensity enhancement, Large-scale Coronal Propagating Fronts (LCPFs), as captured in AIA (SDO) and EUVI (STEREO-B, STEREO-A) images. They are often but not always associated with coronal mass ejections (CMEs).
LCPFs are similar to the phenomena that have often been referred to as Extreme Ultraviolet Imaging Telescope (EIT) waves or extreme-ultraviolet (EUV) waves. Between 2010 April and 2013 January, a total of 171 LCPFs have been identified through visual inspection of AIA images in the 193 Å channel.
The list of movies can be found here: https://www.lmsal.com/nitta/movies/AIA_Waves/
The images used in these movies are shrunk to 768x768. They are 144s cadence for AIA, typically 5m cadence for EUVI. See http://www.lmsal.com/nitta/movies/AIA_Waves/oindex.html for movies that include all AEC-off AIA images. Their cadence is 12s (24s) before (after) October 10, 2010.
Publication DOI 10.1088/0004-637X/776/1/58
PublicationInfo
Title
LARGE-SCALE CORONAL PROPAGATING FRONTS IN SOLAR ERUPTIONS
AS OBSERVED BY THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD
THE SOLAR DYNAMICS OBSERVATORY—AN ENSEMBLE STUDY
Authors
Nariaki V. Nitta, Carolus J. Schrijver, Alan M. Title, and Wei Liu
PublicationDate
2013-10-10 12:00:00
PublishedBy
The Astrophysical Journal, 776:58 (13pp)
LandingPageURL
https://www.lmsal.com/nitta/publ/ApJ_776_58_2013_nitta.pdf
Contacts
Name
CME level
Description
CME levels: (1) weak outflow that
becomes invisible before the heliocentric distance of 5 R; (2)
narrow (<60◦) or slow (<500 km s−1) outflow traceable beyond
5 R, but typically not being reminiscent of the three-part CME
structure; (3) well-formed CME, fast and wide, with a flux
rope or three-part structure; (4) similar to level 3, but very fast
(>1500 km s−1).
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