Data Access
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
Version:2.6.1
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
| Role | Person | StartDate | StopDate | Note | |
|---|---|---|---|---|---|
| 1. | Author | spase://SMWG/Person/Nariaki.V.Nitta |
The catalog is in the paper
https://www.lmsal.com/nitta/publ/ApJ_776_58_2013_nitta.pdf
The movie catalog is online
https://www.lmsal.com/nitta/movies/AIA_Waves/
Date of observation
Start time of event
Strength of Solar Flares
Event location
Active region
Large-scale Coronal Propagating Front speed
Dominant direction of CME propagation
Appearance of the front at the 171 Å channel
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).
Type II radio burst
Event observed by one or both of the Solar and Terrestrial Relations Observatory spacecraft as limb events.
References to related publications