SHINE promotes research on the processes by which energy in the form of magnetic fields and accelerated particles is produced by the Sun, and on the mechanisms by which this energy is transported through the inner heliosphere. The focus is on the connection between events and phenomena on the Sun and related solar wind structures and other in situ measurements in the inner heliosphere.
SHINE has recently decided to encourage detailed studies of a few carefully selected events that may help advance this research. 'Campaign' refers to a concerted, focused effort on one or more event periods or topics, usually taking place over a limited time period with the goal of a final report or papers devoted to the results of the campaign. Since coronal mass ejections (CMEs) are the primary transient phenomena that cause the largest interplanetary disturbances, driving shock waves that in turn accelerate particles and cause the largest geomagnetic storms, it was decided that the SHINE Campaigns should focus on a few carefully selected CME Events. Thus, the overarching theme of the SHINE Campaign Events program is to improve our understanding of both the CME process and the coronal and solar wind context in which they occur. Three general questions that the Campaigns address are 1) How are CMEs initiated? and 2) How do CMEs evolve or propagate? and 3) How are CME-related solar energetic particles accelerated and transported? Bringing as much data and interpretation to bear on a given event as possible, the Campaigns will address these questions by confronting current and developing CME models with observational data and simulations, thereby forcing comparisons between existing models and guiding the development and improvement of new models and simulations. This approach should help us to both enhance our physical understanding of the eruption and propagation of CMEs and to improve our predictive capabilities.
Because of the large, continuous data sets and modeling techniques that have become available since the start of the SOHO era, it was decided to select events occurring since 1996. The chosen events should have reasonably complete data on both its solar source regions and its propagation through the low corona into the heliosphere. It is desirable but not essential to include Earth-directed events so that their in-situ and geoeffective characteristics can be studied. Four events or event periods were selected before the SHINE 2003 Workshop, and 3 leaders assigned to guide the work on each event. Dave Webb and Nick Arge are co-leaders of the overall Campaign Events program.
Why were these particular events selected? The May 1997 event has
already been well studied and the pre-event and event solar and
heliospheric background conditions were relatively simple, therefore
good for modeling. This event has been and is being studied in the
SHINE-GEM-CEDAR Campaign, MURI and CISM. The May 1998 event is also a
MURI event and has good vector magnetic field data (on AR 8210) with
which to work. Both of these events drove shocks and caused major
storms at Earth. The focus on these two events will be on CME
initiation and transport and why they were geoeffective.
The two 2002 events focus on a specific problem in current SEP
research, the origin of variability at high energies. Because the
events were far west, the high-energy particle production reflects
conditions near the Sun. But SEPs above a few tens of MeV/nuc in
these two events have dramatically different spectral and elemental
composition characteristics, even though the associated CMEs and
flares were ostensibly rather similar. Because these events occurred
on the west limb, there were no ejecta observed at Earth. But the
active regions that spawned these events (9906 and 10069,
respectively) also produced many other flares and the CMEs in the ~10
days preceding these events. It is hoped that comparative studies of
the earlier history of these events may also shed light on what made
the west-limb events so different.
These events were also selected to address key science topics or
themes, each of which was discussed by an invited speaker at SHINE
2004. Three themes were selected and their questions and speakers are:
1) Solar Theme: "What are the roles of the magnetic field, dynamics
and evolution in CME initiation?"; George Fisher.
2) Interplanetary Theme: "How can heliospheric observations be used to
better understand the transport and evolution of the solar magnetic
field as it affects CMEs and SEPs?"; Ian Richardson.
3) SEP Theme: "Can we identify solar/IP factors that drive SEP
spectral and compositional variability at high energies?"; Allan Tylka
with short presentations by Nariki Nitta, David Alexander, Matt West,
Mike Andrews, and Mike Reiner.
The Event Leaders have agreed to encourage and facilitate
communications among researchers working on these particular events. A
preliminary website has been established for aiding researchers in
these studies, in particular for depositing pertinent data and for
exchange of models and simulations and general discussions involving
these events and the science themes. The current URL is:
http://cdaw.gsfc.nasa.gov/SHINE_Campain/.
If you wish to become involved with one or more of these events and
science themes, please contact the appropriate Event Leader. Each
leader will maintain an up-to-date email address list for email
communication with the members of his Event study group.
The Community Coordinated Modeling Center (CCMC) has simulated the
SHINE events using the MAS model. The MAS model is a MHD Model of
Solar Corona developed by J. Linker, Z. Mikic, R. Lionello and
P. Riley. The results of these runs can be accessed at the CCMC web
page http://ccmc.gsfc.nasa.gov
by clicking the SHINE Campaign Events link on the side bar menu.
Also, additional runs can be requested by using the Runs on Request
link.
Event Contact
May 12, 1997
Nick Arge (nick.arge@hanscom.af.mil)
(assisted by D. Webb (david.webb@hanscom.af.mil)
May 1, 1998
(includes late April and early May event series) Brian Welsch (welsch@ssl.berkeley.edu)
April 21, 2002
(includes earlier activity from same active region) Allan Tylka (allan.tylka@nrl.navy.mil) and
David Alexander (dalex@rice.edu)
August 24, 2002
(includes earlier activity from same active region) Allan Tylka (allan.tylka@nrl.navy.mil) and
David Alexander (dalex@rice.edu)
Oct-Nov, 2003
Simon Plunkett (simon.plunkett@nrl.navy.mil) and
Bernard Jackson (bvjackson@ucsd.edu)
January 20, 2005
Allan Tylka (allan.tylka@nrl.navy.mil)
For further information, see http://creme96.nrl.navy.mil/20jan05/
<1>
No
<2>
SEP
Date
<3>
SEP
Time
<4>
CME
Time
<5>
Speed
km/s
<6>
Width
Deg
<7>
Region
Location
<8>
Class
Onset
Time
<9>
GOES
X-rays
<10>
SEC
Events
SRS
<11>
Mag. Images
MDI
MWO
<12>
Daily
Movies
LASCO
EIT SXT
<13>
Event
Movies
LASCO EIT
SSW
<14>
Radio
WAVES
Culgoora
HiRAS
<15>
Protons/Ions
EPAM ERNE
GOES I8/Chic
LEMT SIS
ULEIS Fe/O
Event-Int Fe/O
SEPICA
<16>
Electrons
EPAM
<17>
Solar
Wind
<18>
Notes
1
19970512
--:--
06:30
464
Halo
AR 8038
N21W08
C1.3/--
04:42
View
Events
SRS
MDI
MWO
C2
C3
195
SXT
Java Movies
EIT-LASCO
EIT-MDI
MDI
Nobeyama
C2 C2_RD C3 C3_RD 195 195_RD
High/Low
Culgoora
HiRAS
Nancay
OSRA
Spectrum
EPAM ERNE GOES I8/Chic LEMT SIS ULEIS Fe/O EveInt_Fe/O SEPICA_QFe SEPICA_QO
DE1 DE2 DE3 DE4 LE1 LE2 LE3 LE4
SWE
MAG
View
2
19980501
--:--
23:40
585
Halo
AR 8210
S18W05
M1.2/SF
22:36
View
Events
SRS
MDI
MWO
C2
C3
195
SXT
Java Movies
C2 C2_RD C3 C3_RD 195 195_RD
High/Low Culgoora HiRAS
Nobeyama
EPAM ERNE GOES I8/Chic LEMT SIS ULEIS Fe/O EveInt_Fe/O SEPICA_QFe SEPICA_QO
DE1 DE2 DE3 DE4 LE1 LE2 LE3 LE4
SWE
MAG
View
3
20020421
--:--
01:27
2393
Halo
AR 9906
S14W84
X1.5/1F
00:43
View
Events
SRS
MDI
MWO
C2
C3
195
SXT
Java Movies
C2
C3
195
TRACE1
TRACE2
High/Low
Culgoora HiRAS
Nobeyama
GOES_H
ACE/EPAM_H
ACE/ULEIS_Fe&O
Wind/LEMT_Fe&O
ACE/SIS_Fe&O
Fe/O_vs_time
ACE/EPAM
SWE
MAG
View
4
20020824
--:--
01:27
1913
Halo
AR 0069
S02W81
X3.1/1F
00:49
View
Events
SRS
MDI
MWO
C2
C3
195
SXT
Java Movies
C2
C3
195
TRACE1
TRACE2
High/Low
Culgoora HiRAS
Nobeyama
GOES_H
ACE/EPAM_H
ACE/ULEIS_Fe&O
Wind/LEMT_Fe&O
ACE/SIS_Fe&O
Fe/O_vs_time
ACE/EPAM
SWE
MAG
View
5
20031028
--:--
11:30
2459
Halo
AR 0486
S16E08
X17/4B
09:51
View
Events
SRS
MDI
MWO
C2
C3
195
SXT
Java Movies
C2 C2_RD C3 C3_RD 195 195_RD
High+Low
---
---
---
View
Table Notes:
Column 01 (No): Superposition of GOES proton flux, CME height-time plots, GOES X-ray plots for each event.
Column 02 (SEP Date): Click to access various data sources directly.
Column 03 (SEP Time): The SEP time in UTC.
Column 04 (CME Time): The CME time in UTC.
Column 05 (Speed): The CME speed in km/sec.
Column 06 (Width Degrees): The width of the CME from LASCO
Column 07 (Region and Location): NOAA region numer and the flares heliographic position.
Column 08 (Class and Onset Time): GOES X-ray class and start time.
Column 09 (GOES X-rays): 5-min X-rays from GOES.
Column 10 (SEC Events and SRS): NOAA SEC Event List and the Solar Region Summary.
Column 11 (Mag): MDI and MWO map.
Column 12 (Daily Movies): Daily MPEG movies from LASCO, EIT 19.5 nm, and Yohkoh/SXT.
Column 13 (Event Movies): Movies from LASCO, EIT 19.5 nm, and TRACE. RD = running difference. LASCO, TRACE1, and TRACE2 movies were created by M. Andrews, D. Alexander, and N. Nitta, respectively.
Column 14 (Radio):WIND/WAVES high- and low-resolution and
Culgoora spectrograms. The HiRAS plots are high frequency (>20 MHz)
spectra mostly from Hiraiso and WIND/RAD 2.
Column 15 (Protons/Ions): GOES and ACE data were provided by their websites.
Wind/LEMT data were contributed by D.V. Reames. Plots from Tylka et al. (2004, submitted to ApJ).
Column 16 (Electrons): EPAM data from ACE website.
Column 17 (Solar Wind): Wind/SWE data from NSSDC, courtesy of K. Ogilvie.
Column 18 (Notes): View and/or edit the comments files.
Contact: Nat Gopalswamy - gopals@fugee.gsfc.nasa.gov
Webmaster: Seiji Yashiro - yashiro@cdaw.gsfc.nasa.gov
Date: 25-Feb-2004