Logo

VarSITI: Resources recommended by ISEST-MiniMax24

The use of “Resource” for public education efforts and non-commercial purposes is encouraged.
If you want to use the “Resource” in a paper, book, or any kind of electronic publication,
please give appreciate credit to the "Provider".

Ground-based:

The ISEST Event List
WEB address: http://solar.gmu.edu/heliophysics/index.php/The_ISEST_Event_List

Providers: © George Mason Universty Space Weather Lab's Heliophysics
  © VarSITI/ISEST-MiniMax24 team


This is a list of ICMEs arranged by year. The ICMEs are cataloged by the first appearence of a signature in-situ. (Image Data & In-Situ Data) To add an event that is not present in the list, follow the how to guide at Creating A New Event Page

Description:

The ISEST Master CME List
WEB address: http://solar.gmu.edu/heliophysics/index.php/The_ISEST_Master_CME_List

Providers: © George Mason Universty Space Weather Lab's Heliophysics
  © VarSITI/ISEST-MiniMax24 team


That's a big table containing details and links to movies as follows:

 1. ICME Event Start- Beginning of the ICME signature in-situ at ACE

 2. ICME Event End- Estimated End of ICME signature in-situ at ACE

 3. CME in LASCO- First appearance of the CME in LASCO C2, or STEREO COR2 in the event of a LASCO data gap.

 4. ICME TYPE- Describes the signature in-situ, Shock Front (SH), MC (Magnetic Cloud), EJ (CME Ejecta Front)

 5. AR- The Source Active region of the CME, if there is one

 6. Surface Location- The location of the Active Region or, if there is no AR, the approximate location of the eruption.

 7. Flare Magnitude- If the CME is associated with a flare, the strength of the flare.

 8. Flare Onset Time- The beginning of the flare

 9. CDAW VEL C2*- The velocity of the CME, as determined by the CDAW CME Catalog

10. SEEDS VEL C2*- The velocity of the CME, as determined by the SEEDS C2 Catalog

11. SEEDS VEL A*- The velocity of the CME, as determined by the SEEDS STEREO Catalog

12. SEEDS VEL B*- The velocity of the CME, as determined by the SEEDS STEREO Catalog

13. AVG. VEL- The average velocity of the CME as calculated by determining the time of the CME in C2 and the beginning of the signature in-situ

14. Velocity- The average velocity of the ejecta at ACE

15. DST Peak/DST Peak Time- The lowest value of the DST index and the time it occurs (as long as the peak is below -40)

16. Ejecta Start Time- The beginning of the CME Ejecta in-situ (if there is no shock this is the same as the ICME start time)

17. Quality Rating- This denotes the quality of the event's signature in-situ, 1 is the best, 3 is the worst.

18. In-Situ Link- A link to the in-situ data for the event

19. C2 Link- A link to a movie of the CME in LASCO C2

20. COR2 Link- A link to a movie of the CME in STEREO COR2

21. EIT/AIA Link- A link to a movie of the eruption on the Sun as seen by either the SOHO EIT or SDO AIA instrument

Description:


Kanzelhöhe Observatory in Austria
WEB address: http://cesar.kso.ac.at/

Providers: © Kanzelhöhe Observatory, UNI Graz
  © Institute of Geophysics, Astrophysics and Meteorology, UNI Graz


Provides images and/or data files for:
Latest Images of the Sun; Latest H-α (ESA SSA); Latest Sunspot Summary;
Last Week Photosphere and Chromosphere;
Sunspot Numbers; Sunspot Drawings; Whitelight and Hα;
CaIIK 4 Megapixel Camera Photoheliographs at 393.37 nm
Flare detection and Filament eruption detection

Solar Ephemeris Calculation Utility
Description:


Solar Monitor
WEB address: http://www.solarmonitor.org/
Provider: © Solar Physics Group, Trinity College Dublin

These pages contain near-realtime and archived information on active regions and solar activity.

Images of the sun from different satellites and in different wavelengths.
You can: (1) highlight the active areas, (2) select a satellite, (3) select the date.

Today's NOAA Active Regions

Flare Forecast

Further information on SolarMonitor.org can be found in
Peter T. Gallagher, Y.-J. Moon, Haimin Wang, Active-Region Monitoring and Flare Forecasting–I. Data Processing and First Results, (2002) Solar Physics, Vol.209, Iss.1, pp.171–183 (click here)

Description:

Resources

Forecasting the Arrival of ICMEs: The Drag-Based Model
WEB address: http://oh.geof.unizg.hr/DBM/dbm.php
Provider: © Hvar Observatory

The purpose of the basic form of the model is to provide a prediction of the arrival time and impact speed at the Earth. Calculations are based on the assumption that the dominant force in the heliospheric dynamics of ICMEs is the magnetohydrodynamical equivalent of the aerodynamic drag. For a given set of input parameters it provides the ICME Sun-Earth transit time, the arrival time, and the impact speed.

The advanced form of DBM provides this output for any target in the heliosphere and takes into account also the shape of ICME employing the so-called cone-geometry.

Mandatory input parameters:
start_date - CME start date, allowed format: DD-MM-YYYY (DD - days from 01 to 31, MM - months from 01 to 12, YYYY - years from 1900 to 2100).
start_time - CME start time (UTC), allowed format: hh:mm (hh - hours from 00 to 23, mm - minutes from 00 to 59).
R0 - starting radial distance of CME, unit: Rs (Sun diameter), allowed format: number in range from 1 to 214.
v0 - speed of CME at R0, unit: km/s, allowed format: number in range from 50 to 5000.
gamma - drag parameter, unit: 10-7 km-1, allowed format: number in range from 0.1 to 100.
w - asymptotic solar wind speed, unit: km/s, allowed format: number in range from 200 to 800.
Rtarget - target heliocentric distance, unit: AU, allowed format: number in range from 0.01 to 50.

Documentation and description of calculation method for DBM you can find here.

Description:


Forecast of Solar Wind Parameters and Geomagnetic Disturbances SoWi–PaGe (hourly updated)
WEB address: http://www.uni-graz.at/igam-sophy/comesep/solarwind/ Not available longer
Provider: © IGAM-Kanzelhöhe Observatory, UNI Graz

Automated forecasts of high speed solar wind streams (HSS) arriving at Earth. The forecast, made up to four days in advance, is based on coronal hole observations. The information of coronal hole areas is extracted from SDO/AIA 193 images via histogram-based thresholding methods. For Earth-affecting HSS only areas of coronal holes within a slice of +/-7.5° around the central meridian are taken into account.

The area is used to calculate solar wind and geomagnetic parameters at a distance of 1 AU (shown as blue crosses in right panels). Graphs present the total magnetic field strength B and southward component Bz, the proton speed v and the related geomagnetic disturbances in the form of the Dst index.

For a full description of the method see
Rotter, T., Veronig, A.M., Temmer, M. and Vrsnak, B., Relation Between Coronal Hole Areas on the Sun and the Solar Wind Parameters at 1 AU (2012) Solar Physics, Vol.281, Iss.2, pp.793–813 DOI: 10.1007/s11207-012-0101-y

Calculate for individual CH areas the arrival of a HSS at 1 AU by using the tool from Hvar Observatory: CH/CIR Model

Description:


Forecast of Solar Wind and Geomagnetic Activity "CH/CIR Model" (hourly updated)
WEB address: http://oh.geof.unizg.hr/CH/ch.php
Provider: © Hvar Observatory

Forecasts of:
SW speed (4-day), SW magnetic field (2-day),
six-hourly mean of Dst and Ap (3-day),
daily mean of Dst (4-day),
hourly peak value of Dst (4-day)

For a full description of the method see
Rotter, T., Veronig, A.M., Temmer, M. and Vrsnak, B., Relation Between Coronal Hole Areas on the Sun and the Solar Wind Parameters at 1 AU (2012) Solar Physics, Vol.281, Iss.2, pp.793–813 DOI: 10.1007/s11207-012-0101-y

Description: