IAGA Symposium A12.2 Geomagnetic networks, computation and definition of products for space weather and space climate Melbourne, Australia, 2011 GLOBAL, REGIONAL AND LOCAL DYNAMICS OF STRONG GEOMAGNETIC STORMS I.S. Veselovsky 1,2, S.M. Agayan 3, Sh. R. Bogoutdinov 3, A.D. Gvishiani 3, R.G. Kulchinskiy 3, V.G. Petrov 4, O.S. Yakovchouk 1 (1) Institute of Nuclear Physics, Moscow State University, Russia (2) Space Research Institute (IKI), Russian Academy of Sciences, Russia (3) Geophysical center of RAS, Russian Academy of Sciences, Russia (4) IZMIRAN, Russian Academy of Sciences, Russia 1

We analyze INTERMAGNET data about strongest geomagnetic storms observed during 23-rd solar cycle. We compare this data set both statistically and individually with solar, heliospheric and magnetospheric conditions compiled in our data base APEV ( with the aim to investigate general and specific properties of the events, which demonstrate common features and broad diversity of situations. New methods of analysis and dynamical visualization of big data sets related to geomagnetic storms are presented. ABSTRACT

Scheme of Discrete Mathematical Analysis Fuzzy comparisons on positive numbers Nearness in finite metrical space Limit in finite metrical space Density as measure of limitness Smooth time series. Equilibrium Monotonous time series Fuzzy logic and geometry on time series: geometry measures Separation of dense subset. Crystal. Monolith. Clusterization. Rodin Predication of time series. Forecast Anomalies on time series. DRAS. FLARS. FCARS Extremums on time series. Convex time series Search of linear structure. Tracing 2

Global level– search of elevations on rectification Local level– building record rectification Record Logic of the interpreter 5

Local level building record rectification 6

Example of using FCARS algorithm on set of observatories Period: January Component X Hornsund ( HRN) Abisko (ABK ) Nurmijarvi ( NUR) Surlari ( SUR) Antananarivo ( TAN) Port Alfred ( CZT) 11

CASE 1 Complicated geomagnetic storm (consisting of two parts) of November 8-11, CASE 2 Isolated Geomagnetic storm of May 15, Acknowledgement. We are grateful to Prof. Kalevi Mursula who provided his Dxt calculated indexes which represent corrected version of Dst. More detailed comparative investigation is performed for two events:

Complicated Geomagnetic Storm of November 8-11, 2004 consisting of two parts Heliospheric Current Sheet and Multiple Eruptions on the Sun. Solar Wind and Interplanetary Magnetic Field. Two coronal mass ejections. North-South magnetic field rotation during the flux rope crossings in the solar wind. CASE 1

- First Geomagnetic Storm Development (Equatorial Regions). - Symmetry Nov :00:00 Dxt= nT HERHONKAKSJGDxt -101, , ,04-294, , , , , , , , , , , , , , , , , , , , , , , , , , , ,73-444, ,14-304, , , , , , , , , , ,42-321, , , , , , , , ,91-157, ,05 CASE 1: Part 1

HERHONKAKSJGDxt -62, ,215-76, , , , , , , , ,65-209,47-201, , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , ,9-140,07-150, , , , , , , , , , , ,83-297,94-333, , , , , ,851-90, , , , ,162-96, , , ,49-322, , , , ,44-288, , , ,76-181, , , ,497 - Second Geomagnetic Storm Development (Equatorial Regions). - Asymmetry Nov :00:00 Dxt= nT CASE 1: Part 2

CASE 1: Heliospheric Current Sheet and Multiple Eruptions on the Sun

CASE 1: Solar Wind and Interplanetary Magnetic Field

CASE 1: Dynamic analysis using DMA approach and GIS technology

HERHONKAKSJGDxt -11, ,7378-9, , , ,11372,599246, ,128612, ,4634,11236,052172,502954, ,894534,246544,753247,950243, ,053733,127554,877737,510938, ,076-68, ,694425, , , , , , , , , ,07-164, , , , , , , , , , , , , , , , , , , ,21-149,12-161, , , , , , , , , , , , , , , , , , , , ,182 - Geomagnetic Storm Development (Equatorial Regions). - Symmetry May :00:00 Dxt= nT CASE 2: Isolated Geomagnetic storm of May 15, 2005

CASE 2: Heliospheric Current Sheet and Multiple Eruptions on the Sun

CASE 2: Solar Wind and Interplanetary Magnetic Field

CASE 2: Dynamic analysis using DMA approach and GIS technology

The main ring current started to develop with a large delay (~3 hours) after the interplanetary shock arrival to the Earth and the sudden commencement. It is because of the interplanetary electric field unfavorable orientation against the magnetosphere (positive Bz). CASE 2 Time delay

Case 1. Strongly delayed (half a day!) irregular evelopment. Longitudinal asymmetry. Storm like a Substorm. Similar case – Carrington Event (September 1859) Case 2. Nearly simultaneous storm development on the globe. Longitudinal symmetry. Ring current. Dst or Dxt. What do we see on the Equator?

The ring current is not always a main contributor to the equatorial geomagnetic perturbations during the development and the main phase of strong geomagnetic storms. Conclusion 1

Global, regional and local properties of individual geomagnetic storms have common and specific features depending on the driving external conditions in the heliosphere and on the Sun. Based on our analysis we conclude that geomagnetic proxies could serve as an important source of indirect information about solar and heliospheric activity in the past, when direct observations were not available. Reliability and accuracy of physical interpretations and models essentially depend on the quality of geomagnetic input information and assumed conditions on the ground, in the ionosphere, the magnetosphere, the solar wind and on the Sun. Well calibrated INTERMAGNET data in combination with other ground based measurements and multipoint satellite missions are promising for the future progress towards better and broader scientific and technical use of geomagnetic information. Suggested an new approach to analysis of geomagnetic events based on data from the global network of Intermagnet observatories using fuzzy mathematics and GIS technology. Thank you! CONCLUSIONS