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. Veselovsky1,2, S.M. Agayan3, Sh. R. Bogoutdinov3, A.D. Gvishiani3, R.G. Kulchinskiy3, V.G. Petrov4, O.S. Yakovchouk1

(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 (http://dbserv.sinp.msu.ru/apev/fullist.htm) 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 Scheme of Discrete Mathematical AnalysisDiscrete Mathematical Analysis

Fuzzy comparisons onpositive numbers

Nearness in finite metrical space

Limit in finite metrical space

Density as measure oflimitness

Smoothtime series.Equilibrium

Monotonous time series

Fuzzy logicand geometry on

time series:geometrymeasures

Separation of dense subset.

Crystal. Monolith.

Clusterization.Rodin

Predicationof time series.

Forecast

Anomalies ontime series.

DRAS. FLARS. FCARS

Extremums on

time series.

Convextime series

Search of linearstructure.Tracing 2

Global level– search of elevations on rectification

Local level– building record rectification

Record

Logic Logic of the interpreterof the interpreter

5

Local level Local level building record rectification building record rectification

Define: ( ) { }hR t R kh , ( ) { ( ) }ky t y kh y , 0,1,2,k hT R .

0 - local scanning parameter, , , , ,kk k ky y y y - record fragment.

Definition:

1) Functional ВР y is non-negative mapping : J R , defined on the set of its fragments

2 1kJ y .

2) Superposition ( ) ( )def

k kyk y y k is rectification y on the base .

1. Length of scanning fragment: 1

1

kk

j jj k

L y y y

2. Energy of scanning fragment: 2k

kj k

j k

E y y y

, where 1

2 1

k

k jj k

y y

3. Oscillation of scanning fragment: ( ) max mink k

kj j

j kj kO y y y

.

6

Example of using FCARS algorithm on set of observatoriesExample of using FCARS algorithm on set of observatoriesPeriod: January 1-31 2005. Component X

Hornsund (HRN)

Abisko (ABK)

Nurmijarvi (NUR)

Surlari (SUR)

Antananarivo (TAN)

Port Alfred (CZT)

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CASE 1

Complicated geomagnetic storm (consisting of two parts) of November 8-11, 2004.

CASE 2 Isolated Geomagnetic storm of May 15, 2005.

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.- 08-Nov-2004 06:00:00 Dxt=- 372.823 nT

HER HON KAK SJG Dxt

-101,977 -187,121 -133,04 -294,667 -179,201

-42,2067 -274,287 -168,407 -252,576 -184,369

-75,476 -313,647 -214,775 -285,509 -222,352

-134,174 -377,606 -284,739 -282,826 -269,836

-178,182 -471,419 -373,583 -329,765 -338,237

-282,734 -487,434 -420,486 -270,259 -365,228

-333,73 -444,527 -408,14 -304,894 -372,823

-355,865 -380,609 -354,861 -282,861 -343,549

-396,214 -353,516 -374,996 -159,42 -321,036

-364,833 -306,578 -353,068 -173,889 -299,592

-320,551 -201,067 -264,91 -157,671 -236,05

CASE 1: Part 1

HER HON KAK SJG Dxt

-62,7475 -105,215 -76,3288 -167,112 -102,851

-38,2508 -202,187 -158,922 -308,661 -177,005

-164,65 -209,47 -201,964 -274,226 -212,578

-169,719 -168,413 -174,622 -217,152 -182,476

-156,237 -182,822 -150,403 -205,917 -173,845

-118,002 -167,838 -128,512 -191,738 -151,522

-101,158 -153,256 -109,839 -180,009 -136,066

-90,3041 -195,085 -115,679 -191,795 -148,216

-89,4801 -206,239 -121,472 -199,267 -154,114

-91,7383 -216,039 -152,9 -140,07 -150,187

-112,466 -282,026 -223,445 -158,112 -194,012

-148,524 -320,236 -278,647 -204,206 -237,903

-210,83 -297,94 -333,446 -187,955 -257,543

-268,906 -287,085 -382,851 -90,3296 -257,293

-323,606 -269,177 -345,162 -96,0022 -258,487

-332,907 -234,49 -322,301 -168,266 -264,491

-281,711 -180,44 -288,922 -178,288 -232,34

-277,76 -181,535 -281,618 -193,073 -233,497

- Second Geomagnetic Storm Development (Equatorial Regions) .- Asymmetry.- 10-Nov-2004 10:00:00 Dxt=- 264.491 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

HER HON KAK SJG Dxt

-11,7983 -12,7378 -9,25427 -9,19637 -10,7467

21,1137 2,59924 6,23173 21,1286 12,7683

74,46 34,112 36,0521 72,5029 54,2817

47,8945 34,2465 44,7532 47,9502 43,7111

28,0537 33,1275 54,8777 37,5109 38,3925

-130,076 -68,5879 -56,6944 25,2686 -57,5224

-217,569 -305,182 -268,671 -116,066 -226,872

-160,864 -339,149 -311,07 -164,259 -243,836

-173,428 -270,083 -283,159 -154,662 -220,333

-170,429 -210,847 -195,102 -153,273 -182,413

-169,825 -193,133 -174,906 -155,331 -173,299

-160,656 -177,975 -157,21 -149,12 -161,24

-160,072 -165,753 -146,344 -153,214 -156,346

-138,034 -154,687 -132,706 -153,591 -144,754

-120,281 -144,838 -120,654 -148,011 -133,446

-114,464 -122,557 -105,228 -126,479 -117,182

- Geomagnetic Storm Development (Equatorial Regions) .- Symmetry.- 15-May-2005 08:00:00 Dxt=- 243.836 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