ACSAtmospheric and Climate Sciences2160-0414Scientific Research Publishing10.4236/acs.2013.34063ACS-38225ArticlesEarth&Environmental Sciences Solar Activity, Solar Wind and Geomagnetic Signatures ean-LouisZerbo1*FrédéricOuattara2ChristineAmory Mazaudier3Jean-PierreLegrand4JohnD. Richardson5Ecole Normale Supérieure de l’Université de Koudougou, Koudougou, Burkina FasoUniversité Polytechnique de Bobo-Dioulasso, Bobo-Dioulasso, Burkina FasoLPP-Laboratoire de Physique des Plasmas/UPMC/Polytechnique/CNRS, Saint-Maur-des-Fossés, FranceKavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, USAInstitut National des Sciences de l’Univers (INSU), Paris, France* E-mail:jeanlouis.zerbo@gmail.com(EZ);260820130304610617September 13, 2013October 10, 2013 October 18, 2013© Copyright 2014 by authors and Scientific Research Publishing Inc. 2014This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/

The present study investigates solar events through geomagnetic activity and physical processes on the Sun: 1) Quiet activity (QA) related to the slow solar wind, 2) Recurrent activity (RA) related to high and moderate speed solar wind streams from coronal holes, 3) Shock activity (SA) identified by observations of SSCs and 4) Unclear activity (UA) which contains all activity not covered by the first three cases. For recent cycles, we analyze and emphasize some important results: Quiet activity is predominant for cycle 23, comprising 40% of the total activity and over 80% of the activity near solar minimum. Shock and recurrent activity contributions to total geomagnetic activity are largest in cycle 20. The most fluctuating events are observed during cycles 21 and 22. Throughout solar cycle 23, the contribution, from each type of activity, differs from recent solar cycles, with larger percentages of quiet and recurrent activity and less unclear activity. These percentages are similar to those in solar cycles observed in the late 1800s. Since 1963, solar wind data are available. We analyze the distribution of the solar wind velocity for each geomagnetic class of activity and find that: 1) Within each activity type aa does not depend on V, 2) Approximately 80% of the solar wind has V < 450 km/s for QA and 80% of the solar wind has V > 450 km/s for RA, 3) SA and UA both have 60% of the solar wind V > 450 km/s. We found the following conditions for all four solar cycles: 1) For QA 95% of solar wind speeds are in the range 399 ± 69 km/s, 2) For RA 95% of the solar wind speeds range from 582 ± 110 km/s, 3) For SA 95% of the solar wind velocities are order of 482 ± 101.4 km/s, and 4) For UA 95% of solar wind speeds are 480 ± 85.82 km/s. These results confirm the classification scheme that QA reflects slow wind effects, RA effects high wind stream and UA answers to the fluctuations between high wind stream (~60%) and slow wind (~40%). The study shows that high wind stream (~60%) and slow wind (~40%) are both registered for SA.

Solar Wind; Geomagnetic Activity; Solar Activity; Geomagnetic Index aa1. Introduction

Geomagnetic activity may be divided into four classes: quiet, recurrent, shock, and fluctuating/unclear [1-7]. Legrand and Simon [1] and Simon and Legrand [2] proposed the first classification of geomagnetic activity for the period 1868-1977 using pixel diagram. Pixel diagrams represent the geomagnetic data as a function of solar activity for each solar rotation (27 days) and give an overview of the geoeffectiveness of solar events. Previous pixel diagrams were built using the the geomagnetic aa index defined and explained by Mayaud [8-10], the times of SSCs (Sudden Storm Commencements) and the strong correlation between the aa index and solar wind established by Svalgaard [11]. Important works [12, 13] show that geomagnetic activity has two components. The first component varies in phase with the sunspot cycle and the second begins immediately after the maximum of the sunspot cycle. Following Legrand and Simon [1]’s works, Ouattara and Amory-Mazaudier [6] investigate the time variation of solar activity from 1968 to 1996. Very recent study [7] extends and improves the classification of geomagnetic activity, and we use it to investigate the time profiles of geomagnetic activity during solar cycles 20, 21, 22, and 23. We also study the statistical distribution of solar wind speeds in each class of geomagnetic activity for cycles 20 to 23.

2. Data and Methodology2.1. Data

The times of sudden substorm commencements (SSC), which are rapid increases in the magnetic field observed at the ground per day are taken from http://isgi.latmos. ipsl.fr/. The solar wind speed and the international sunspot number (SSN) are obtained from http://omniweb. gsfc.nasa.gov/form/dx1.html.

2.2. Geomagnetic Classification Methodology

Legrand and Simon [1] justified their use of the aa index to classify geomagnetic activity on two features: 1) The contribution of solar wind shocks to geomagnetic activity can be determined from ground-based observations of SSCs; time periods with SSCs are defined to have shock activity (SA). 2) The strong correlation between the aa index [8-10] and the solar wind speed [11]. This correlation allows the data to be divided into three classes of geomagnetic activity: 1) low-speed solar wind, 2) variable-speed solar wind and 3) high speed solar wind. Zerbo J.-L. et al. [7] consider these criteria, the contributions of magnetic clouds, and the contribution of moderate speed wind streams to improve the classifications [1]. We divide the solar wind into classes using the aa index and then use the results to study correlations with solar wind parameters. Figure 1 illustrates the pixel diagrams of the aa indices. The top panel illustrates the year 1974a very active year [7], and the bottom panel the year 2009, a very geomagnetic quiet year at the minimum of the sunspot cycle. The pixel diagrams display the daily averages of aa as a table. Each horizontal line contains 27 days corresponding to a 27-day Bartels solar rotation with two days of overlap on each end. The number in each square is the mean daily value of the aa index and the squares are color coded based on these values using the color bar shown in Figure 1. Circles show the days when SSCs were observed. This diagram, similar to a Bartels diagram, simplifies the identification of geomagnetic phenomena. From the pixel diagrams, the class of activity, QA, SA, RA or UA, for each day is determined. The 1974 pixel diagram illustrates the different classes of activity. The use of these diagrams is best explained by Zerbo J.-L. et al. [7]. 1) Quiet activity days are defined as days when aa < 20 nT (colors white and blue on Figure 1). The three other classes (shock activity, recurrent activity and fluctuating activity) constitute the disturbed geomagnetic activity classes which occur on days when aa ≥ 20 nT. These classes are distinguished as follows:

2) Recurrent (stream) activity corresponds in the pixel diagrams to days where aa ≥ 20 which repeat at the same solar longitude for at least two consecutive solar rotations. This class is driven by fast solar wind from coronal holes which persist for more than one solar rotation. SSCs are not observed during the main phases of storms driven by recurrent streams. An example of RA is shown in Figure 1 (top panel).

3) Shock activity is defined to occur on days when SSCs are observed and up to 3 days after the shock passage if aa remains > 20 nT. SA is driven by CMEs on the Sun which often produces high solar wind speeds. An example of shock activity which persists for three days is shown in Figure 1 (top panel).

4) Unclear activity includes all times which do not fit the criteria for the other three classes and is thus a mixed class of disturbances. This activity results from variable moderate and high-speed solar wind and may be related to the fluctuations of the heliospheric neutral sheets.

3. Results3.1. Geomagnetic Classes, Their Activity Variation during the Solar Cycles 20, 21, 22, and 23

In this section, we study the four latest solar cycles using aa indices and solar wind data. Figure 1 shows the large difference in solar activity between the beginning of the declining phase in 1974 and very quiet recent solar minimum in 2009.

Figure 2 extends the Legrand and Simon [1]’s work to include 32 more years of data. It shows the yearly percentage of occurrence of each class of geomagnetic activity from 1868 through 2009. Figures 2(a)-(e) show long time variations of QA, RA, SA, FA, and SSN respectively (classification of Legrand and Simon, 1989). QA decreases with time from 1868 until solar cycle 22 and then strongly increases at the end of solar cycle 23.

ReferencesJ. P. Legrand and P. A. Simon, “Solar Cycle and Geomagnetic Activity: A Review for Geophysicists. Part I. The Contributions to Geomagnetic Activity of Shock Waves and of the Solar Wind,” Annales Geophysicae, Vol. 7, No. 6, 1989, pp. 565-578.P. A. Simon and J. P. Legrand, “Solar Cycle and Geomagnetic Activity: A Review for Geophysicists Part II. The Solar Sources of Geomagnetic Activity and Their Links with Sunspot Cycle Activity,” Annales Geophysicae, Vol. 7, No. 6, 1989, pp. 579-594.I. G. Richardson, H. V. Cane and E. W. Cliver, “Sources of Geomagnetic Activity during Nearly Three Solar Cycles (1972-2000),” Journal of Geophysical Research, Vol. 107, No. A8, 2002, pp. 107-118. http://dx.doi.org/10.1029/2001JA000504I. G. Richardson, E. W. Cliver and H. V. Cane, “Sources of Geomagnetic Activity over the Solar Cycle: Relative Importance of Coronal Mass Ejections, High-Speed Streams, and Slow Solar Wind,” Journal of Geophysical Research, Vol. 105, No. A8, 2000, pp. 200-213. http://dx.doi.org/ 10.1029/1999JA000400F. Ouattara, C. Amory-Mazaudier, M. Menvielle, P. Simon and J.-P. Legrand, “On the Long Term Change in the Geomagnetic Activity during the XXth Century,” Annales Geophysicae, Vol. 27, No. 5, 2009, pp. 2045-2051. http://dx.doi.org/10.5194/angeo-27-2045-2009F. Ouattara and C. Amory-Mazaudier, “Solar-Geomagnetic Activity and Aa Indices toward a Standard,” Journal of Atmospheric and Solar-Terrestrial Physics, Vol. 71, No. 17-18, 2009, pp. 1736-1748. http://dx.doi.org/10.1016/j.jastp.2008.05.001J. L. Zerbo, C. Amory-Mazaudier, F. Ouattara and J. Richardson, “Solar Wind and Geomagnetism, toward a Standard Classification 1868-2009,” Annales Geophysicae, Vol. 30, 2012, pp. 421-426. http://dx.doi.org/10.5194/angeo-30-421-2012P. N. Mayaud, “Une Mesure Planétaire d’Activité Magnétique Basée sur deux Observatoires Antipodaux,” Annales Geophysicae, Vol. 27, 1971, p. 71.P. N. Mayaud, “A Hundred Series of Geomagnetic Data, 1868-1967,” IAGA Bulletin, Vol. 33, Zurich, 1973, p. 251.P. N. Mayaud, “Deviation, Meaning, and Use of Geomagnetic Indices,” Geophysical Monograph Series, Vol. 22, Washington DC, 1980, p. 154.L. Svalgaard, “Geomagnetic Activity: Dependence on Solar Wind Parameters,” In: J. B. Zirker, Ed., Coronal Holes and High Speed Wind Streams, Colorado Association University Press, Boulder, 1977, pp. 371-432.P. A. Simon and J. P. Legrand, “A Two Component Solar Cycle,” Solar Physics, Vol. 131, 1992, pp. 187-209.J. P. Legrand and P. A. Simon, “Toward a Model of Two-Component Solar Cycle,” Solar Physics, Vol. 141, 1991, pp. 391-410.J. Feynman and N. U. Crooker, “The Solar Wind at the Turn of the Century,” Nature, Vol. 275, No. 5681, 1978, pp. 626-627. http://dx.doi.org/10.1038/275626a0L. Svalgaard and E. W. Cliver, “Interhourly Variability Index of Geomagnetic Activity and Its Use in Deriving Long-Term Variation of Solar Wind Speed,” Journal of Geophysical Research, Vol. 112, No. A10, 2007, Article ID: A10111. http://dx.doi.org/10.1029/2007JA012437J. P. Legrand and P. A. Simon, “Some Solar Cycle Phenomena Related to the Geomagnetic Activity from 1868 to 1980, I. The Shock Events, or the Interplanetary Expansion of the Toroidal Field,” Astronomy and Astrophysics, Vol. 152, No. 2, 1985, pp. 199-204.P. N. Mayaud, “The aa Indices: A 100-Year Series Characterizing the Magnetic Activity,” Journal of Geophysical Research, Vol. 77, No. 34, 1972, pp. 6870-6874. http://dx.doi.org/10.1029/ JA077i034p06870