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Current Sheets from Ulysses Observation Ann. Geophys., 29, 237–249, 2011 www.ann-geophys.net/29/237/2011/ Annales doi:10.5194/angeo-29-237-2011 Geophysicae © Author(s) 2011. CC Attribution 3.0 License. Current sheets from Ulysses observation B. Miao1,3, B. Peng2, and G. Li1,2 1CSPAR, University of Alabama in Huntsville, Huntsville, AL 35805, USA 2Department of Physics, University of Alabama in Huntsville, Huntsville, AL 35805, USA 3CAS Key Laboratory of Basic Plasma Physics, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China Received: 1 October 2010 – Revised: 5 January 2011 – Accepted: 25 January 2011 – Published: 2 February 2011 Abstract. Current sheet is a significant source of solar wind very difficult. In particular, studying the dynamical evo- MHD turbulence intermittency. It has long been recognized lution of MHD turbulence in terrestrial laboratory experi- that these structures can arise from non-linear interactions ments is difficult because these experiments are short lived. of MHD turbulence. Alternatively, they may also be relic In comparison, solar wind provides a natural laboratory to structures in the solar wind that have a solar origin, e.g., study MHD turbulence in a collisionless plasma. In partic- magnetic walls of flux tubes that separate solar wind plasma ular, the launches of multiple spacecraft in the past several into distinct parcels. Identifying these structures in the solar decades, noticeably Voyager, Helios, WIND, Ulysses and wind is crucial to understanding the properties of the solar Cluster, have accumulated a significant amount of plasma wind MHD turbulence. Using Ulysses observations we ex- and magnetic field data These data have revealed valuable amine 3-year worth of solar wind magnetic field data when information about MHD turbulence and its dynamical evolu- the Ulysses is at low latitude during solar minimum. Ex- tion. tending the previous work of Li (2007, 2008), we develop an A central topic of the solar wind MHD turbulence is inter- automatic data analysis method of current sheet identifica- mittency. In a collisionless plasma such as the solar wind, in- tion. Using this method, we identify more than 28000 current termittency arises because the fluctuations of magnetic field sheets. Various properties of the current sheet are obtained. or fluid velocity are not scale invariant as conjectured in These include the distributions of the deflection angle across the first hydrodynamic turbulence theory Kolmogorov (1941) the current sheet, the thickness of the current sheet and the (hereafter K41 theory). Roughly speaking, intermittency re- waiting time statistics between current sheets. flects how turbulence is unevenly distributed in space. Math- Keywords. Solar physics, astrophysics, and astronomy ematically, intermittency describes how a structure function Sp(l) p Sp(l) p (Magnetic fields) – Space plasma physics (Discontinuities; q varies with the order . Here q is the -th order q q Turbulence) structure function defined for a physical quantity ( can be e.g. v|| or B of solar wind measurement) through, p p ζp Sq (l) =< |q(x)−q(x +l)| >≈ l . (1) 1 Introduction p In the above, the quantity ζp is the scaling exponent of Sq (l) Magnetohydrodynamics (MHD) turbulence has been a cen- and is in general a function of p. In the absence of inter- = = tral topic of space plasma physics (see Tu and Marsch, 1995; mittency, ζp p/m where m 3 for normal fluid and 4 for Goldstein et al., 1995; Bruno and Carbone, 2005, for exten- magnetofluid. Any deviation from this linear dependence in- sive reviews). Because of the presence of a strong mag- dicates the presence of intermittency. netic field, MHD turbulence differs in many aspects from In the context of solar wind MHD turbulence, systematic the hydrodynamic turbulence (Iroshnikov, 1964; Kraichnan, study of intermittency was first done by Burlaga. In a series 1965; Biskamp, 1993). Various technical difficulties have of papers (Burlaga, 1991a,b,c), using Voyager data at var- made studying of MHD turbulence in terrestrial laboratories ious heliocentric distances, Burlaga showed that the ζp as- sociated with fluctuating solar wind speed is not linear with p. Marsch and Liu (1993) analyzed Helios data in the in- Correspondence to: G. Li ner heliosphere and showed that not only intermittency ex- ([email protected]) ists in the solar wind, but its strength can also differ much Published by Copernicus Publications on behalf of the European Geosciences Union. 238 B. Miao et al.: Current sheets from Ulysses observation depending on plasma properties: small scales are more inter- spheric structures, making a remarkable connection between mittent than large scales and slow wind is more intermittent structures in the solar wind and those on the surface of the than fast wind. Since the work of Marsch and Liu (1993), Sun. studies on the intermittent character of solar wind have been While the analysis of Bruno et al. (2001) showed that cur- widely reported (e.g. Marsch and Tu, 1994, 1997; Carbone rent sheets are common in the solar wind and they may be the et al., 1995a,b; Ruzmaikin et al., 1995; Tu et al., 1996; Hor- boundaries of flux tubes, there are alternative views about bury et al., 1996, 1997; Bruno et al., 1999, 2001, 2003, 2004; the origin of current sheets. For example, numerical MHD Veltri et al., 2005; Salem et al., 2007, 2009). Relating in- simulations by Zhou et al. (2004) showed that current sheets termittency with specific solar wind turbulence models has emerge as the dynamical evolution of the nonlinear interac- been reported by Ruzmaikin et al. (1995). In this paper, the tions of the solar wind MHD turbulence, i.e. the generation of authors showed that if one reduces the measured spectral in- current sheet can be spontaneous. Similarly study by Chang dex of magnetic field fluctuations by an amount governed by et al. (2004) also showed that starting from an isotropic ini- the intermittency scaling exponent, then the reduced power tial MHD turbulence state, non-linear interactions in the solar spectral index will yield a scaling agreeing with the random- wind can lead to the emergence of various coherent struc- phase Alfvenic´ turbulence model of Kraichnan (1965). Later, tures, including current sheet. These studies (Zhou et al., Tu et al. (1996) tried to integrate the p-model of Meneveau 2004; Chang et al., 2004) suggested that current sheet is an and Sreenivasan (1987) to the Tu (1988) model of a develop- intrinsic property of the solar wind MHD turbulence. In con- ing solar wind. Clearly, these works suggested that to under- trast, advocating Bruno et al. (2001)’s idea, Borovsky (2008), stand the solar wind turbulence a good understanding of the on examining one-year worth magnetic field data from the solar wind MHD intermittency is necessary. ACE spacecraft, has found a clear signature of two popula- Observationally, a very important intermittent structure in tion of current sheets with one extending to large angle sepa- the solar wind is current sheet. A current sheet is a 2-D rations. Borovsky (2008) suggested that these current sheets structure where the magnetic field direction changes signif- are the “magnetic walls” of flux tubes in the solar wind and icantly from one side to the other. Using a Haar wavelets they are relic structures which can be traced back to the sur- technique and magnetic field and fluid velocity data from face of the Sun. In this picture, current sheets are carried out ISEE space experiment, Veltri and Mangeney (1999) calcu- by the solar wind as passive structures. The plasma in the lated solar wind power spectra and structure functions for a solar wind are bundled in “spaghetti-like” flux tubes. Such time range between 1 min to about 1 day. They found that a picture is consistent with some old ideas proposed over 40 in solar wind (a magneto-fluid) the most intermittent struc- years ago. Indeed, solar wind being consist of “spaghetti- tures are shocks and current sheets where magnetic field ro- like” flux tubes has been suggested by Bartley et al. (1966) tates by an angle of about 120–130 degrees. This differs and McCracken and Ness (1966) as an attempt to explain from ordinary fluids where the most intermittent structures the modulation of cosmic rays and later adopted by Mariani are two-dimensional vortices. Veltri and Mangeney (1999) et al. (1973) to explain the observed variations in the occur- also pointed out that by using a conditional sampling scheme, rence rate of discontinuities in interplanetary magnetic field. one can eliminate the intermittency effects in the power spec- The suggestion of Bruno et al. (2001) and later Borovsky tra of the turbulence. Such studies therefore can provide a (2008) is interesting because in this picture, flux tubes will possible distinguishment between Kolmogorov type cascad- introduce an extra source of intermittency besides that gener- ing and Kraichnan type cascading in the solar wind. ated by non-linear interactions such as shown by Zhou et al. Later Bruno et al. (2001) studied current sheets using He- (2004). Since this intermittency is not intrinsic to the so- lios 2 data at 0.9 AU. They performed a minimum variance lar wind MHD turbulence, one has to pay extra attention to analysis to study how the solar wind magnetic field vector these structures in understanding the properties of the solar evolves for several selected time periods. By plotting the tra- wind MHD turbulence. jectory of the tip of the magnetic field vector in the minimum Extending the work of Borovsky (2008), Li (2008) devel- variance reference system, Bruno et al. (2001) showed that oped a systematic method to identify current sheets in the the magnetic field direction at times undergo abrupt changes, solar wind.
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