Detection of Small-Scale Structures in the Dissipation Regime of Solar-Wind Turbulence

2012 ◽  
Vol 109 (19) ◽  
Author(s):  
S. Perri ◽  
M. L. Goldstein ◽  
J. C. Dorelli ◽  
F. Sahraoui
Keyword(s):  
Solar Wind ◽  
Small Scale ◽  
Solar Wind Turbulence ◽  
Wind Turbulence ◽  
Scale Structures ◽  
Small Scale Structures

scholarly journals Solar cycle changes in the geo-effectiveness of small-scale solar wind turbulence measured by Wind and ACE at 1 AU

2007 ◽  
Vol 25 (5) ◽  
pp. 1183-1197 ◽  
Author(s):  
M. L. Parkinson ◽  
R. C. Healey ◽  
P. L. Dyson
Keyword(s):  
Solar Wind ◽  
Solar Cycle ◽  
Solar Minimum ◽  
Large Scale ◽  
Small Scale ◽  
Scaling Exponent ◽  
Mhd Turbulence ◽  
Scaling Exponents ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Abstract. Multi-scale structure of the solar wind in the ecliptic at 1 AU undergoes significant evolution with the phase of the solar cycle. Wind spacecraft measurements during 1995 to 1998 and ACE spacecraft measurements during 1997 to 2005 were used to characterise the evolution of small-scale (~1 min to 2 h) fluctuations in the solar wind speed vsw, magnetic energy density B2, and solar wind ε parameter, in the context of large-scale (~1 day to years) variations. The large-scale variation in ε most resembled large-scale variations in B2. The probability density of large fluctuations in ε and B2 both had strong minima during 1995, a familiar signature of solar minimum. Generalized Structure Function (GSF) analysis was used to estimate inertial range scaling exponents aGSF and their evolution throughout 1995 to 2005. For the entire data set, the weighted average scaling exponent for small-scale fluctuations in vsw was aGSF=0.284±0.001, a value characteristic of intermittent MHD turbulence (>1/4), whereas the scaling exponents for corresponding fluctuations in B2 and ε were aGSF=0.395±0.001 and 0.334±0.001, respectively. These values are between the range expected for Gaussian fluctuations (1/2) and Kolmogorov turbulence (1/3). However, the scaling exponent for ε changed from a Gaussian-Kolmogorov value of 0.373±0.005 during 1997 (end of solar minimum) to an MHD turbulence value of 0.247±0.004 during 2003 (recurrent fast streams). Changes in the characteristics of solar wind turbulence may be reproducible from one solar cycle to the next.

SMALL-SCALE SOLAR WIND TURBULENCE DUE TO NONLINEAR ALFVÉN WAVES

2015 ◽  
Vol 812 (1) ◽  
pp. 69 ◽  
Author(s):  
Sanjay Kumar ◽  
R. P. Sharma ◽  
Y.-J. Moon
Keyword(s):  
Solar Wind ◽  
Alfven Waves ◽  
Alfvén Waves ◽  
Small Scale ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Localized magnetic field structures and their boundaries in the near-Sun solar wind from Parker Solar Probe measurements

2020 ◽  
Author(s):  
Vladimir Krasnoselskikh ◽  
Keyword(s):  
Solar Wind ◽  
Radial Component ◽  
Plasma Pressure ◽  
Small Scale ◽  
The Sun ◽  
Ion Plasma ◽  
Scale Structures ◽  
Localized Magnetic Field ◽  
Probe Measurements ◽  
Small Scale Structures

<p>One of the most striking discoveries made by Parker Solar Probe during its first three encounters with the Sun is the presence of a multitude of relatively small-scale structures that stand out as sudden deflections of the magnetic. They were named “switchbacks” since some of them show up the full reversal of the radial component of the magnetic field and return to “regular” solar wind conditions. We carried out an analysis of three typical switchback structures having slightly different characteristics: I. Alfv´enic structures, where the variations of the magnetic field components take place conserving the magnitude of the magnetic field constant; II. Compressional, where the magnetic field magnitude varies together with changes of the components of the magnetic field; III. Structures manifesting full reversal of the magnetic field, they may be presumably similar to Alfv´enic, but they are some extremal class of “switchback structures”. We analyzed the properties of the magnetic field of these structures and the characteristics of their boundaries. Our observations and analysis lead to the conclusion that the structures represent localized magnetic field tubes moving with respect to surrounding plasma. The very important characteristic of these tubes consists of the existence of a relatively narrow boundary layer on the surface of the tube that accommodates flowing currents. These currents supposedly closed on the surface of the structure, and typically they have comparable azimuthal and the tube axes aligned components. These currents are supported by the presence of the effective electric field ensured by quite strong gradients of the density, and ion plasma pressure. The ion beta is typically larger than one inside the structure, and less than one outside. Another important feature is an electromagnetic wave accommodated on the surface of the structure. Its role consists in assistance to particles in carrying currents, to electrons parallel to magnetic field, and perpendicular to field to ions.</p>

scholarly journals Small‐Scale Energy Cascade of the Solar Wind Turbulence

2008 ◽  
Vol 674 (2) ◽  
pp. 1153-1157 ◽  
Author(s):  
O. Alexandrova ◽  
V. Carbone ◽  
P. Veltri ◽  
L. Sorriso‐Valvo
Keyword(s):  
Solar Wind ◽  
Energy Cascade ◽  
Small Scale ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

Fractal dissipation of small-scale magnetic fluctuations in solar wind turbulence as seen by CLUSTER

2010 ◽  
Author(s):  
K. Kiyani ◽  
S. Chapman ◽  
Y. Khotyaintsev ◽  
M. Dunlop ◽  
F. Sahraoui ◽  
...  
Keyword(s):  
Solar Wind ◽  
Small Scale ◽  
Magnetic Fluctuations ◽  
Solar Wind Turbulence ◽  
Wind Turbulence

scholarly journals Heliospheric current sheet inclinations at Venus and Earth

1999 ◽  
Vol 17 (5) ◽  
pp. 642-649 ◽  
Author(s):  
G. Ma ◽  
K. Marubashi ◽  
T. Maruyama
Keyword(s):  
Solar Wind ◽  
Magnetic Fields ◽  
Current Sheet ◽  
Solar Maximum ◽  
Heliospheric Current Sheet ◽  
Small Scale ◽  
Sector Boundary ◽  
Scale Structures ◽  
Transient Structures ◽  
Small Scale Structures

Abstract. We investigate the inclinations of heliospheric current sheet at two sites in interplanetary space, which are generated from the same solar source. From the data of solar wind magnetic fields observed at Venus (0.72 AU) and Earth (1 AU) during December 1978-May 1982 including the solar maximum of 1981, 54 pairs of candidate sector boundary crossings are picked out, of which 16 pairs are identified as sector boundaries. Of the remainder, 12 pairs are transient structures both at Venus and Earth, and 14 pairs are sector boundaries at one site and have transient structures at the other site. It implies that transient structures were often ejected from the coronal streamer belt around the solar maximum. For the 16 pairs of selected sector boundaries, we determine their normals by using minimum variance analysis. It is found that most of the normal azimuthal angles are distributed between the radial direction and the direction perpendicular to the spiral direction both at Venus and Earth. The normal elevations tend to be smaller than ~ 45° with respect to the solar equatorial plane, indicating high inclinations of the heliospheric current sheet, in particular at Earth. The larger scatter in the azimuth and elevation of normals at Venus than at Earth suggests stronger effects of the small-scale structures on the current sheet at 0.72 AU than at 1 AU. When the longitude difference between Venus and Earth is small (<40° longitudinally), similar or the same inclinations are generally observed, especially for the sector boundaries without small-scale structures. This implies that the heliospheric current sheet inclination tends to be maintained during propagation of the solar wind from 0.72 AU to 1 AU. Detailed case studies reveal that the dynamic nature of helmet streamers causes variations of the sector boundary structure.Key words. Interplanetary physics (interplanetary magnetic fields; sources of solar wind)

Exploring Coronal Structures with SOHO

2000 ◽  
Vol 179 ◽  
pp. 403-406
Author(s):  
M. Karovska ◽  
B. Wood ◽  
J. Chen ◽  
J. Cook ◽  
R. Howard
Keyword(s):  
Solar Corona ◽  
Image Enhancement ◽  
Coronal Mass Ejections ◽  
Dynamical Evolution ◽  
Small Scale ◽  
Low Contrast ◽  
Contrast Structures ◽  
Scale Structures ◽  
Small Scale Structures ◽  
Coronal Structures

AbstractWe applied advanced image enhancement techniques to explore in detail the characteristics of the small-scale structures and/or the low contrast structures in several Coronal Mass Ejections (CMEs) observed by SOHO. We highlight here the results from our studies of the morphology and dynamical evolution of CME structures in the solar corona using two instruments on board SOHO: LASCO and EIT.

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