SPATIAL AND TEMPORAL MONITORING OF THE INTERMITTENT DYNAMICS IN THE TERRESTRIAL FORESHOCK Péter Kovács, Gergely Vadász, András Koppán 1.Geological and.

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SPATIAL AND TEMPORAL MONITORING OF THE INTERMITTENT DYNAMICS IN THE TERRESTRIAL FORESHOCK Péter Kovács, Gergely Vadász, András Koppán 1.Geological and Geophysical Institute of Hungary, Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Outline 1.Basic dynamics of the terrestrial foreshock (wave and turbulent properties) 2.Study of intermittent turbulence in the foreshock using PDF analysis 3.Applying high-pass filtering to enhance the properties of small amplitude fluctuations 4.Study of intermittency in terms of the foreshock geometry and solar wind parameters 5.Summary Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA SPATIAL AND TEMPORAL MONITORING OF THE INTERMITTENT DYNAMICS IN THE TERRESTRIAL FORESHOCK

Basic dynamics of the terrestrial foreshock Treumann, Jaroschek, 2008 Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Magnetic field spectra in the foreshock Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Basic properties of the waves in the Q || foreshock Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA Waves are developed by the BS reflected particles The waves frequencies are mostly in the Ultra low frequency (ULF) range (i.e. below 0.1 Hz) Waves have usually large amplitudes In the plasma rest frame they propagate upstream, but due to the convection they are swept back to the bow shock

Upstream wave related geomagnetic pulsations Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Upstream wave related geomagnetic pulsations Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA Heilig et al., Ann. Geophys., 2010

Aims, data, methodology Aim: -To show the turbulent properties of the foreshock in a wavy and non-stationary environment. -To study the influence of the solar wind driver to the turbulent behaviour of the foreshock. Data: FGM 5 Hz (5VPS) data from Cluster 1,2,3,4 Time period: January-April, Method: PDF analysis of difference time-series __________________________________ Main sources of the non-stationarity: 1.The movement of the spacecraft 2.The change of the downstream solar wind parameters (IMF, plasma pressure, bulk velocity, …) affecting the plasma environment and the configuration of the bow shock. Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA IMF  Bn d Bow shock model: Farris et al., 1995 Model parameters (SW bulk velocity, proton density, MA number) have been obtained from Cluster CIS_HIA instrument records or optionally from OMNI2 database Data selection

   Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA PDF analysis of temporal increments

Study of intermittency in spatial scale Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA Cluster configuration

Sliding window PDF analysis Window length: 20 min. (6000 points) Overlap: 5 min Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Mean flatness in terms of temporal and spatial scales 10 years of average, Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Referencing of the temporal intermittency to space Window length: 20 min. (6000 point) Step length: 5 min Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA IMF  Bn d Bow shock model: Farris et al., 1995 Model parameters (SW bulk velocity, proton density, MA number) have been obtained from Cluster CIS_HIA instrument (Dandouras et al., 2001) records or optionally from OMNI2 database Condition for quasi-parallel magnetic observation:  Bn < 50° Reference frame of the observattions

Strongest intermittency:  Bn ~ 35° Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA „Map” of intermittency in the foreshock

Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA Intermittency in temporal scaleIntermittency in spatial scale

Investigation of turbulent noise in wavy environment – Synthetic analysis Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA

Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA „Map” of intermittency in the foreshock Strongest intermittency:  Bn ~ 15-25°

Mean flatness vs. Solar wind parameters Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA 10 years of average,

Summary Cluster FGM data have been analysed from periods in the years of , when the mission located in the foreshock In 10 years of average, intermittent fluctuations were apparent in the foreshock, both in temporal and spatial scales It is argued that PDF analysis can give misleading results regarding to turbulence, if wave activitiy is strong in the analysed signal High-pass filtered FGM data exhibit decaying intermittency with the distance from the BS along the IMF and with angle of incidence of IMF to the BS In 10 years of average, intermittency increases with solar wind bulk speed and Alfvén Mach number. This behaviour is similar to that related to the ULF wave activities observed in ground observatories. Solar system plasma turbulence, intermittency and multifractals International Workshop and School, September 2015, Mamaia, ROMANIA