space weather effects of the solar wind on different regions of the magnetosphere viviane pierrard...
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Space weather effects of the solar wind on different
regions of the magnetosphere
Viviane PIERRARD
BELGISCH INSTITUUT VOOR RUIMTE-AERONOMIE INSTITUT D’AERONOMIE SPATIALE DE BELGIQUE BELGIAN INSTITUTE OF SPACE AERONOMY BELGISCH INSTITUUT VOOR RUIMTE-AERONOMIE INSTITUT D’AERONOMIE SPATIALE DE BELGIQUE BELGIAN INSTITUTE OF SPACE AERONOMY BELGISCH INSTITUUT VOOR RUIMTE-AERONOMIE INSTITUT D’AERO
Belgian Institute for Space Aeronomy (BIRA-IASB)
Institut d’Aéronomie Spatiale de Belgique (IASB)
Belgisch Instituut voor Ruimte-Aeronomie (BIRA)
IAP Charm
Kinetic models based on the solution of the evolution equationSolar wind
]1)[(2
1WPIfD
vfA
vv
fa
r
fv
t
f
Exosphere: Kn>>1 Vlasov equation
Exobase: Kn=1 Solar wind escape: 1.1-5 Rs
Barosphere: Kn<<1 Fokker-Planck
1. Vlasov (analytic) Pierrard et al., Sol. Phys., 20142. Fokker-Planck Pierrard et al., JGR, 20013. WPI kinetic Alfven waves Pierrard & Voitenko, Sol. Phys.20134. WPI Whistler turbulence Pierrard et al., Sol. Phys. 2011
Pierrard V., “Exploring the solar wind”, 221-240, Intech, ISBN 978-953-51-0339-4, 2012
Knudsen = mean free path/H
Friction Diffusion
Velocity distribution functions observed in situ in the solar wind
Electrons 1 AU WIND Protons 0.5 AU Helios Ions He O Ne 1 AU WIND
halo
corestrahl
B
Ulysses electron distributions fitted with Kappa functions
Results:
<> = 3.8 +/- 0.4 for v > 500 km/s (4878 observ.) <> = 4.5 +/- 0.6 for v < 500 km/s (11479 observ.)
Ions WIND:
=2.5
General in space plasmas
Kappa functions
Pierrard and Lazar, Sol. Phys., 287, 153-174, 10.1007/s11207-010-9640-2, 2010
)1(22/3
2/3 21
22
kT
mvA
kT
mnf ekappa k
Solar wind kinetic model: profiles of the moments
Maxwellian
Kappa=2
Pierrard, Space Sci. Rev., 172, 315, 2012
Not classical heat flux
Pierrard et al., Solar Phys., 2014
Solar wind minor ions
Pierrard, Space Sci. Rev., 172, 315, 2012
Kappa=5 for all species
T=10000 K at the top of chromosphere
Heating of the corona by velocity filtration
Acceleration of the ions
Solar wind model
SDO observations29 May 2013 coronal holes directed to the Earth.
Pierrard & Pieters, ASP,167-172, 2014
ACE observations of velocity at 1 AU
Model with collisions and whistler turbulence
Bottom (collision-dominated):
f(2 Rs,>0,v) = maxwellian
Top (collisionless conditions):
f(14 Rs,<0,v<ve) = f(14 Rs,>0,v<ve)
f(14 Rs,<0,v>ve) = 0
Pierrard, Lazar & Schlickeiser, Sol. Phys. 287, 421, 2011
Electron velocity distribution function
Kp [0-9] 1939 13 stations (11N, 2S 44-60°) Dst 1964 4 stations (eq) AE 1966 12 stations N (aur)PC 1991 1 station (pol)
Geomagnetic activity indices (based on B at the surface of the Earth)
Storms and substorms
Auroral regions
Pierrard et al., J. Atmosph. Sol. Terr. Phys., 69 doi: 10.1016/j.jastp.2007.08.005, 2007
Current-voltage relationship FUV IMAGE
Electron flux in the 0.5-0.6 MeV at 820 km measured by EPT on PROBA-V
Van Allen Radiation beltsEnergetic protons and electrons
Pierrard et al., Space Sci. Rev., doi: 10.1007/s11214-014-0097-8, 2014
AP8 Max J(E>10 MeV) AE8 Max J(E >1 MeV)
L (Re) L (Re)
internal: p+ (100 keV-500 MeV) external: p+ (<10 MeV) e- (10 keV-10 MeV) e- (10 keV-5 MeV) 4 Rt 10 Rt
Van Allen Radiation belts
Dynamic model of the radiation belts
Dynamic model of the electron radiation belts based on CLUSTER/RAPID observations (2001-2012)
www.spaceweather.eu
Pierrard & Borremans, subm. SWSC, 2014
Links Plasmasphere/radiation belts
Plasmasphere: 1 eV Radiation belts: > 200 keV
Pierrard and Benck, AIP, 1500, 216, 2012 (SAC-C)Darrouzet et al., JGR, 118, 4176-4188, 2013 (Cluster)
9-6-2001/ 10-6-2001
Terrestrial plasmasphere and plasmapauseposition
Pierrard and Voiculescu, GRL 38, L12104, 2011
on www.spaceweather.eu http://ccmc.gsfc.nasa.govIonosphere, GPS
Web-based forecasting and nowcasting model
Before substorm9 June 20018h00
After substorm10 June 20017h00
Comparison with observations
IMAGE (2000-2006):RPI and EUV He+ ions at 30.4 nm
Pierrard V., Planet. Space Sci., doi : 10.1016/j.pss.2009.04.011, 2009
Electron density in the exosphere of Jupiter
Auroral oval and footprints on Jupiter
Saturn and Jupiter
- CMEs and solar wind high speed streams cause geomagnetic storms and substorms
- Variations measured by geomagnetic activity indices (Kp, Dst) - Auroral oval larger and wider - High flux variations in the outer electron Van Allen belt - High variability of the plasmapause position - Comparison with the magnetosphere of other planets - Kinetic models developed for space plasmas - Models provided on www.spaceweather.eu
IASB-BIRA/STCE / IUAP CHARM
Conclusions
BELGISCH INSTITUUT VOOR RUIMTE-AERONOMIE INSTITUT D’AERONOMIE SPATIALE DE BELGIQUE BELGIAN INSTITUTE OF SPACE AERONOMY BELGISCH INSTITUUT VOOR RUIMTE-AERONOMIE INSTITUT D’AERONOMIE SPATIALE DE BELGIQUE BELGIAN INSTITUTE OF SPACE AERONOMY BELGISCH INSTITUUT VOOR RUIMTE-AERONOMIE INSTITUT D’AERO
Conclusions
• CMEs and solar wind high speed streams cause geomagnetic substorms and storms• Variations measured by geomagnetic activity indices at the ground (Kp, Dst)• Auroral oval larger and wider• High flux variations in the outer electron Van Allen belt• High variability of the plasmapause position• Comparison with the magnetosphere of other planets • Kinetic models developed for space plasmas• Models provided on www.spaceweather.eu
IASB-BIRA/STCE / IUAP CHARM
The moments of f
vdvrfrn
),()(
)(
)()(
rn
rFru
vdvvrfrF
),()(
Number density [m-3]
Particle flux [m-2 s-1]
Bulk velocity [m s-1]
Energy flux [Jm-2 s-1]
Pressure [Pa]
Temperature [K]
vduvuvvrfmrP
))()(,()(
vduvvrfrnk
mrT
2),(
)(3)(
vduvuvvrfm
rE
)(),(2
)(2
Kappa distributions: theory and applications in space plasmas
• Generation of Kappa in space plasmas: • turbulence and long-range properties of particle interactions in a plasma
- plasma immersed in suprathermal radiation (Hasegawa et al., 1985)- random walk with power law (Collier, 1993)- turbulent thermodynamic equilibrium (Treumann, 1999)- entropy generalization in nonextensive Tsallis statistics (Leubner, 2002)- resonant interactions with whistler waves (Vocks and Mann, 2003)
• Dispersion properties and stability of Kappa distributions
– Vlasov-Maxwell kinetics. Dielectric tensor– The modified plasma dispersion function– Isotropic /Anisotropic Kappa distributions
Pierrard and Lazar, Sol. Phys., 287, 153-174, 10.1007/s11207-010-9640-2, 2010
Consequence 3. Solar wind accelerated to high bulk velocity due to the presence of suprathermal electrons (Vlasov model)
=2Maxwell
Pierrard and Lemaire, JGR 101, 7923-7934, 1996Pierrard, Space Sci. Rev., 172, 315-324, 2012
Consequence: Non classical heat flux
Temperature inversion around 2 Rs- Peak in electron temperature at 2 Rs - Corresponds to coronal brightness measurements obtained during solar eclipses
Heat flux-not given by the Spitzer-Harm expression-Spitzer-Harm heat flux assumed in fluid models-No need of additional heating source to heat the corona or to accelerate the wind
Pierrard V., K. Borremans, K. Stegen and J. Lemaire, Solar Phys., doi: 10.1007/S11207-013-0320-x, 2014
Te model
Te obs. polar
Te obs. equator
Qe model
Qp model
Classical heat flux
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