particle transport in the heliosphere: part 1 gaetano zimbardo universita’ della calabria,...
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Particle Transport in the Heliosphere:
Part 1
Gaetano Zimbardo
Universita’ della Calabria, Cosenza, Italy
with contributions from S. Perri, P. Pommois, P. Veltri
Internationl School of Space Science,
L'Aquila, 21-25 September 2015
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Energetic particles with energies well above the thermal energy are observed
everywhere in space:
In the solar corona
In the Earth's magnetosphere
At heliospheric shocks
At the solar wind termination shock
From supernova remnants (galactic cosmic rays)
Extragalactic cosmic rays
For instance ...
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Tsuneta, 1998
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Hard X rays from RHESSI spacecraft:
Hard X rays imply energies of several MeV for electrons and ions.
Acceleration times are about 0.1 seconds – big challenge for models!
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CME shocks are the main source of solar energetic particles
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CME shocks have been studied in detail by Bemporad and Mancuso, ApJ (2010, 2011) and Bemporad et al., ApJ (2014). All the shock parameters have been determined using SoHO white light and UVCS instruments.
SoHO data
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Propagation of solar energetic particles (SEPs):
Reames, Space Sci. Rev. (1999)
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MeV particles are observed in the Earth's radiation belts:
Horne, Nature Phys., 2007
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Local electron acceleration in the radiation belts as seen by the Van Allen Probe B
Mozer et al., PRL, 2014
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Two step acceleration process!
Multi step processes also possible!
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Fast and slow streams in the solar wind lead to corotating interaction regions (CIRs) shocks
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Protons and electrons are accelerated at heliospheric shocks
Kunov et al., 1999
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Observations at the solar wind Termination Shock
Ion data from LECP onboard Voyager 2, at the termination shock crossing of 2007 (from Decker et al., Nature, 2008)
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Cas A supernova remnant (SNR)
Blue filaments are due to X ray synchrotron emission by 10 TeV electrons
Galactic cosmic rays are thought to be accelerated at SNRs
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Intensity of energetic particles
observed in the solar system:
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Possible acceleration mechanisms:
Fermi acceleration: first order (shock), second order (stochastic); Wave particle interaction: ion cyclotron
heating, electron-whistler acceleration; Reconnection electric fields, reconnection
jets; Turbulence Betatron effects Shock surfing Drift shock acceleration Pump acceleration (Fisk and Gloecker) ...
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Solar Energetic Particles (SEPs)
Clear association with solar cycle
From Lee et al., SSRv, 2012
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“Halloween” 2003 SEP event. Particles are accelerated both by flares and by shocks, but mostly close to the Sun. From Mewaldt et al., 2005.
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SEPs acceleration depends on the physical parameters
local to the shock
Adapted from M. Lee, ApJS (2005)
SPP
SEPs
SO
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Particle transport in the presence of magnetic fluctuations:
For magnetic field lines:
For particles following the magnetic field lines:
From Matthaeus et al., ApJL 2003
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Perpendicular transport due to magnetic turbulence:
• Particles perpendicular transport induced by magnetic fluctuations
• Parallel transport can be either scatter free or not
• Numerical simulation of particle transport in the presence of magnetic turbulence
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Numerical SimulationNumerical Simulation
The magnetic field is represented as a superposition of a constant field and a fluctuating field
0B r B B r
0 0 zB eB ( ) ( )
,
expB e i
k
k
B r k k k r
where
with
1 2 10
0
, e i e i e
k B k
k k kk B k
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Wave vectors on a cubic lattice 128x128x128
2x y zn n n
L
k
Anisotropic power law spectrum:
12 2 2 2 2 2 4 2x x y y z z
CB
k l k l k l
k
Numerical SimulationNumerical Simulation
2 2 2 2 2min maxx y zN n n n N
Band spectrum:
Here Nmin= 4, Nmax= 16. Future simulations with longer spectrum (see work by Francesco Pucci)
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Anisotropy in physical and phase space
Quasi-2DQuasi-slab
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Crooker et al., 1999
Balogh et al, 1995
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We performed analyses of Ulysses data who observed particles accelerated at CIR shock
• Ulysses observed a series of Corotating Interaction Regions in 1992-1993; both protons and electrons are accelerated at CIR shocks:
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Among the others, model by Zimbardo, Pommois, Veltri (2001)
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Cross latitude transport of CIR accelerated particles detected by Ulysses:
Pom
mois e
t al., JG
R, 2
00
1.
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Solar energetic particle drop outsfor impulsive events:
ACE data, Mazur et al., 2000Simulation in turbulence model, Giacalone et al., 2000
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Giacalone et al., 2000
Trenchi et al., 2013
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The structure of magnetic flux tubes is influenced by magnetic turbulence:
From Isichenko, PPCF, 1991
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Magnetic flux tube cross section for axisymmetric anisotropies and B/B = 0.5 at 1 AU (Zimbardo et al., JGR 2004)
Quasi-2D
Quasi-slab
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Injecting particles
with different Larmor
radii
Pommois et al., Ph.Pl. 2007;
Zimbardo et al., IEEE
Trans. Plasma
Sci., 2008)
Quasi-slab
Quasi-2D
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Space observations of energetic particles dropouts reveal the complex structure of magnetic flux tubes in solar wind
Mazur et al., Astrophys. J. 2000
Pommois et al., Adv. Spa. Res. 2005
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Similar study by Ruffolo, Matthaeus and
Chuychai (2003)
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Conclusions – Part 1
We have illustrated the different energetic particle populations which are found in space
• Solar energetic particles are most dangerous for space weather
• Numerical simulation of perpendicular transport can help to understand energetic particle transport to large heliographic latitudes as well as SEP dropouts
• The forthcoming Solar Probe Plus and Solar Orbiter spacecraft will boost our understanding of both SEP acceleration and transport