from the heliosphere into the sun · of the energy released during a flare. (lin & hudson 1971,...
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511th WE-Heraeus-Seminar
From the Heliosphere into the Sun– Sailing against the Wind –
Collection of presentationsEdited by Hardi Peter ([email protected])
Physikzentrum Bad Honnef, GermanyJanuary 31 – February 3, 2012
http://www.mps.mpg.de/meetings/heliocorona/
Bad Honnef, Febr. 2, 2012 1 1
Particle Acceleration and Plasma Kinetics in the Corona and Wind
Gottfried Mann Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany
e-mail: [email protected]
The Sun is a giant particle accelerator.
MHD is not appropriate to describe these phenomena.
Plasma kinetics is needed !!!
Flare: - enhanced emission of electromagnetic waves (radio - �-ray range) - acceleration of particles (e, p, and heavy ions)
Bad Honnef, Febr. 2, 2012 2
XX--RRaayy EEmmiissssiioonn DDuurriinngg SSoollaarr FFllaarreess
Basic problem: How are electrons accelerated up to high energies (> 20 keV) within a fraction of a second during solar flares? (� RHESSI) Energetic electrons carry a substantial part of the energy released during a flare. (Lin & Hudson 1971, 1976; Emslie et al. 2004)
RHESSI mission
Bad Honnef, Febr. 2, 2012 3
IInnvveerrssiioonn ooff PPhhoottoonn SSppeeccttrraa iinnttoo EElleeccttrroonn SSppeeccttrraa
(forward fitting method, Holman et al. 2003)
Bad Honnef, Febr. 2, 2012 4
RRHHEESSSSII RReessuullttss IIII
FFlluuxxeess aanndd PPoowweerr ooff EEnneerrggeettiicc EElleeccttrroonnss
Fe Pe mean energy
moderate flares 4.7 �1034 s-1 2.8 �1020 W 37 keV
large flares (Fe > 1036 s-1) 1.5 �1036 s-1 9.1 �1021 W 38 keV
(Mann & Warmuth, 2010)
sample of 25 flares
Bad Honnef, Febr. 2, 2012 5
TThhee SSttaannddaarrdd FFllaarree MMooddeell
� filament becomes instabil
� it is rising up
� a current sheet is establisted
� magnetic reconnection takes place
� outflow shock (Forbes, 1986; Tsuneta & Naito, 1998; Aurass, Vrsnak & Mann, 2002; Aurass & Mann, 2004)
(Carmichael, 1964; Sturrock, 1996; Hiroyama, 1974; Kopp & Pneumann, 1976) (or CSHKP-model)
electron acceleration at the termination shock
(Mann et al., 2007, 2009)
Bad Honnef, Febr. 2, 2012 6
RReellaattiivviissttiicc SShhoocckk DDrriifftt AAcccceelleerraattiioonn II
reflection in the de Hoffmann-Teller frame Lorentz-transformations:
laboratory frame �� shock rest frame �� HT frame �� back
�� motional electric field has been removed
� conservation of kinetic energy:
� conservation of magnetic moment:
const2HT,
2HT,II =�+� �
constB
constB
p
HT
2HT,
HT
2HT, =
��= ��
fast magnetosonic shock � magnetic field compression
� moving magnetic mirror
� reflection and acceleration
non-relativistic approach (Ball & Melrose, 2003; Mann & Klassen, 2005)
relativistic approach (Mann et al., 2006)
Bad Honnef, Febr. 2, 2012 7
� transformation of the particle velocities
( )downuplc
II,is2s
Ic,i
sII,i
B/Bsinarc:angleconeloss
)(1
tan
=��
�����
�>�
���
�
RReellaattiivviissttiicc SShhoocckk DDrriifftt AAcccceelleerraattiioonn IIII
};{}{ ,rII,r,i;II,i �� �����
c/secv
ß21
)1(
21
)1(2
ss
,i2ssII,i
2s
,r
2ssII,i
2sII,is
II,r
��=�
��+���
��=�
�+���
�+���=�
��
� reflection conditions:
� only particles with are accelerated for 0II,i >� lc*ss cos �=�>�
Bad Honnef, Febr. 2, 2012 8
SShhoocckk DDrriifftt AAcccceelleerraattiioonn aatt tthhee TTeerrmmiinnaattiioonn SShhoocckk
resulted differential fluxes
T = 10 MK MA = 2.3 vs = 1500 km/s 87°
88°
89° � reflection and acceleration of e at the TS
� substantial decrease of the pitch angle
� transmission into the downstream region
at the 2nd shock encounter
� moving towards the dense chromosphere
� hard X-ray emission
W � sdrift
12 keV 86° 6 m
50 keV 88° 25 m
20 MeV 89° 10 km
E = V � B = 2 kV/m
Bad Honnef, Febr. 2, 2012 9
coronal parameters from radio observations (at 150 MHz):
shock parameters:
comparison: theory � observations
CCoommppaarriissoonn ooff TThheeoorryy aanndd OObbsseerrvvaattiioonnss
MK40TG6.4B
cm108.2N
o
38e
=
=
�= �
220s
sA
updownupdown
cm109.2A
s/km2000v5.3M
2B/BN/N
�=
��=�
=�
)RHESSIbyobserveds107.1(s102F 136136e
�� ���=
The theory can approximately explain the observations.
)RHESSIbyobservedserg105.1(serg101P 129129e
�� �����=
Bad Honnef, Febr. 2, 2012 10
CCoonncclluussiioonnss
�� The termination shock is able to efficiently generate energetic electrons. �� quantitative confirmations of Tsuneta & Naito��s (1998) suggestion �� quantitative agreement with RHESSI observations concerning the flux and power of energetic electrons (> 20keV) �� Electrons accelerated at the termination shock could be the source of nonthermal hard X- and ��-ray radiation in chromospheric footpoints as well as in coronal loop top sources.
Bad Honnef, Febr. 2, 2012 11 11
Supra-Thermal Electrons in the Quiet Solar Corona
result of SOHO mission: differential heating (Te < Tp < THe)
(Wilhelm et al., 1998; Cranmer et al., 2002; Marsch & Tu, 2008) result of WIND and STEREO mission: F���core F���halo F���super-halo What creates supra-thermal tails?
Plasma kinetics is needed, again !!!
Bad Honnef, Febr. 2, 2012
CCoorroonnaall FFuunnnneellss
(Hassler et al., 1999)
solar interior: magnetic field is confined to supergranular boundaries
solar corona: rapid expansion of magnetic flux tubes
(Gabriel, 1976; Hackenberg, Mann & Marsch, 2000 )
differential heating
F����4/>D6�?*>.;�*:.�0.6.:*<.-�*<�<1.�+*;.�7/�<1.�/=66.4�F���8:7<76;�*6-�276;�*:.�1.*<.-�+A�276�,A,47<:76�:.;76*6,.�F���;74*:�?26-�*,,.4.:*<276�
see: Axford & McKenzie (1991), Marsch & Tu (1997), Vocks & Marsch (2001)
Bad Honnef, Febr. 2, 2012 13
EElleeccttrroonn AAcccceelleerraattiioonn bbyy WWaavveess
Ion cyclotron waves (LHP) are discussed for coronal heating and solar wind acceleration. (Marsch & Tu,1997; Vocks & Marsch, 2002) the model: resonant interaction between electrons and whistler (RHP) waves F���!�#�*6-�$�#�?*>.;�*:.�.52<<.-�/:75�<1.�+*;.�7/�<1.�/=66.4;�F���$�#�?*>.;��?12;<4.:;��:.;76*6<4A�26<.:*,<�?2<1�.4.,<:76; F���power law spectrum for the waves F���high-frequency tail of spectrum � electron frequencies � less wave energy for electrons than for ions
But bulk heating of electrons is not needed
Bad Honnef, Febr. 2, 2012 14
WWhhiissttlleerr--EElleeccttrroonn IInntteerraaccttiioonn II
resonance condition: dispersion relation: waves away from the Sun:
frequency sweeping:
B and �e decrease with height
� Electrons with high v|| < 0
interact preferably with the waves
The thermal electrons does not absorb the waves!
Bad Honnef, Febr. 2, 2012 15
WWhhiissttlleerr--EElleeccttrroonn IInntteerraaccttiioonn IIII
quasilinear theory: diffusion of electrons along lines of constant speed in the wave reference frame (Isenberg et al., 1999).
effect on electron distribution: F���26,:.*;.�7/�>�due to resonance F���.6.:0A�0*26� F���26,:.*;.�7/�>II due to mirror force
(vA,e = 0.5 c) (vA,e = 0.05 c)
Bad Honnef, Febr. 2, 2012
SSoollaarr WWiinndd EElleeccttrroonn FFlluuxxeess aatt 11 AAUU
effects of waves: F���flux enhancement over wide energy range F���electron spectrum less steep (Vocks & Mann, 2003, 2008)
solid line: with waves dashed line: without waves dotted line: initial condition
Bad Honnef, Febr. 2, 2012 17
SSuummmmaarryy
summary:
� a quiet stellar corona produces supra-thermal e- � same wave spectrum as for heating the corona common mechanism: � coronal heating
� solar wind acceleration � production of supra-thermal electrons
This mechanism is probably also acting in other stellar coronae.
Bad Honnef, Febr. 2, 2012 18
TThhaannkk yyoouu ffoorr yyoouurr aatttteennttiioonn!!
Plasma kinetics are necessary to describe astrophysical phenomena (e.g. particle acceleration, non Maxwellian distributions), appropriately.
Bad Honnef, Febr. 2, 2012
BBoollttzzmmaannnn -- VVllaassoovv EEqquuaattiioonn
gyrotropy: F���electron gyroperiods much shorter than other time scales F���1 spatial coordinate, s, along B F���2 velocity coordinates, vII and v�
Boltzmann - Vlasov equation for electrons:
right hand side: F���wave-particle interaction: quasilinear theory
F���Coulomb collisions, with protons and electrons:
Landau collision integral, collision partners with Maxwellian distribution
Coul.w.p.II
IIIIIIIIII t
f+tf=
vfv
vfv
sBln
B2v
vfE
meg+
sfv+
tf
�
��
���
�
��
���
�
��
�
��
���
��
���
�
��
� ���
��
��
�
Bad Honnef, Febr. 2, 2012 20
EElleeccttrroonn DDiissttrriibbuuttiioonnss
height above coronal base: 1.06 R�
.4.,<:76��4/>D6�;8..-��������������,�height above coronal base: 6.5 R�
.4.,<:76��4/>D6�;8..-���������������,�