paper figures纸上的数字

Rest frame spectrum
103
consists of Fa(Wlo)c=af(wl )–5
powe10r0la0w
F(W) =f(w)
tthaial ptoswtearrltasw
at
w
≈ 1.7 and htaaisl an
101
Suprathermal ? Power Law Tails
Suprathermal ? Power Law Tails
SW ICS
ULEIS
10-5
10-7
Roll over 1
10-9
m1=1.3e3;m2=5;m3=18;m4=1.5;m5=0;m6=1; m7=0e3;
1
10
Proton speed (in solar wind frame) /solar wind speed
Magnetic field and plasma signatures of a CIR --
will be covered in CIR session by Lan Jian’s talk
Energetic Particle properties and
acceleration theories
0.433
108.425
0.80000
Phase Space Density (s3/km6)
Halo Solar Wind
107 105
2003
Start DOY 319.121
Stop DOY 320.496
<Vsw>
Байду номын сангаас
707.545
107 chi2 105 parabola
103
101 10-1 10-3
Mason et al., ApJ., 678, 1458, 2008
F(W) Phase Space Density (s 3/km6)
109 107 105 103 101 10-1 10-3 10-5 10-7 10-9 1
Ulysses 4.5 AU
199 1.2 92. 0400- 293. 040 0 4.485 AU
Gloeckler et al., JGR, 99, 17637, 1994.
He+ at 1 AU: • observed routinely in CIRs • lower average abundance than at several AU: He+/He++ = 0.25 • other heavy ions show mostly higher charge states
e-fold0i.n1g speed wo ≈ 18
f(w )=1.3•103w –5exp[-(w /18)2.1]
0.001
1.300 3.700
1fi.t0100 m1=3.9e4;m2=5;m31=.1920;0m4=.6;
10c-51=m1*(c0^-m2c)2*e=x2p.7(-e(3c*0c/70m..^69-3009)00;^c3m=4c)1*+e
tthraants0bp.e0o0nr1dt sefdfeocwtsn due to
fit1 m1=3.9e4;m2=5;m3=12;m4=.6;
10c-51=m1*(c0^-m2c)2*e=x2p.7(-e(3c*0c/0m^-39);^c3m=4c)1*+e
10-7
10-9
fr(w )= 2m•71=0206ee5;xm8pm=1[1-=.11(;52m;m98=2/1=w;5m;m1)031==.211850;0]mw;m114==–115.;1me55;xm=0p1;2m[=-65(=e1w2;;m/113=.114).15;.0]
Mason et al., ApJ., 678, 1458, 2008
Average composition of 41 CIRs is close to solar wind except for He and Ne.
Agreement with fast solar wind composition is slightly better
top panel: plastic sw proton speed
middle panel: SIT He, for 189, 384, and 787 keV/nucleon
arrow marks selection threshold figure shows events 15-21 in Table 1. Note increases starting on days 258, 261,284 and 291 are below the selection threshold and so are not in the table
Roll over 2 10-7
9.000 10f0i.t0200 c1=mm11=*6(ce03^;m-m2=24)0*..e37x;0mp0(3-=(c90;/mm
c2=1.65e3*c0^-9.7;c6=c
Downstream of
10-9
100
Compression
(w)
Mach numbe
R. Bucik M. I. Desai A. B. Galvin G. Gloeckler
A. Korth R. A. Leske
U. Mall R. A. Mewaldt
K. Simunac
Outline:
• Introduction • Energetic particle properties and acceleration theories • STEREO observations of short term variability
Mason et al., ApJ., 678, 1458, 2008
Evidence for a solar wind source for CIR Fe
the CIR Fe/O ratio is significantly correlated with the solar wind Fe/O ratio 2-4 days before passage of the CIR
1
10
Proton speed (in solar wind frame) /solar wind speed
100
(w)
10-7 10-9
fit 2 m1=6e3;m2=4.3;m3=9;m c1=m1*(c0^-m2)*exp(-(c0/m
c2=1.65e3*c0^-9.7;c6=c
Downstream of
Ratios of heavy ion abundances show that spectral forms are virtually identical for species with a wide
range of Q/M values
intensities change by a factor of ~10^8 over range shown
F(W) =f(w)
Rest 1fr0a0m0 e sFp(We)c=tfr(uwm)
consists of atalilopcoawler–l5aw
power law thtaailt starts at
w
≈
110and
tail2
hasusmsharp
exponential roll over with
He + H+
HI-SCALE
He ++
SWICS
He 10 W Ion Speed (SC frame)/V
sw
Ulysses observations of pick up He+:
•at 4.5 AU He+ more abundant than solar wind He++ (!)
• evidence that bulk solar wind is not source of the CIR energetic ions
Mason et al., ApJ., 678, 1458, 2008
Challenge for most models: at high energies, intense CIRs show power law spectral form, while most models predict exponential roll-overs
CIR overview -
see ISSI Space Science Series book - 1999
• solar origins
• formation in IP medium
• turbulence and acceleration
• etc
Solar wind and magnetic field signatures of CIRs
bottom panel: SIT O for 67, 136, and 266 keV/nucleon
note high speed streams with no suprathermals around day 305, 315, and 330
Mason et al., Solar Phys, 256, 393, 2009 “STEREO science results at solar min”
Spectral index shows large range of values at low energies, with steepening above ~1 MeV/nucleon