Proton and Alpha from Pamela
Proton and Alpha from Pamela
Proton and Alpha from Pamela
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31st ICRC 2009<br />
July 7-15, 2009, in Łódź,<br />
<strong>Proton</strong> <strong>and</strong> <strong>Alpha</strong> <strong>from</strong> <strong>Pamela</strong><br />
M. Casolino<br />
INFN & University of Roma Tor Vergata<br />
Nico De Simone<br />
Nikolay Nikonov<br />
on behalf of the PAMELA collaboration<br />
M. Casolino, INFN & University Roma Tor Vergata
<strong>Pamela</strong> in the Hillas plot<br />
Neutron<br />
Stars<br />
10 12 eV protons<br />
White Dwarfs<br />
.<br />
10 20 eV protons<br />
10 9 eV protons<br />
M. Casolino, INFN & University Roma Tor Vergata
Selection of galactic component according to<br />
geomagnetic cutoff<br />
R cutoff =14.9GV/L 2<br />
M. Casolino, INFN & University Roma Tor Vergata
Particle rigidity vs Vertical Stormer Cutoff<br />
Galactic positive<br />
(above cutoff)<br />
e+ p<br />
Rig=cutoff<br />
subcutoff<br />
saa<br />
e- p-<br />
M. Casolino, INFN & University Roma Tor Vergata
Solar Modulation of Galactic Cosmic Rays<br />
Balloon: low frequency<br />
modulation<br />
<strong>Pamela</strong>: low <strong>and</strong> high<br />
frequency modulation<br />
Long solar minimum<br />
Variation in Galactic<br />
flux<br />
Short Term<br />
(months)<br />
Long term (years)<br />
<strong>Pamela</strong><br />
AMS-01<br />
Caprice / Mass /TS93<br />
BESS<br />
Charge dependence<br />
(e.g. Asaoka Y. et al. 2002, Phys.<br />
Rev. Lett. 88, 051101)<br />
Nm, сm -2 s -1<br />
3.5<br />
3.0<br />
2.5<br />
2.0<br />
R c = 0.03 и 0.6 GV<br />
R c = 2.4 CV<br />
J<br />
2 2<br />
E E 1.5<br />
0<br />
( r,<br />
E,<br />
t)<br />
<br />
J ( ,<br />
E (<br />
M. Casolino, 2 INFN & 2University 2 Roma Tor Vergata<br />
( E (<br />
t))<br />
E0<br />
t))<br />
1955 1965 1975 1985 1995 2005<br />
Year<br />
Dati meteor 0.03 GV 0.6 GV, Stozkov 2008
Solar modulation at minimum of solar cycle XXIII years 2006-2008<br />
F is<br />
= 1.54 is<br />
0.7<br />
R is<br />
-2.76<br />
p/(cm 2 s sr GV)<br />
J<br />
Spectral index<br />
2.75 <br />
2 2<br />
E E0<br />
( r,<br />
E,<br />
t)<br />
<br />
2 2 2<br />
( E (<br />
t))<br />
E0<br />
J(<br />
,<br />
E (<br />
t))<br />
Decreasing sol activity<br />
July 2006<br />
August 2007<br />
February 2008<br />
increasing particle<br />
flux<br />
M. Casolino, INFN & University Roma Tor Vergata<br />
Solar modulation parameters<br />
(GV) error<br />
JUL06 5.01-01 2e-03<br />
JAN07 4.16-01 2-03<br />
AUG07 4.02-01 3-03
Trapped proton flux in the Van Allen belt<br />
(South Atlantic Anomaly)<br />
Arxiv 0810.4980v1<br />
P/(cm^2 sr GeV s)<br />
Trapped<br />
Turquoise 0.3 G < B<br />
Yellow 0.22 G < B < 0.23 G<br />
Blue 0.21 G < B < 0.22 G<br />
Green 0.20 G < B < 0.21 G<br />
Red 0.19 G < B < 0.20 G<br />
Black B35 MeV)<br />
(PSB97 plot by SPENVIS<br />
project, model by BIRA-IASB)<br />
<br />
A E<br />
M. Casolino, INFN & University Roma Tor Vergata<br />
<br />
( 0 1E<br />
)<br />
nero<br />
rosso<br />
verde<br />
A<br />
0.11±0.01<br />
(2.3±0.3) 10 -2<br />
(5±3) 10 -4<br />
γ 0<br />
6.0±0.4<br />
5.9±0.5<br />
8.1±1.8<br />
γ 1<br />
3.1±0.5<br />
2.6±0.6<br />
4.7±1.8<br />
GeV<br />
χ 2 /ndf<br />
7.1<br />
6.8<br />
10.
Helium spectrum at 1 AU: after Imp-8<br />
Reference for Voyager 1,2<br />
M. Casolino, INFN & University Roma Tor Vergata
Helium/proton ratio at 1AU – Reference for Voyagers<br />
M. Casolino, INFN & University Roma Tor Vergata
Particle identification: basic principle<br />
Beta = v/c (<strong>from</strong> TOF)<br />
antiparticles<br />
albedo<br />
e +<br />
p<br />
4<br />
He+d<br />
particles<br />
albedo<br />
particles<br />
antiparticles<br />
M. Casolino, INFN & University Roma Tor Vergata<br />
Rigidity (<strong>from</strong> Tracker)
<strong>Proton</strong> Absolute flux<br />
•Montecarlo efficency for cuts<br />
•Trigger efficiency<br />
•Tracking efficiency<br />
•Multiple Scattering<br />
•Correction for energy loss in det<br />
•Back scattering…<br />
•Systematics under close<br />
investigation, currently<br />
about 1-2% uncertainty on abs<br />
flux.<br />
Selection criteria<br />
Fitted, single track<br />
High lever arm, Nx<br />
Rigidity R>0<br />
Beta>.2<br />
No anti<br />
M. Casolino, INFN & University Roma Tor Vergata<br />
Energy loss <strong>from</strong> tracker<br />
antiparticles<br />
albedo<br />
particles<br />
particles<br />
albedo<br />
antiparticles
EXT PARAMETER<br />
NO. NAME VALUE ERROR<br />
1 p0 2.18935e+003 8.79294e+000<br />
2 p1 5.08849e-001 1.40979e-004<br />
3 p2 3.86465e-002 1.17953e-004<br />
4 p3 1.76546e+002 2.05500e+000<br />
5 p4 6.66809e-001 1.07337e-003<br />
6 p5 5.64675e-002 7.33827e-004<br />
d<br />
4 He<br />
M. Casolino INFN e Univ Tor Vergata<br />
p<br />
3 He<br />
M. Casolino, INFN & University Roma Tor Vergata
<strong>Proton</strong> <strong>and</strong> Helium spectra, rigidity Jul 2006<br />
preliminary<br />
P: 2% fitting error<br />
M. Casolino, INFN & University Roma Tor Vergata
<strong>Proton</strong> <strong>and</strong> Helium spectra, kinetic energy, Jul 2006<br />
preliminary<br />
M. Casolino, INFN & University Roma Tor Vergata
M. Casolino, INFN & University Roma Tor Vergata<br />
preliminary
<strong>Proton</strong> flux fitting<br />
vs starting <strong>and</strong> ending energy<br />
Emax<br />
M. Casolino, INFN & University Roma Tor Vergata<br />
Emin
M. Casolino, INFN & University Roma Tor Vergata<br />
<strong>Proton</strong> fitting in various energy range
He fitting at various energy range<br />
M. Casolino, INFN & University Roma Tor Vergata
Comparison with other experiments<br />
preliminary<br />
M. Casolino, INFN & University Roma Tor Vergata
Comparison with other experiments<br />
preliminary<br />
M. Casolino, INFN & University Roma Tor Vergata
M. Casolino, INFN & University Roma Tor Vergata<br />
Total kin ene
M. Casolino, INFN & University Roma Tor Vergata<br />
Total kin ene
M. Casolino, INFN & University Roma Tor Vergata<br />
Total kin ene
Current work: extend the maximum energy<br />
range for p (1TeV) <strong>and</strong> He (500 GeV)<br />
Underst<strong>and</strong> systematic <strong>and</strong> statistical errors<br />
to reach required precision of less than 1%<br />
M. Casolino, INFN & University Roma Tor Vergata
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