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Helium in near earth orbit

Authors :
D. Vité
Peter H. Fisher
Yu. Galaktionov
J. Alcaraz
Roald Z. Sagdeev
D.X. Zhao
K. Karlamaa
A. Arefiev
S.W. Ye
E. Riihonen
W. Hungerford
M. A. Huang
R. R. McNeil
B. Meillon
V. Shoutko
G. Kenney
J. Ritakari
Y. H. Chang
J. Engelberg
C. Camps
G. Sartorelli
D. Barancourt
A. Mihul
Timo Laitinen
R. Ionica
Jorge Dias de Deus
W. Kim
H. von Gunten
P. G. Rancoita
V. Postolache
M. Pauluzzi
G. Lu
C. Maña
Werner Lustermann
Federico Cindolo
F. Mayet
G. Fluegge
Mao-Zhi Yang
D. Ren
A. Schultz von Dratzig
G. Barbier
W.Z. Zhu
W. J. Burger
A. Papi
J. Casaus
U. Roeser
M. Ribordy
G. Ambrosi
Y.L. Chuang
A. Contin
P. Levtchenko
M. Buenerd
X.W. Tang
M. Pimenta
W. Wallraff
T. S. Dai
F. Vezzu
B. Verlaat
Maria Ionica
G.S. Sun
Samuel C.C. Ting
Frank Raupach
E. Shoumilov
P. Berges
B.C. Wang
S. Urpo
Ari Mujunen
G. Bruni
H. Suter
P. Bene
Hengchang Liu
D. Rapin
C. Roissin
V. Plyaskin
G. Laurenti
S. Waldmeier Wicki
D. Grandi
A. Pevsner
Z. L. Ren
F. Velcea
Tao Song
G. Lamanna
M. J. Boschini
B. Bertucci
J. J. Torsti
Antonino Zichichi
Waclaw Karpinski
J. Berdugo
H. Anderhub
V. Commichau
R. Becker
Roberto Battiston
B. Alpat
N. Fouque
J.P. Richeux
Zhenghao Xu
M. Bourquin
A. Lebedev
Dong-Chul Son
E. Fiandrini
F. Palmonari
Yun Wang
G. Boella
P. Yeh
J.L. Yan
H.F. Chen
L. Brocco
Felicitas Pauss
L. Baldini
A. Pesci
H. S. Chen
J. Ulbricht
K. Wiik
R. Kossakowski
N.A. Chernoplekov
Nicolas Produit
K. Lübelsmeyer
S. X. Wu
M. Basile
P. Cannarsa
Hao Zhang
S. Blasko
M. Jongmanns
G. Castellini
E. P. Velikhov
B. Zimmermann
G.P. Barreira
K. Hangarter
H. L. Zhuang
Anselmo Margotti
Tzihong Chiueh
J. P. Da Cunha
Y.S. Lu
Inkyu Park
J.P. Vialle
Ciaran Williams
A. Klimentov
G. Laborie
L. Ao
M. Pohl
N. Dinu
Merja Tornikoski
Markus Cristinziani
M. Steuer
P.C. Xia
G. Viertel
D. Luckey
Jose Maria Kenny
J. Trümper
L. Djambazov
Paolo Zuccon
O. Grimm
T. Eronen
E. Babucci
U. Becker
I. Vetlitsky
S.C. Lee
Eun-Suk Seo
E. Perrin
M. Kraeber
F. J. Eppling
S. M. Ting
Changgen Yang
V. Koutsenko
Eino Valtonen
P. Giusti
Adrian Biland
G. Scolieri
G. Esposito
Z.R. Dong
Claudia Cecchi
Philipp Azzarello
I. Lopes
Massimo Gervasi
P. Emonet
S. Bizzaglia
Z.G. Chen
J. Favier
M. Capell
R. Siedling
X. D. Cai
C.L. Liu
L. Bellagamba
L.G. Yan
Ilya Usoskin
Jing Wang
J. Vandenhirtz
A. Hasan
Mauro Menichelli
G. Schwering
P. Extermann
W.Q. Gu
H. Hofer
F. Barao
V. Hermel
Zhidong Zhang
D. Casadei
I. D'Antone
Guohuai Zhu
J. D. Burger
A. Mourao
V. Pojidaev
Giuseppe Levi
Laboratoire de Physique Subatomique et de Cosmologie (LPSC)
Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)
Laboratoire d'Annecy de Physique des Particules (LAPP)
Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)
AMS
Alcaraz, J
Alpat, B
Ambrosi, G
Anderhub, H
Ao, L
Arefiev, A
Azzarello, P
Babucci, E
Baldini, L
Basile, M
Barancourt, D
Barao, F
Barbier, G
Barreira, G
Battiston, R
Becker, R
Becker, U
Bellagamba, L
Béné, P
Berdugo, J
Berges, P
Bertucci, B
Biland, A
Bizzaglia, S
Blasko, S
Boella, G
Boschini, M
Bourquin, M
Brocco, L
Bruni, G
Buenerd, M
Burger, J
Burger, W
Cai, X
Camps, C
Cannarsa, P
Capell, M
Casadei, D
Casaus, J
Castellini, G
Cecchi, C
Chang, Y
Chen, H
Chen, Z
Chernoplekov, N
Chiueh, T
Chuang, Y
Cindolo, F
Commichau, V
Contin, A
Cristinziani, M
Cunha, J
Dai, T
Deus, J
Dinu, N
Djambazov, L
D'Antone, I
Dong, Z
Emonet, P
Engelberg, J
Eppling, F
Eronen, T
Esposito, G
Extermann, P
Favier, J
Fiandrini, E
Fisher, P
Fluegge, G
Fouque, N
Galaktionov, Y
Gervasi, M
Giusti, P
Grandi, D
Grimm, O
Gu, W
Hangarter, K
Hasan, A
Hermel, V
Hofer, H
Huang, M
Hungerford, W
Ionica, M
Ionica, R
Jongmanns, M
Karlamaa, K
Karpinski, W
Kenney, G
Kenny, J
Kim, W
Klimentov, A
Kossakowski, R
Koutsenko, V
Kraeber, M
Laborie, G
Laitinen, T
Lamanna, G
Laurenti, G
Lebedev, A
Lee, S
Levi, G
Levtchenko, P
Liu, C
Liu, H
Lopes, I
Lu, G
Lu, Y
Lübelsmeyer, K
Luckey, D
Lustermann, W
Maña, C
Margotti, A
Mayet, F
Mcneil, R
Meillon, B
Menichelli, M
Mihul, A
Mourao, A
Mujunen, A
Palmonari, F
Papi, A
Park, I
Pauluzzi, M
Pauss, F
Perrin, E
Pesci, A
Pevsner, A
Pimenta, M
Plyaskin, V
Pojidaev, V
Pohl, M
Postolache, V
Produit, N
Rancoita, P
Rapin, D
Raupach, F
Ren, D
Ren, Z
Ribordy, M
Richeux, J
Riihonen, E
Ritakari, J
Roeser, U
Roissin, C
Sagdeev, R
Sartorelli, G
Schultz&nbsp
von&nbsp
Dratzig, A
Schwering, G
Scolieri, G
Seo, E
Shoutko, V
Shoumilov, E
Siedling, R
Son, D
Song, T
Steuer, M
Sun, G
Suter, H
Tang, X
Ting, S
Tornikoski, M
Torsti, J
Trümper, J
Ulbricht, J
Urpo, S
Usoskin, I
Valtonen, E
Vandenhirtz, J
Velcea, F
Velikhov, E
Verlaat, B
Vetlitsky, I
Vezzu, F
Vialle, J
Viertel, G
Vité, D
Gunten, H
Wicki, S
Wallraff, W
Wang, B
Wang, J
Wang, Y
Wiik, K
Williams, C
Wu, S
Xia, P
Yan, J
Yan, L
Yang, C
Yang, M
Ye, S
Yeh, P
Xu, Z
Zhang, H
Zhang, Z
Zhao, D
Zhu, G
Zhu, W
Zhuang, H
Zichichi, A
Zimmermann, B
Zuccon, P
Ambrosi, Giovanni
Azzarello, Philipp
Bene, Pierre
Bourquin, Maurice
Cristinziani, Markus
Emonet, Pascal Philippe
Extermann, Pierre
Perrin, Eric
Pohl, Martin
Produit, Nicolas
Rapin, Divic Jean
Ribordy, Mathieu
Richeux, Jean-Pierre
Vite, Davide
Source :
Physics Letters B, Physics Letters B, Elsevier, 2000, 494, pp.193-202, HAL, Physics Letters. B, Vol. 494, No 3-4 (2000) pp. 193-202
Publication Year :
2000

Abstract

The helium spectrum from 0.1 to 100 GeV/nucleon was measured by the Alpha Magnetic Spectrometer (AMS) during space shuttle flight STS-91 at altitudes near 380 km. Above the geomagnetic cutoff the spectrum is parameterized by a power law. Below the geomagnetic cutoff a second helium spectrum was observed. In the second helium spectra over the energy range 0.1 to 1.2 GeV/nucleon the flux was measured to be (6.3±0.9)×10 −3 ( m 2 sec sr ) −1 and more than ninety percent of the helium was determined to be 3He (at the 90% CL). Tracing helium from the second spectrum shows that about half of the 3He travel for an extended period of time in the geomagnetic field and that they originate from restricted geographic regions similar to protons and positrons.

Details

ISSN :
03702693
Database :
OpenAIRE
Journal :
Physics Letters B, Physics Letters B, Elsevier, 2000, 494, pp.193-202, HAL, Physics Letters. B, Vol. 494, No 3-4 (2000) pp. 193-202
Accession number :
edsair.doi.dedup.....5042d1397a07b7cd66fc8ee3763a496f