Cosmic ray measurements with Pamela experiment

Casolino, M.; Simone, N. De; Pascale, M. P. De; Felice, V. Di; Marcelli, L.; Minori, M.; Picozza, P.; Sparvoli, R.; Castellini, G.; Adriani, O.; Bonechi, L.; Bongi, M.; Bottai, S.; Fedele, D.; Papini, P.; Ricciarini, S.; Спиллантини, П.; Taddei, E.; Vannuccini, E.; Barbarino, G. C.; Campana, D.; Carbone, R.; Rosa, G. De; Osteria, G.; Boezio, M.; Bonvicini, V.; Mocchiutti, E.; Vacchi, A.; Zampa, G.; Zampa, N.; Bruno, A.; Cafagna, F.; Ricci, M.; Hofverberg, P.; Pearce, Mark; Carlson, P.; Bogomolov, É. A.; Krutkov, S. Y.; Nikonov, N.; Vasilyev, G.; Menn, W.; Simon, M.; Galper, A. M.; Grishantseva, L.; Koldashov, S. V.; Leonov, A. A.; Mikhailov, V. V.; Voronov, S. A.; Yurkin, Y. T.; Zverev, V. G.; Bazilevskaya, G. A.; Kvashnin, A. N.; Maksumov, O.; Stozhkov, Y. I.

doi:10.1016/j.nuclphysbps.2009.03.102

Cited by 11 publications

(4 citation statements)

References 22 publications

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“…To obtain an agreement with all the available data at low energies we need the injection spectrum α ∼ 1.5 − 2.0 below ∼ 4 GeV and a modulation parameter in the range Φ = 400−600 MV. The latter was set to match proton spectrum at low energy during the first year of Fermi LAT operation [34]. An example of such a calculation using GALPROP code [35] is shown in Fig.…”

Section: Resultsmentioning

confidence: 99%

Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV

Ackermann¹,

Ajello²,

Atwood³

et al. 2010

Phys. Rev. D

320

287

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We present the results of our analysis of cosmic-ray electrons using about 8 × 10 6 electron candidates detected in the first 12 months on-orbit by the Fermi Large Area Telescope. This work extends our previously published cosmic-ray electron spectrum down to 7 GeV, giving a spectral range of approximately 2.5 decades up to 1 TeV. We describe in detail the analysis and its validation using beam-test and on-orbit data. In addition, we describe the spectrum measured via a subset of events selected for the best energy resolution as a cross-check on the measurement using the full event sample. Our electron spectrum can be described with a power law ∝ E −3.08±0.05 with no prominent spectral features within systematic uncertainties. Within the limits of our uncertainties, we can accommodate a slight spectral hardening at around 100 GeV and a slight softening above 500 GeV.

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Section: Resultsmentioning

confidence: 99%

Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV

Ackermann¹,

Ajello²,

Atwood³

et al. 2010

Phys. Rev. D

320

287

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“…The estimated threshold for H and 4 He averages ∼120 MeV nucleon −1 over the instrument's upper hemisphere (the threshold for the spacecraft-facing side is similar but harder to assess). During 1997-2008 there is an excellent correlation between the E9 count rate and >120 MeV proton intensities from the BESS balloon-borne instrument (Shikaze et al 2007) and PAMELA mission (Casolino et al 2009), relating the E9 count rate and >120 MeV proton intensity with ∼2% accuracy.…”

Section: Observationsmentioning

confidence: 96%

Record-Setting Cosmic-Ray Intensities in 2009 and 2010

Mewaldt

Davis

Lave

et al. 2010

ApJ

186

151

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We report measurements of record-setting intensities of cosmic-ray nuclei from C to Fe, made with the Cosmic Ray Isotope Spectrometer carried on the Advanced Composition Explorer in orbit about the inner Sun-Earth Lagrangian point. In the energy interval from ∼70 to ∼450 MeV nucleon −1 , near the peak in the near-Earth cosmic-ray spectrum, the measured intensities of major species from C to Fe were each 20%-26% greater in late 2009 than in the 1997-1998 minimum and previous solar minima of the space age (1957-1997). The elevated intensities reported here and also at neutron monitor energies were undoubtedly due to several unusual aspects of the solar cycle 23/24 minimum, including record-low interplanetary magnetic field (IMF) intensities, an extended period of reduced IMF turbulence, reduced solar-wind dynamic pressure, and extremely low solar activity during an extended solar minimum. The estimated parallel diffusion coefficient for cosmic-ray transport based on measured solar-wind properties was 44% greater in 2009 than in the 1997-1998 solar-minimum period. In addition, the weaker IMF should result in higher cosmic-ray drift velocities. Cosmic-ray intensity variations at 1 AU are found to lag IMF variations by 2-3 solar rotations, indicating that significant solar modulation occurs inside ∼20 AU, consistent with earlier galactic cosmic-ray radial-gradient measurements. In 2010, the intensities suddenly decreased to 1997 levels following increases in solar activity and in the inclination of the heliospheric current sheet. We describe the conditions that gave cosmic rays greater access to the inner solar system and discuss some of their implications.

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“…In order to determine the solar activity parameter, the modulation potential, during recent times we determine the individual ϕ values by adjusting the solutions to measurements. This is done by using the proton spectrum during solar minimum conditions in July 2006 observed with the PAMELA instrument [see Casolino et al , 2009, Figure 1], with the energy given in GeV and the differential proton flux in protons (cm −2 sr −1 s −1 GeV −1 ). For each LIS an individual value of ϕ is needed to describe the observation as best as possible.…”

Section: Lis Proton Spectramentioning

confidence: 99%

On the importance of the local interstellar spectrum for the solar modulation parameter

Herbst¹,

Kopp²,

Heber³

et al. 2010

J. Geophys. Res.

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[1] Cosmogenic Isotopes are produced in the Earth's atmosphere due to the interaction of galactic cosmic rays with nuclei of atmospheric atoms. Among others, the 10 Be concentration in ice cores depends on the galactic cosmic ray flux outside of the Earth's magnetosphere and provides therefore a unique tool to investigate the solar modulation over very long time periods. In this study we investigate the importance of different local interstellar proton spectra often used in literature obtained outside of the Earth's magnetosphere. In order to parameterize the heliospheric modulation we apply the forcefield solution using individual local interstellar proton spectrum (LIS) model dependent values. Thus among atmospheric and magnetospheric processes, the 10 Be concentration depends on an interplay of the different LIS and their modulation parameters. Since 10 Be measurements do not provide any spectral resolution, PAMELA data have been used for a comparison with the calculated spectra and to provide the model dependent modulation parameters during the solar minimum in July 2006. Within the limitation of the force-field solution and the freedom in parameter space, all LIS lead to a reasonable agreement with the data. Taking the LIS dependency of the modulation parameter into account, we derive linear equations to convert the individual between the different LIS. The conversions used here are then applied to a long-term reconstruction of derived from a record of the cosmogenic radionuclide 10 Be. By using the derived LIS conversions, we show that the occasionally observed negative values in the reconstruction of Steinhilber et al. (2008) vanish if another LIS model is used. In order to estimate other processes which alter this conclusion, the influence of the palaeo-magnetic field has been included. Thus, if all inner-heliospheric effects on the 10 Be flux would be known, this investigation would have the potential to rule out certain LIS.

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Cosmic ray measurements with Pamela experiment

Cited by 11 publications

References 22 publications

Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV

Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV

Record-Setting Cosmic-Ray Intensities in 2009 and 2010

On the importance of the local interstellar spectrum for the solar modulation parameter

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