Proton Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24

Martucci, M.; Munini, R.; Boezio, M.; Felice, V. Di; Adriani, O.; Barbarino, G. C.; Bazilevskaya, G. A.; Bellotti, R.; Bongi, M.; Bonvicini, V.; Bottai, S.; Bruno, A.; Cafagna, F.; Campana, D.; Carlson, P.; Casolino, M.; Castellini, G.; Santis, C. De; Galper, A. M.; Karelin, A. V.; Koldashov, S. V.; Koldobskiy, S.; Krutkov, S. Y.; Kvashnin, A. N.; Leonov, A.; Malakhov, V.; Marcelli, L.; Marcelli, N.; Mayorov, A. G.; Menn, W.; Мерге, М.; Mikhailov, V. V.; Mocchiutti, E.; Monaco, A.; Mori, N.; Osteria, G.; Panico, B.; Papini, P.; Pearce, Mark; Picozza, P.; Ricci, M.; Ricciarini, S.; Simon, M.; Sparvoli, R.; Спиллантини, П.; Stozhkov, Y. I.; Vacchi, A.; Vannuccini, E.; Vasilyev, G.; Voronov, S. A.; Yurkin, Y. T.; Zampa, G.; Zampa, N.; Potgieter, M. S.; Raath, Jan-Louis

doi:10.3847/2041-8213/aaa9b2

Cited by 89 publications

(74 citation statements)

References 38 publications

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“…Above about 6 GV, the modulation effect becomes progressively less evident. These results are consistent with PAMELA proton observations reported recently by Martucci et al (2018); see also Di Felice et al (2017) and Munini et al (2018).…”

Section: Simulated Spectrasupporting

confidence: 94%

“…In this context, we note that as more precise CR spectra become available, e.g., daily fluxes or spectra over a wide energy range for a complete 11 yr solar cycle, it will become necessary to adapt an automated statistical tool to scan the full parameter space, investigating, e.g., if the rigidity dependence of all three diffusion coefficients is exactly the same, or if drift effects are changing meaningfully toward solar maximum activity; see, e.g., Martucci et al (2018) and Aslam et al (2019). Apart from proton spectra, the AMS-02 helium flux data have become available as well (Aguilar et al 2018a).…”

Section: Discussionmentioning

confidence: 99%

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A Numerical Study of Cosmic Proton Modulation Using AMS-02 Observations

Luo

Potgieter

Bindi

et al. 2019

ApJ

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Since 2011 May, the Alpha Magnetic Spectrometer (AMS-02) on board the International Space Station has provided monthly cosmic proton fluxes for various low-rigidity levels (P<50 GV). These precise measurements, in terms of high time and rigidity resolution, have provided a good opportunity to study cosmic ray modulation over a wide range of rigidities, together with transient events. Subsequently, a comprehensive numerical transport model has been constructed, based on Parker's transport equation that includes all known physical mechanisms: diffusion, convection, drift, and adiabatic cooling. Propagating diffusion barriers to simulate Forbush decreases (Fds) and global merged interaction regions (GMIRs) have also been incorporated: (1) utilizing a time-varying tilt angle of the heliospheric current sheet and interplanetary magnetic field, the general trend of the time variation of cosmic proton fluxes has been reproduced; (2) the Fd events in 2011 October and 2012 March have been simulated, and the first GMIR event in solar cycle 24 has also been simulated and studied; and (3) the rigidity dependence of the proton fluxes, as revealed by the AMS-02 data, has been reproduced with the appropriate chosen rigidity dependent diffusion coefficients. In order to reproduce the proton observations, we find that apart from the transient events, the derived mean free paths in interplanetary space also need to be changed with time.

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Section: Simulated Spectrasupporting

confidence: 94%

Section: Discussionmentioning

confidence: 99%

A Numerical Study of Cosmic Proton Modulation Using AMS-02 Observations

Luo

Potgieter

Bindi

et al. 2019

ApJ

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“…In the past decades, precious information have been gained thanks to space missions CRIS/ACE (Wiedenbeck et al, 2009), IMP-7/8 (Garcia-Munoz et al, 1997), Ulysses (Heber et al, 2009), and Voyager-1 (Cummings et al, 2016). The recent data from EPHIN/SOHO (Kühl et al, 2016), PAMELA (Adriani et al, 2013;Martucci et al, 2018), and AMS (Aguilar et al, 2018a,b) are giving a deep characterization of effect in the current Solar Cycle 24 (Bindi, 2017). The solar modulation effect is known to be caused by a combination of basic processes such as magnetic diffusion, drift motion, convection, and adiabatic energy losses (Parker, 1965;Krymsky, 1964;Fisk, 1971;Jokipii, 1967).…”

Section: Introductionmentioning

confidence: 99%

Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24

Tomassetti

Barão

Bertucci

et al. 2019

Advances in Space Research

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Thanks to space-borne experiments of cosmic-ray (CR) detection, such as the AMS and PAMELA missions in low-Earth orbit, or the Voyager-1 spacecraft in the interstellar space, a large collection of multi-channel and time-resolved CR data has become available. Recently, the AMS experiment has released new precision data, on the proton and helium fluxes in CRs, measured on monthly basis during its first six years of mission. The AMS data reveal a remarkable long-term behavior in the temporal evolution of the proton-to-helium ratio at rigidity R ≡ p/Z 3 GV. As we have argued in a recent work, such a behavior may reflect the transport properties of low-rigidity CRs in the inteplanetary space. In particular, it can be caused by mass/charge dependence of the CR diffusion coefficient. In this paper, we present our developments in the numerical modeling of CR transport in the Milky Way and in the heliosphere. Within our model, and with the help of approximated analytical solutions, we describe in details the relations between the properties of CR diffusion and the time-dependent evolution of the proton-to-helium ratio.

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“…The next phase of this study is to apply this model to Galactic electron and positron spectra observed by AMS -02 (Aguilar et al 2018) for the period 2011-2017, as was done for PAMELA protons (Martucci et al 2018). These AMS -02 observations together with the PAMELA observations for 2006-2009, can provide electron and positron spectra over a full solar cycle.…”

Section: Discussionmentioning

confidence: 99%

Modeling of Heliospheric Modulation of Cosmic-Ray Positrons in a Very Quiet Heliosphere

Aslam

Bisschoff

Potgieter

et al. 2019

ApJ

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Heliospheric modulation conditions were unusually quite during the last solar minimum activity between Solar Cycles 23/24. Fortunately, the PAMELA space-experiment measured six-month averaged Galactic positron spectra for the period July 2006 to December 2009, over an energy range of 80 MeV to 30 GeV, which is important for solar modulation. The highest level of Galactic positrons was observed at Earth during the July-December 2009 period. A well-established, comprehensive three-dimensional (3D) numerical model is applied to study the modulation of the observed positron spectra. This model had been used previously to understand the modulation of Galactic protons and electrons also measured by PAMELA for the same period. First, a new very local interstellar spectrum for positrons is constructed, using the well-known GALPROP code together with the mentioned PAMELA observations. The 3D model is used to distinguish between the dominant mechanisms responsible for the heliospheric modulation of Galactic positrons, and to understand the effect of particle drift during this unusual minimum in particular, which is considered diffusion dominant, even though particle drift still had a significant role in modulating positrons. Lastly, the expected intensity of Galactic positrons during an A>0 polarity minimum, with similar heliospheric conditions than for 2006-2009, is predicted to be higher than what was observed by PAMELA for the 2006-2009 unusual minimum.

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Proton Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24

Cited by 89 publications

References 38 publications

A Numerical Study of Cosmic Proton Modulation Using AMS-02 Observations

A Numerical Study of Cosmic Proton Modulation Using AMS-02 Observations

Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24

Modeling of Heliospheric Modulation of Cosmic-Ray Positrons in a Very Quiet Heliosphere

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