Evidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment

Munini, R.; Boezio, M.; Bruno, A.; Christian, Eric; Nolfo, G. A. de; Felice, V. Di; Martucci, M.; Мерге, М.; Richardson, I. G.; Ryan, J. M.; Stochaj, S. J.; Adriani, O.; Barbarino, G. C.; Bazilevskaya, G. A.; Bellotti, R.; Bongi, M.; Bonvicini, V.; Bottai, S.; 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.; Mayorov, A. G.; Menn, W.; 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.

doi:10.3847/1538-4357/aaa0c8

Cited by 31 publications

(14 citation statements)

References 47 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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%

“…We should be able to investigate this feature in detail and hopefully find the basic physical explanation for it. 10 A similar challenge is the interpretation of the observed electron-positron ratio over the period of solar maximum, including the reversal of the IMF polarity during extreme solar activity, first reported using PAMELA data by Munini et al (2018) and now for AMS-02 data by Aguilar et al (2018b).…”

Section: Discussionmentioning

confidence: 99%

“…This particular approach has already been used to reproduce PAMELA proton spectra (Potgieter et al 2014) and electron spectra (Potgieter et al 2015;Di Felice et al 2017) from 2006 to 2009. Luo et al (2018) also adapted this functional form to simulate electron Fds for the first time; see also Munini et al (2018). In this context, we prefer to simplify rather than complicate our modeling approach using SDEs, which is inherently complicated and rather tedious, especially when comparisons are made to observations.…”

Section: Diffusion Coefficients and Diffusion Barrier Modelmentioning

confidence: 99%

See 2 more Smart Citations

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

Luo

Potgieter

Bindi

et al. 2019

ApJ

View full text Add to dashboard Cite

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.

show abstract

Section: Simulated Spectrasupporting

confidence: 94%

Section: Discussionmentioning

confidence: 99%

Section: Diffusion Coefficients and Diffusion Barrier Modelmentioning

confidence: 99%

See 1 more Smart Citation

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

Luo

Potgieter

Bindi

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…Observations of the long-term evolution of GRC intensities can date back to 1950s [4], with significantly improved measurements by PAMELA [5] and AMS-02 [6,7] recently. The FD behaviors of different particle species were also observed for the first time by PAMELA [8].…”

Section: Introductionmentioning

confidence: 90%

Observation of time evolution of cosmic ray electron and positron flux with Dark Matter Particle Explorer

Zang¹,

Liu²,

Yuan³

et al. 2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

View full text Add to dashboard Cite

In this analysis, we measure the time-dependence of the primary cosmic ray electron and positron (CRE) fluxes using over 3 years of data from the Dark Matter Particle Explorer (DAMPE). The monthly CRE fluxes show clear variabilities due to the solar modulation effect. We also investigate the short-term structures of the CRE fluxes in September, 2017 when an X level solar flare event occurred. Energy-dependent Forbush descreases have been observed. The Forbush decrease amplitude and recovery time of the CRE fluxes depend on energies, which may have interesting implication in understanding the disturbances of interplanetary environment due to solar activities. All these results indicate that the DAMPE has a great potential to probe the interplay between particles and the heliosphere environment.

show abstract

“…Although particle drift played a significant role (Di Felice et al 2017; Munini et al 2018) in the modulation of electrons and positrons during the unusual 2006-2009 minimum period, the process was diffusion dominated. As such, an unexpected result for an A<0 solar minimum epoch (phase).…”

Section: Discussionmentioning

confidence: 99%

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

Aslam

Bisschoff

Potgieter

et al. 2019

ApJ

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Evidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment

Cited by 31 publications

References 47 publications

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

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

Observation of time evolution of cosmic ray electron and positron flux with Dark Matter Particle Explorer

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

Contact Info

Product

Resources

About