Geomagnetically trapped, albedo and solar energetic particles: Trajectory analysis and flux reconstruction with PAMELA

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

doi:10.1016/j.asr.2016.06.042

Cited by 16 publications

(9 citation statements)

References 22 publications

(31 reference statements)

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“…PAMELA is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment [see, e.g., Adriani et al, 2013Adriani et al, , 2015aAdriani et al, , 2015bAdriani et al, , 2016Bruno et al, 2015aBruno et al, , 2015b. In particular, PAMELA is able to precisely measure the SEP events during the solar cycles 23 and 24, in a wide energy interval encompassing the low-energy observations by in situ instruments and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors [Adriani et al, 2011[Adriani et al, , 2015cBruno et al, 2015cBruno et al, , 2016a. Full details about apparatus performance, proton selection, detector efficiencies, and experimental uncertainties can be found in Adriani et al [2013Adriani et al [ , 2014.…”

Section: Pamela Datamentioning

confidence: 99%

“…Since the present calibration work is focused on GOES 13 and 15 detectors (whose data are available starting from 2010 May and 2011 January, respectively), the 13 and 14 December 2006 SEP events [Adriani et al, 2011] were excluded from the selected data sample-a calibration study of the GOES 10/11/12 proton detectors, based on the aforementioned events, will be the object of a forthcoming publication. So far, a relatively low rate of energetic events has been registered during the current solar cycle, with the most relevant including the 17 May 2012 GLE [Gopalswamy et al, 2013;Adriani et al, 2015c;Bruno et al, 2016a] and the 6 January 2014 (sub? )GLE [Thakur et al, 2014].…”

Section: Pamela Datamentioning

confidence: 99%

“…In case of multiple events, the GCR component estimated for the first event is also used for the second one. Pitch angle anisotropies with respect to the local interplanetary magnetic field direction are accounted for by estimating the instrument "asymptotic" exposition along the satellite orbit (see Bruno et al [2015cBruno et al [ , 2016a for details).…”

Section: Pamela Datamentioning

confidence: 99%

“…PAMELA SEP fluxes are evaluated on a relatively short timescale (∼48 min), corresponding to spacecraft semi-orbits; the same time resolution is used for the EPEADs by averaging the 5 min intensities (https://satdat.ngdc.noaa.gov/sem/goes/data/new_avg/). Time bins characterized by anisotropic flux distributions (e.g., during the onset phase of the 17 May 2012 GLE event [Adriani et al, 2015c;Bruno et al, 2016a]) are excluded. 2.…”

Section: Epead Calibrationmentioning

confidence: 99%

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Calibration of the GOES 13/15 high‐energy proton detectors based on the PAMELA solar energetic particle observations

Bruno

2017

Space Weather

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The Energetic Proton, Electron, and Alpha Detector (EPEAD) and High Energy Proton and Alpha Detector (HEPAD) instruments on the Geostationary Operational Environmental Satellite (GOES) spacecraft have served over many years as monitors of the solar particle intensities, surveying the Sun and measuring in situ its effect on the near‐Earth solar‐terrestrial environment. However, the reconstruction of the differential energy spectra is affected by large uncertainties related to the poor energy resolution, the small geometrical factor, and the high contamination by out‐of‐acceptance particles. In this work, the high‐quality data set from the Payload for Antimatter Matter Exploration and Light‐nuclei Astrophysics (PAMELA) space mission is used to calibrate the high‐energy (>80 MeV) proton channels of the EPEAD and the HEPAD sensors on board the GOES 13 and 15, bringing the measured spectral intensities inline with those registered by PAMELA. Suggested corrections significantly reduce the uncertainties on the response of GOES detectors, thus improving the reliability of the spectroscopic observations of solar energetic particle events.

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Section: Pamela Datamentioning

confidence: 99%

Section: Pamela Datamentioning

confidence: 99%

Section: Pamela Datamentioning

confidence: 99%

Section: Epead Calibrationmentioning

confidence: 99%

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Calibration of the GOES 13/15 high‐energy proton detectors based on the PAMELA solar energetic particle observations

Bruno

2017

Space Weather

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“…The Resurs-DK1 satellite, carrying the apparatus, was launched into a semi-polar 70 • inclination, elliptical (350-610 km) orbit on 2006 June 15. PAMELA provided comprehensive observations of the galactic, solar and magnetospheric radiation in the near-Earth environment [24,25,26,27,28]. The mission lifetime was extended beyond 2015, in part due to the promise of new PAMELA SEP science, such as that presented in this paper.…”

Section: Pamela and Fermi Observationsmentioning

confidence: 99%

Long Duration Gamma-ray Flares and High Energy Solar Energetic Particles: Is there a Connection?

Nolfo¹,

Bruno²,

Ryan³

et al. 2019

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

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Long Duration Gamma-Ray Flares (LDGRFs) are characterized by delayed and long-duration gamma-ray emission above ∼50 MeV. Despite dozens of observations in the last decade with Fermi/LAT, the nature of this emission has been a challenge to explain. The highest energy emission has generally been attributed to the decay of pions produced by the interaction of highenergy protons with ambient solar material. The fact that the γ-ray emission is delayed from the onset of the initial eruption and that the emission is, in some cases, unusually long in duration suggests that particle acceleration occurs within large volumes extending to high altitudes, either by stochastic acceleration within large coronal loops or by back-precipitation from CME-driven shocks. We have tested these models by a making direct comparisons between the properties of the accelerated ion population at the flare derived from the observations of Fermi/LAT and those of solar energetic particles detected at Earth by PAMELA at comparable high energies. We investigated 27 high-energy gamma ray events (from [1]), and for 14 events we compare the two populations (SEPs in space and the interacting population at the Sun) and discuss the implications in terms of potential sources of the LDGRFs.

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Measurement of the low-energy charged particle background with the space detector HEPD

Vitale

2019

Rend. Fis. Acc. Lincei

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Geomagnetically trapped, albedo and solar energetic particles: Trajectory analysis and flux reconstruction with PAMELA

Cited by 16 publications

References 22 publications

Calibration of the GOES 13/15 high‐energy proton detectors based on the PAMELA solar energetic particle observations

Calibration of the GOES 13/15 high‐energy proton detectors based on the PAMELA solar energetic particle observations

Long Duration Gamma-ray Flares and High Energy Solar Energetic Particles: Is there a Connection?

Measurement of the low-energy charged particle background with the space detector HEPD

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