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Publications (10 of 191) Show all publications
Xie, F., Pearce, M. & SPHiNX, C. (2018). A Study of Background Conditions for Sphinx-The Satellite-Borne Gamma-Ray Burst Polarimeter. Galaxies, 6(2), Article ID 50.
Open this publication in new window or tab >>A Study of Background Conditions for Sphinx-The Satellite-Borne Gamma-Ray Burst Polarimeter
2018 (English)In: Galaxies, E-ISSN 2075-4434, Vol. 6, no 2, article id 50Article in journal (Refereed) Published
Abstract [en]

SPHiNX is a proposed satellite-borne gamma-ray burst polarimeter operating in the energy range 50-500 keV. The mission aims to probe the fundamental mechanism responsible for gamma-ray burst prompt emission through polarisation measurements. Optimising the signal-to-background ratio for SPHiNX is an important task during the design phase. The Geant4 Monte Carlo toolkit is used in this work. From the simulation, the total background outside the South Atlantic Anomaly (SAA) is about 323 counts/s, which is dominated by the cosmic X-ray background and albedo gamma rays, which contribute similar to 60% and similar to 35% of the total background, respectively. The background from albedo neutrons and primary and secondary cosmic rays is negligible. The delayed background induced by the SAA-trapped protons is about 190 counts/s when SPHiNX operates in orbit for one year. The resulting total background level of similar to 513 counts/s allows the polarisation of similar to 50 GRBs with minimum detectable polarisation less than 30% to be determined during the two-year mission lifetime.

Place, publisher, year, edition, pages
MDPI, 2018
Keywords
polarimeter, Compton scattering, GRB, background
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-232265 (URN)10.3390/galaxies6020050 (DOI)000436552000012 ()2-s2.0-85047239209 (Scopus ID)
Note

QC 20180719

Available from: 2018-07-19 Created: 2018-07-19 Last updated: 2018-07-19Bibliographically approved
Munini, R., Boezio, M., Bruno, A., Christian, E. C., Nolfo, G. A., Felice, V. D., . . . Potgieter, M. S. (2018). Evidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment. Astrophysical Journal, 853(1), Article ID 76.
Open this publication in new window or tab >>Evidence of Energy and Charge Sign Dependence of the Recovery Time for the 2006 December Forbush Event Measured by the PAMELA Experiment
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2018 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 853, no 1, article id 76Article in journal (Refereed) Published
Abstract [en]

New results on the short-term galactic cosmic-ray (GCR) intensity variation (Forbish decrease) in 2006 December measured by the PAMELA instrument are presented. Forbush decreases are sudden suppressions of the GCR intensities, which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). Most of the past measurements of this phenomenon were carried out with groundbased detectors such as neutron monitors or muon telescopes. These techniques allow only the indirect detection of the overall GCR intensity over an integrated energy range. For the first time, thanks to the unique features of the PAMELA magnetic spectrometer, the Forbush decrease, commencing on 2006 December 14 and following a CME at the Sun on 2006 December 13, was studied in a wide rigidity range (0.4-20 GV) and for different species of GCRs detected directly in space. The daily averaged GCR proton intensity was used to investigate the rigidity dependence of the amplitude and the recovery time of the Forbush decrease. Additionally, for the first time, the temporal variations in the helium and electron intensities during a Forbush decrease were studied. Interestingly, the temporal evolutions of the helium and proton intensities during the Forbush decrease were found to be in good agreement, while the low rigidity electrons (<2 GV) displayed a faster recovery. This difference in the electron recovery is interpreted as a charge sign dependence introduced by drift motions experienced by the GCRs during their propagation through the heliosphere.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2018
Keywords
cosmic rays, Sun: coronal mass ejections (CMEs), Sun: heliosphere, Sun: particle emission
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-222300 (URN)10.3847/1538-4357/aaa0c8 (DOI)000423361100012 ()2-s2.0-85041112562 (Scopus ID)
Funder
Swedish National Space BoardSwedish Research Council
Note

QC 20180206

Available from: 2018-02-06 Created: 2018-02-06 Last updated: 2018-02-19Bibliographically approved
Martucci, M., Munini, R., Boezio, M., Di Felice, V., Adriani, O., Barbarino, G. C., . . . Raath, J. L. (2018). Proton Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24. Astrophysical Journal Letters, 854(1), Article ID L2.
Open this publication in new window or tab >>Proton Fluxes Measured by the PAMELA Experiment from the Minimum to the Maximum Solar Activity for Solar Cycle 24
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2018 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 854, no 1, article id L2Article in journal (Refereed) Published
Abstract [en]

Precise measurements of the time-dependent intensity of the low-energy (<50 GeV) galactic cosmic rays (GCRs) are fundamental to test and improve the models that describe their propagation inside the heliosphere. In particular, data spanning different solar activity periods, i.e., from minimum to maximum, are needed to achieve comprehensive understanding of such physical phenomena. The minimum phase between solar cycles 23 and 24 was peculiarly long, extending up to the beginning of 2010 and followed by the maximum phase, reached during early 2014. In this Letter, we present proton differential spectra measured from 2010 January to 2014 February by the PAMELA experiment. For the first time the GCR proton intensity was studied over a wide energy range (0.08-50 GeV) by a single apparatus from a minimum to a maximum period of solar activity. The large statistics allowed the time variation to be investigated on a nearly monthly basis. Data were compared and interpreted in the context of a state-of-the-art three-dimensional model describing the GCRs propagation through the heliosphere.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2018
Keywords
astroparticle physics, cosmic rays, Sun: heliosphere
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-223499 (URN)10.3847/2041-8213/aaa9b2 (DOI)000424238600002 ()2-s2.0-85042130192 (Scopus ID)
Note

QC 20180223

Available from: 2018-02-23 Created: 2018-02-23 Last updated: 2018-02-23Bibliographically approved
Friis, M., Kiss, M., Mikhalev, V., Pearce, M. & Takahashi, H. (2018). The PoGO+ balloon-borne hard X-ray polarimetry mission. Galaxies, 6(1), Article ID 30.
Open this publication in new window or tab >>The PoGO+ balloon-borne hard X-ray polarimetry mission
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2018 (English)In: Galaxies, E-ISSN 2075-4434, Vol. 6, no 1, article id 30Article in journal (Refereed) Published
Abstract [en]

The PoGO mission, including the PoGOLite Pathfinder and PoGO+, aims to provide polarimetric measurements of the Crab system and Cygnus X-1 in the hard X-ray band. Measurements are conducted from a stabilized balloon-borne platform, launched on a 1 million cubic meter balloon from the Esrange Space Center in Sweden to an altitude of approximately 40 km. Several flights have been conducted, resulting in two independent measurements of the Crab polarization and one of Cygnus X-1. Here, a review of the PoGO mission is presented, including a description of the payload and the flight campaigns, and a discussion of some of the scientific results obtained to date. 

Place, publisher, year, edition, pages
MDPI AG, 2018
Keywords
Attitude control, Compton polarimeter, Crab, Cygnus X-1, Hard X-rays, Payload design, Scientific ballooning
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-227400 (URN)10.3390/galaxies6010030 (DOI)000428554900030 ()2-s2.0-85043362309 (Scopus ID)
Note

Export Date: 9 May 2018; Article; Correspondence Address: Kiss, M.; KTH Royal Institute of Technology, Department of PhysicsSweden; email: mozsi@kth.se; Funding details: Knut och Alice Wallenbergs Stiftelse; Funding details: JSPS, Japan Society for the Promotion of Science; Funding details: TRC, The Research Council; Funding details: SNSB, Swedish National Space Board; Funding details: DST, Department of Science and Technology, Ministry of Science and Technology; Funding details: CASIS, Center for the Advancement of Science in Space; Funding text: Acknowledgments: This research was supported in Sweden by The Swedish National Space Board, The Knut and Alice Wallenberg Foundation, and The Swedish Research Council. In Japan, support was provided by the Japan Society for Promotion of Science and ISAS/JAXA. SSC are thanked for providing expert mission support and launch services at Esrange Space Center. DST Control developed the PoGO+ attitude control system under the leadership of J.-E. Strömberg. Contributions from past collaboration members and students are acknowledged. QC 20180529

Available from: 2018-05-29 Created: 2018-05-29 Last updated: 2018-06-25Bibliographically approved
Adriani, O., Barbarino, G. C., Bazilevskaya, G. A., Bellotti, R., Boezio, M., Bogomolov, E. A., . . . Zampa, N. (2018). Unexpected Cyclic Behavior in Cosmic-Ray Protons Observed by PAMELA at 1 au. Astrophysical Journal Letters, 852(2), Article ID L28.
Open this publication in new window or tab >>Unexpected Cyclic Behavior in Cosmic-Ray Protons Observed by PAMELA at 1 au
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2018 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 852, no 2, article id L28Article in journal (Refereed) Published
Abstract [en]

Protons detected by the PAMELA experiment in the period 2006-2014 have been analyzed in the energy range between 0.40 and 50 GV to explore possible periodicities besides the well known solar undecennial modulation. An unexpected clear and regular feature has been found at rigidities below 15 GV, with a quasi-periodicity of similar to 450 days. A possible Jovian origin of this periodicity has been investigated in different ways. The results seem to favor a small but not negligible contribution to cosmic rays from the Jovian magnetosphere, even if other explanations cannot be excluded.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD, 2018
Keywords
cosmic rays, Sun: heliosphere
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-221941 (URN)10.3847/2041-8213/aaa403 (DOI)000419785000004 ()2-s2.0-85040668902 (Scopus ID)
Note

QC 20180130

Available from: 2018-01-30 Created: 2018-01-30 Last updated: 2018-01-30Bibliographically approved
Chauvin, M., Friis, M., Jackson, M., Kawano, T., Kiss, M., Mikhalev, V., . . . Pearce, M. (2017). Calibration and performance studies of the balloon-borne hard X-ray polarimeter PoGO. Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 859, 125-133
Open this publication in new window or tab >>Calibration and performance studies of the balloon-borne hard X-ray polarimeter PoGO
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2017 (English)In: Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, ISSN 0168-9002, E-ISSN 1872-9576, Vol. 859, p. 125-133Article in journal (Refereed) Published
Abstract [en]

Polarimetric observations of celestial sources in the hard X-ray band stand to provide new information on emission mechanisms and source geometries. PoGO+ is a Compton scattering polarimeter (20-150 keV) optimised for the observation of the Crab (pulsar and wind nebula) and Cygnus X-1 (black hole binary), from a stratospheric balloon-borne platform launched from the Esrange Space Centre in summer 2016. Prior to flight, the response of the polarimeter has been studied with polarised and unpolarised X-rays allowing a Geant4-based simulation model to be validated. The expected modulation factor for Crab observations is found to be M-Crab = (41.75 +/- 0.85)%, resulting in an expected Minimum Detectable Polarisation (MDP) of 7.3% for a 7 day flight. This will allow a measurement of the Crab polarisation parameters with at least 5 sigma statistical significance assuming a polarisation fraction similar to 20% - a significant improvement over the PoGOLite Pathfinder mission which flew in 2013 and from which the PoGO+ design is developed.

Place, publisher, year, edition, pages
ELSEVIER SCIENCE BV, 2017
Keywords
X-ray, Polarisation, Compton scattering, Scientific ballooning, Crab, Cygnus X-1, Monte Carlo simulations
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-219572 (URN)10.1016/j.nima.2017.03.027 (DOI)000402464700018 ()2-s2.0-85018696451 (Scopus ID)
Note

QC 20171207

Available from: 2017-12-07 Created: 2017-12-07 Last updated: 2018-05-21Bibliographically approved
Bruno, A., Adriani, O., Barbarino, G. C., Bazilevskaya, G. A., Bellotti, R., Boezio, M., . . . Zampa, N. (2017). Geomagnetically trapped, albedo and solar energetic particles: Trajectory analysis and flux reconstruction with PAMELA. Advances in Space Research, 60(4), 788-795
Open this publication in new window or tab >>Geomagnetically trapped, albedo and solar energetic particles: Trajectory analysis and flux reconstruction with PAMELA
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2017 (English)In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 60, no 4, p. 788-795Article in journal (Refereed) Published
Abstract [en]

The PAMELA satellite experiment is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment. Thanks to its identification capabilities and the semi-polar orbit, PAMELA is able to precisely measure the energetic spectra and the angular distributions of the different cosmic-ray populations over a wide latitude region, including geomagnetically trapped and albedo particles. Its observations comprise the solar energetic particle events between solar cycles 23 and 24, and the geomagnetic cutoff variations during magnetospheric storms. PAMELA's measurements are supported by an accurate analysis of particle trajectories in the Earth's magnetosphere based on a realistic geomagnetic field modeling, which allows the classification of particle populations of different origin and the investigation of the asymptotic directions of arrival.

Place, publisher, year, edition, pages
Elsevier, 2017
Keywords
Cosmic-rays, Radiation belts, Albedo particles, Geomagnetic cutoff, Solar energetic particles
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-211588 (URN)10.1016/j.asr.2016.06.042 (DOI)000405975700005 ()2-s2.0-85002846984 (Scopus ID)
Funder
Swedish National Space BoardSwedish Research Council
Note

QC 20170815

Available from: 2017-08-15 Created: 2017-08-15 Last updated: 2017-08-15Bibliographically approved
Mikhailov, V. V., Adriani, O., Barbarino, G., Bazilevskaya, G. A., Bellotti, R., Boezio, M., . . . Zampa, N. (2017). Sharp increasing of positron to electron fluxes ratio below 2 GV measured by the PAMELA. Journal of Physics, Conference Series, 798(1), Article ID 012019.
Open this publication in new window or tab >>Sharp increasing of positron to electron fluxes ratio below 2 GV measured by the PAMELA
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2017 (English)In: Journal of Physics, Conference Series, ISSN 1742-6588, E-ISSN 1742-6596, Vol. 798, no 1, article id 012019Article in journal (Refereed) Published
Abstract [en]

Magnetic spectrometer PAMELA was launched onboard a satellite Resurs-DK1 into low-Earth polar orbit with altitude 350-600 km to study cosmic ray antiparticle fluxes in a wide energy range from ∼ 100 MeV to hundreds GeV. This paper presents the results of observations of temporal variations of the positron and electron fluxes in the 2006-2015. The ratio of the positron and electron fluxes below 2 GV shows sharp increasing since 2014 due to changing of the polarity of the solar magnetic field.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2017
Keywords
Astrophysics, Cosmology, Electrons, Magnetic polarity, Orbits, Positrons, Earth polar orbit, Electron flux, Magnetic spectrometers, Solar magnetic fields, Temporal variation, Wide energy range, Cosmic rays
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-208027 (URN)10.1088/1742-6596/798/1/012019 (DOI)2-s2.0-85016239114 (Scopus ID)
Note

QC 20170602

Available from: 2017-06-02 Created: 2017-06-02 Last updated: 2017-06-02Bibliographically approved
Galper, A. M., Sparvoli, R., Adriani, O., Barbarino, G., Bazilevskaya, G. A., Bellotti, R., . . . Zampa, N. (2017). The PAMELA experiment: A decade of Cosmic Ray Physics in space. Journal of Physics, Conference Series, 798(1), Article ID 012033.
Open this publication in new window or tab >>The PAMELA experiment: A decade of Cosmic Ray Physics in space
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2017 (English)In: Journal of Physics, Conference Series, ISSN 1742-6588, E-ISSN 1742-6596, Vol. 798, no 1, article id 012033Article in journal (Refereed) Published
Abstract [en]

The PAMELA detector was launched on June 15 th of 2006 on board the Russian Resurs-DK1 satellite and during ten years of continuous data-taking it has observed very interesting features in cosmic rays, especially in the fluxes of protons, helium and electrons. Moreover, PAMELA measurements of cosmic antiproton and positron fluxes and positron-to-all-electron ratio have set strong constraints to the nature of Dark Matter. Measurements of boron, carbon, lithium and beryllium (together with the isotopic fraction) have also shed new light on the elemental composition of the cosmic radiation. Search for signatures of more exotic processes (such as the ones involving Strange Quark Matter) has also been pursued. Furthermore, over the years the instrument has allowed a constant monitoring of the solar activity and a prolonged study of the solar modulation, improving the comprehension of the heliosphere mechanisms. PAMELA has also measured the radiation environment around the Earth, and detected for the first time the presence of an antiproton radiation belt surrounding our planet. In this highlight paper PAMELA main results will be reviewed.

Place, publisher, year, edition, pages
Institute of Physics Publishing (IOPP), 2017
Keywords
Astrophysics, Carbon, Cosmology, Earth (planet), High energy physics, Positrons, Radiation belts, Solar energy, Continuous data, Elemental compositions, Heliospheres, Measurements of, Quark matter, Radiation environments, Solar activity, Solar modulation, Cosmic rays
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-208030 (URN)10.1088/1742-6596/798/1/012033 (DOI)2-s2.0-85016270621 (Scopus ID)
Note

QC 20170602

Available from: 2017-06-02 Created: 2017-06-02 Last updated: 2017-06-02Bibliographically approved
Dong, Y., Pearce, M., Ryde, F., Zhang, S. & et al., . (2016). Experimental verification of the HERD prototype at CERN SPS. In: Proceedings of SPIE: SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY: . Paper presented at Conference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray, Edinburgh, SCOTLAND, JUN 26-JUL 01, 2016. SPIE - International Society for Optical Engineering
Open this publication in new window or tab >>Experimental verification of the HERD prototype at CERN SPS
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2016 (English)In: Proceedings of SPIE: SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, SPIE - International Society for Optical Engineering, 2016Conference paper, Published paper (Refereed)
Abstract [en]

The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads of the cosmic light house program onboard China's Space Station, which is planned for operation starting around 2020 for about 10 years. Beam test with a HERD prototype, to verify the HERD specifications and the reading out method of wavelength shifting fiber and image intensified CCD, was taken at CERN SPS in November, 2015. The prototype is composed of an array of 5∗5∗10 LYSO crystals, which is 1/40th of the scale of HERD calorimeter. Experimental results on the performances of the calorimeter are discussed.

Place, publisher, year, edition, pages
SPIE - International Society for Optical Engineering, 2016
Keywords
3d imaging, Calorimeter, Cosmic ray, Dark matter, Gamma ray, ICCD, Shower, WLSF
National Category
Accelerator Physics and Instrumentation
Identifiers
urn:nbn:se:kth:diva-202109 (URN)10.1117/12.2231804 (DOI)000387731500178 ()2-s2.0-85003633069 (Scopus ID)
Conference
Conference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray, Edinburgh, SCOTLAND, JUN 26-JUL 01, 2016
Note

QC 20170217

Available from: 2017-02-17 Created: 2017-02-17 Last updated: 2017-02-17Bibliographically approved
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ORCID iD: ORCID iD iconorcid.org/0000-0001-7011-7229

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