A source of very energetic oxygen located in Jupiter’s inner radiation belts

Elias Roussos; Christina Cohen; Peter Kollmann; Marco Pinto; Norbert Krupp; Patricia Gonçalves; Konstantinos Dialynas

doi:10.1126/sciadv.abm4234

Earth's magnetotail as the reservoir of accelerated single‐ and multicharged oxygen ions replenishing radiation belts

Journal of Geophysical Research Space Physics ◽

10.1029/2020ja028217 ◽

2021 ◽

Author(s):

M. I. Panasyuk ◽

E. I. Zhukova ◽

V. V. Kalegaev ◽

H. V. Malova ◽

V.Yu. Popov ◽

...

Keyword(s):

Radiation Belts ◽

Oxygen Ions

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The effects of the big storm events in the first half of 2015 on the radiation belts observed by EPT/PROBA-V

Annales Geophysicae ◽

10.5194/angeo-34-75-2016 ◽

2016 ◽

Vol 34 (1) ◽

pp. 75-84 ◽

Cited By ~ 10

Author(s):

V. Pierrard ◽

G. Lopez Rosson

Keyword(s):

Charged Particle ◽

High Resolution ◽

Geomagnetic Storm ◽

Energetic Particle ◽

High Energy ◽

Radiation Belts ◽

Radiation Environment ◽

Storm Event ◽

Storm Events ◽

Particle Radiation

Abstract. With the energetic particle telescope (EPT) performing with direct electron and proton discrimination on board the ESA satellite PROBA-V, we analyze the high-resolution measurements of the charged particle radiation environment at an altitude of 820 km for the year 2015. On 17 March 2015, a big geomagnetic storm event injected unusual fluxes up to low radial distances in the radiation belts. EPT electron measurements show a deep dropout at L > 4 starting during the main phase of the storm, associated to the penetration of high energy fluxes at L < 2 completely filling the slot region. After 10 days, the formation of a new slot around L = 2.8 for electrons of 500–600 keV separates the outer belt from the belt extending at other longitudes than the South Atlantic Anomaly. Two other major events appeared in January and June 2015, again with injections of electrons in the inner belt, contrary to what was observed in 2013 and 2014. These observations open many perspectives to better understand the source and loss mechanisms, and particularly concerning the formation of three belts.

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Separating γ- and hadron-induced cosmic ray air showers with feed-forward neural networks using the charged particle information

Astroparticle Physics ◽

10.1016/0927-6505(95)00028-4 ◽

1995 ◽

Vol 4 (2) ◽

pp. 119-132 ◽

Cited By ~ 12

Author(s):

S. Westerhoff ◽

B. Funk ◽

A. Lindner ◽

N. Magnussen ◽

H. Meyer ◽

...

Keyword(s):

Neural Networks ◽

Charged Particle ◽

Cosmic Ray ◽

Air Showers ◽

Feed Forward ◽

Feed Forward Neural Networks

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Implications of unusual pitch-angle distributions observed by ISEE-1 and 2

Annales Geophysicae ◽

10.5194/angeo-24-3099-2006 ◽

2006 ◽

Vol 24 (11) ◽

pp. 3099-3113 ◽

Cited By ~ 2

Author(s):

C. A. Zuluaga ◽

E. S. Beiser ◽

J. Chen ◽

T. A. Fritz

Keyword(s):

Charged Particle ◽

High Latitude ◽

Pitch Angle ◽

Angular Resolution ◽

Radial Distance ◽

Local Magnetic Field ◽

Particle Source ◽

Small Pitch ◽

Short Period ◽

Geosynchronous Satellites

Abstract. Unusual energetic particle pitch angle distributions (PADs) were observed by the ISEE-1 and 2 satellites at 3 h MLT and a radial distance of about 10–15 RE during the time period of 07:00-14:00 UT on 3 March 1979. The ISEE-1 satellite obtained complete 3-D distributions of energetic proton and electron fluxes as a function of energy, while ISEE-2 was configured to provide higher time resolution but less angular resolution than ISEE-1. The ISEE-1 observed a butterfly PAD (a minimum in the 90° PA particle flux) for a period of about 2 h (10:00–12:00 UT) for the electrons, and 3 h (09:00–12:00 UT) for the protons over an energy range of 22.5–189 keV (E1–E4) for the electrons and 24–142 keV (P1–P4) for the protons. The small pitch angle (15°, 30°) charged particles (electrons and protons) are seen to behave collectively in all four energy ranges. The relative differences in electron fluxes between 15° PA and 90° PA are more significant for higher energy channels during the butterfly PAD period. Three different types of electron PADs (butterfly, isotropic, and peaked-at-90°) were observed at the same location and time as a function of energy for a short period of time before 10:00 UT. Electron butterfly distributions were also observed by the ISEE-2 for about 1.5 h over 28–62 keV (E2–E4), although less well resolved than ISEE-1. Unlike the ISEE-1, no butterfly distributions were resolved in the ISEE-2 proton PADs due to less angular resolution. The measured drift effects by ISEE-1 suggest that the detected protons were much closer to the particle source than the electrons along their trajectories, and thus ruled out a nightside source within 18:00 MLT to 03:00 MLT. Compared to 07:30 UT, the charged particle fluxes measured by ISEE-1 were enhanced by up to three orders of magnitude during the period 08:30–12:00 UT. From 09:10:00 UT to 11:50 UT, the geomagnetic conditions were quiet (AE<100 nT), the LANL geosynchronous satellites observed no substorms, and the local magnetic field measured by ISEE-1 was almost constant, while the small PA charged particle (both electron and proton) fluxes measured by ISEE-1 increased gradually, which implies a particle source other than the substorm source. Based on detailed particle trajectory tracings in a realistic geomagnetic field model, the 50–200 keV protons with small PA at 10:00 UT ISEE-1 location on 3 March 1979 were passing through the northern high-altitude and high-latitude morningside region where the cusp should be located under a dawnward IMF component condition, while those protons with large PA may connect to the high-latitude morningside magnetopause. It is possible that the cusp source is responsible for the all particles observed during the event.

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Time-calibration of the semiconductor charged particle detector using the ThC' α-particle source

Nuclear Instruments and Methods ◽

10.1016/0029-554x(75)90665-5 ◽

1975 ◽

Vol 127 (4) ◽

pp. 601-602

Author(s):

M. Matoba ◽

J. Niidome ◽

Y. Matsumoto ◽

H. Yamamoto ◽

N. Koori

Keyword(s):

Charged Particle ◽

Particle Detector ◽

Particle Source ◽

Time Calibration

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A radiation belt of energetic protons located between Saturn and its rings

Science ◽

10.1126/science.aat1962 ◽

2018 ◽

Vol 362 (6410) ◽

pp. eaat1962 ◽

Cited By ~ 12

Author(s):

E. Roussos ◽

P. Kollmann ◽

N. Krupp ◽

A. Kotova ◽

L. Regoli ◽

...

Keyword(s):

Radiation Belt ◽

Cosmic Ray ◽

High Energy ◽

Radiation Belts ◽

Exchange Reactions ◽

Dipole Magnetic Field ◽

Imaging Instrument ◽

Multiple Charge ◽

Strong Dipole ◽

Dense Atmosphere

Saturn has a sufficiently strong dipole magnetic field to trap high-energy charged particles and form radiation belts, which have been observed outside its rings. Whether stable radiation belts exist near the planet and inward of the rings was previously unknown. The Cassini spacecraft’s Magnetosphere Imaging Instrument obtained measurements of a radiation belt that lies just above Saturn’s dense atmosphere and is decoupled from the rest of the magnetosphere by the planet’s A- to C-rings. The belt extends across the D-ring and comprises protons produced through cosmic ray albedo neutron decay and multiple charge-exchange reactions. These protons are lost to atmospheric neutrals and D-ring dust. Strong proton depletions that map onto features on the D-ring indicate a highly structured and diverse dust environment near Saturn.

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Search for galactic γ-rays with energies greater than 500 MeV on board OGO-5

Symposium - International Astronomical Union ◽

10.1017/s0074180900004435 ◽

1970 ◽

Vol 37 ◽

pp. 297-299 ◽

Cited By ~ 1

Author(s):

J. A. M. Bleeker ◽

J. J. Burger ◽

A. J. M. Deerenberg ◽

H. C. Van De Hulst ◽

A. Scheepmaker ◽

...

Keyword(s):

Cosmic Ray ◽

Radiation Belts ◽

Eccentric Orbit ◽

The Earth ◽

Γ Rays ◽

Γ Ray

A cosmic ray detector, sensitive to γ-Rays with energies greater than 500 MeV is being flown on board the OGO-5 satellite. The spacecraft was launched into a highly eccentric orbit, apogee 145000 km, on March 4, 1968. γ-Ray observations are restricted to altitudes higher than 80000 km, thereby excluding interference from the radiation belts and reducing the influence from the earth albedo flux. A description of the instrument is published in the literature (Rogowski et al., 1969).

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