The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons Mission

McNutt, R. L.; Livi, S.; Gurnee, R. S.; Hill, M. E.; Cooper, Kim A.; Andrews, G. B.; Keath, E. P.; Krimigis, S. M.; Mitchell, D. G.; Tossman, B. E.; Bagenal, F.; Boldt, J.; Bradley, Walter; Devereux, William S.; Ho, G. C.; Jaskulek, S.; LeFevere, Thomas W.; Malcom, Horace; Marcus, Geoffrey A.; Hayes, J. R.; Moore, G. Ty; Perry, Mark; Williams, Bruce D.; Wilson, Paul; Brown, L. E.; Kusterer, M. B.; Vandegriff, J. D.

doi:10.1007/s11214-008-9436-y

Cited by 52 publications

(27 citation statements)

References 50 publications

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“…The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons spacecraft is a compact, light‐weight (1.5 kg), multidirectional, time‐of‐flight spectrometer measuring ions from ∼15 keV to over 1 MeV, and electrons from 25 keV through ∼0.5 MeV [ McNutt et al , 2008]. PEPSSI obtains angular distributions through multiple views that continuously sample within a 160° by 12° field of view.…”

Section: Observationsmentioning

confidence: 99%

Composition of energetic particles in the Jovian magnetotail

et al. 2009

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The New Horizons spacecraft offered a unique opportunity to explore the distant Jovian magnetotail to over 2565 Jovian Radii. Previous observations of ion abundances were available only out to ∼150 Jovian Radii. During the 100+‐day exploration of the magnetotail, New Horizons observed a number of energetic particle bursts, similar to particle bursts observed by Galileo much closer to Jupiter. We examine the composition of these dynamic structures and compare the ion abundances with those found in more quiescent regions. We show that the composition of these energetic bursts is Iogenic and suggest it is within these bursts that Jupiter releases the bulk of its energetic material. We report on the ion composition ratios as a function distance down the Jovian magnetotail, finding an increasing intrusion of interplanetary He into the tail with distance from the planet. These observations show that the radial gradients in particle flux observed by Galileo in the magnetotail close to Jupiter extend deep into the magnetotail. We observed large electron intensities at the noon magnetopause crossing and continuous strong 10‐h modulations in electron intensity to nearly 500 Jovian Radii toward the tail. Our current hypothesis is that Jupiter enforces azimuthal rotation on some fields to distances of over a few hundred Jovian Radii. At distances greater than 500 Jovian Radii we observed long‐duration periods of strong electron anisotropy beaming down the magnetotail. Intermittent observations of 10‐h electron modulations continue into distant regions of the magnetotail and we suggest these are a signature of occasional field line connection to the magnetosphere.

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Section: Observationsmentioning

confidence: 99%

Composition of energetic particles in the Jovian magnetotail

et al. 2009

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“…Initial results from SWAP (and also the Pluto Energetic Particle Spectrometer Science Investigation instrument [McNutt et al, 2008]) were published in Bagenal et al [2016]. These included SWAP observations of the pristine solar wind before and after the flyby, which indicated that the solar wind was quite steady with approximate inferred proton moments [Elliott et al, 2016] at the time of the flyby of v p~4 03 km s À1 , n p~0 .025 cm…”

Section: Introductionmentioning

confidence: 99%

Pluto's interaction with the solar wind

et al. 2016

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This study provides the first observations of Plutogenic ions and their unique interaction with the solar wind. We find ~20% solar wind slowing that maps to a point only ~4.5 RP upstream of Pluto and a bow shock most likely produced by comet‐like mass loading. The Pluto obstacle is a region of dense heavy ions bounded by a “Plutopause” where the solar wind is largely excluded and which extends back >100 RP into a heavy ion tail. The upstream standoff distance is at only ~2.5 RP. The heavy ion tail contains considerable structure, may still be partially threaded by the interplanetary magnetic field (IMF), and is surrounded by a light ion sheath. The heavy ions (presumably CH4+) have average speed, density, and temperature of ~90 km s−1, ~0.009 cm−3, and ~7 × 105 K, with significant variability, slightly increasing speed/temperature with distance, and are N‐S asymmetric. Density and temperature are roughly anticorrelated yielding a pressure ~2 × 10−2 pPa, roughly in balance with the interstellar pickup ions at ~33 AU. We set an upper bound of <30 nT surface field at Pluto and argue that the obstacle is largely produced by atmospheric thermal pressure like Venus and Mars; we also show that the loss rate down the tail (~5 × 1023 s−1) is only ~1% of the expected total CH4 loss rate from Pluto. Finally, we observe a burst of heavy ions upstream from the bow shock as they are becoming picked up and tentatively identify an IMF outward sector at the time of the NH flyby.

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“…LENI utilizes a variation of the mirror‐free electron optics developed and flown successfully for the hockey puck style ion detectors (New Horizons PEPSSI [ McNutt et al ., ], Van Allen RBSPICE [ Mitchell et al ., ], Juno JEDI [ Mauk et al ., ], MMS‐EIS [ Mauk et al ., ]). This electron optical arrangement operates by placing a puller electrooptical element toward the MCP and a pusher element above as shown in the electron optical SIMION simulation in Figure .…”

Section: Techniquementioning

confidence: 99%

The Low‐Energy Neutral Imager (LENI)

et al. 2016

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To achieve breakthroughs in the areas of heliospheric and magnetospheric energetic neutral atom (ENA) imaging, a new class of instruments is required. We present a high angular resolution ENA imager concept aimed at the suprathermal plasma populations with energies between 0.5 and 20 keV. This instrument is intended for understanding the spatial and temporal structure of the heliospheric boundary recently revealed by Interstellar Boundary Explorer instrumentation and the Cassini Ion and Neutral Camera. The instrument is also well suited to characterize magnetospheric ENA emissions from low‐altitude ENA emissions produced by precipitation of magnetospheric ions into the terrestrial upper atmosphere, or from the magnetosheath where solar wind protons are neutralized by charge exchange, or from portions of the ring current region. We present a new technique utilizing ultrathin carbon foils, 2‐D collimation, and a novel electron optical design to produce high angular resolution (≤2°) and high‐sensitivity (≥10−3 cm2 sr/pixel) ENA imaging in the 0.5–20 keV energy range.

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The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons Mission

Cited by 52 publications

References 50 publications

Composition of energetic particles in the Jovian magnetotail

Composition of energetic particles in the Jovian magnetotail

Pluto's interaction with the solar wind

The Low‐Energy Neutral Imager (LENI)

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