Ralph: A Visible/Infrared Imager for the New Horizons Pluto/Kuiper Belt Mission

Reuter, Dennis C.; Stern, S. A.; Scherrer, J.; Jennings, Donald E.; Baer, James W.; Hanley, J.; Hardaway, Lisa; Lunsford, Allen; McMuldroch, Stuart; Moore, Jeffrey M.; Olkin, C. B.; Parizek, Robert; Reitsma, Harold; Sabatke, Derek; Spencer, J. R.; Stone, John Marshall; Throop, H. B.; Cleve, Jeffrey Van; Weigle, Gerald; Young, L. A.

doi:10.1007/978-0-387-89518-5_7

Cited by 38 publications

(55 citation statements)

References 7 publications

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“…Image data used in this study come from the LOng‐Range Reconnaissance Imager (LORRI) (Cheng et al, ) and Multi‐spectral Visible Imaging Camera (MVIC) (Reuter et al, ) aboard the New Horizons spacecraft (Fountain et al, ; Stern, ). We used individual images as well as basemaps produced from the LORRI and MVIC panchromatic images in this work (Schenk et al, ).…”

Section: Methodsmentioning

confidence: 99%

Investigation of Charon's Craters With Abrupt Terminus Ejecta, Comparisons With Other Icy Bodies, and Formation Implications

et al. 2018

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On the moon and other airless bodies, ballistically emplaced ejecta transitions from a thinning, continuous inner deposit to become discontinuous beyond approximately one crater radius from the crater rim and can further break into discrete rays and secondary craters. In contrast, on Mars, ejecta often form continuous, distinct, and sometimes thick deposits that transition to a low ridge or escarpment that may be circular or lobate. The Martian ejecta type has been variously termed pancake, rampart, lobate, or layered, and in this work we refer to it as “abrupt termini” ejecta (ATE). Two main formation mechanisms have been proposed, one requiring interaction of the ejecta with the atmosphere and the other mobilization of near‐surface volatiles. ATE morphologies are also unambiguously seen on Ganymede, Europa, Dione, and Tethys, but they are not as common as on Mars. We have identified up to 38 craters on Charon that show signs of ATE, including possible distal ramparts and lobate margins. These ejecta show morphologic and morphometric similarities with other moons in the solar system, which are a subset of the properties observed on Mars. From comparison of these ejecta on Charon and other solar system bodies, we find the strongest support for subsurface volatile mobilization and ejecta fluidization as the main formation mechanism for the ATE, at least on airless, icy worlds. This conclusion comes from the bodies on which they are found, an apparent preference for certain terrains, and the observation that craters with ATE can be near to similarly sized craters that only have gradational ejecta.

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Section: Methodsmentioning

confidence: 99%

Investigation of Charon's Craters With Abrupt Terminus Ejecta, Comparisons With Other Icy Bodies, and Formation Implications

et al. 2018

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“…Charon, Pluto’s large companion, has a variety of terrains that exhibit tectonic features. We present observations of them here from New Horizons’ Long-Range Reconnaissance Imager (LORRI, Cheng et al, 2008 ) and the Multi-spectral Visible Imaging Camera (MVIC) on the Ralph instrument ( Reuter et al, 2008 ). This work analyzes these observations and measures tectonic strike, estimates elastic thickness, compares these features to those seen on Pluto, and concludes that Charon has undergone global extension.…”

Section: Introductionmentioning

confidence: 99%

Charon tectonics

Beyer

Nimmo

McKinnon

et al. 2017

Icarus

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“…These images were reported to have been taken at UTs of 06:00, 06:26, and 06:41 and yielded a wave velocity of 220 to 250 m/s, 120+ m/s higher than the background clouds [ Reuter et al ., ]. The waves were visible in all the New Horizons Ralph/MVIC filters [ Reuter et al ., ] but were most apparent in the narrow methane absorption (889 nm) band, in part because that was the only filter not saturated away from the terminator. The waves were also visible in the high‐spatial resolution LORRI panchromatic channel [ Reuter et al ., ; Cheng et al ., ].…”

Section: Introductionmentioning

confidence: 99%

Small‐scale waves on Jupiter: A reanalysis of New Horizons, Voyager, and Galileo data

Simon-Miller

Reuter

2015

Geophysical Research Letters

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Jupiter's equator‐encircling mesoscale waves were a distinguishing feature observed during the New Horizons Jupiter flyby. Measured velocities indicated eastward propagation, inconsistent with standing wave models developed after the Voyager encounters. We present revised New Horizons mesoscale wave velocities of 164 to 176 m/s, approximately 90 m/s higher than the tropospheric zonal winds on that date, while Voyager and Galileo mesoscale waves do not show any apparent motion. This is consistent with an eastward propagating inertia‐gravity or Kelvin wave, or a wave propagating with the wind at certain altitudes, given proper vertical wind shears. New Horizons high solar phase angle methane band observations show wave crest shadows or aerosol clearing, implying altitudes above the cloud deck for the observed features. New Horizons and Voyager data also indicate that wave trains have lifetimes exceeding two Jovian rotations.

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Ralph: A Visible/Infrared Imager for the New Horizons Pluto/Kuiper Belt Mission

Cited by 38 publications

References 7 publications

Investigation of Charon's Craters With Abrupt Terminus Ejecta, Comparisons With Other Icy Bodies, and Formation Implications

Investigation of Charon's Craters With Abrupt Terminus Ejecta, Comparisons With Other Icy Bodies, and Formation Implications

Charon tectonics

Small‐scale waves on Jupiter: A reanalysis of New Horizons, Voyager, and Galileo data

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