W. R. Pryor

Central Arizona College

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G. R. Gladstone

Southwest Research Institute

K. D. Retherford

Southwest Research Institute

Denis Grodent

University of Liège

T. K. Greathouse

Southwest Research Institute

Jean‐Claude Gérard

University of Liège

S. A. Stern

Southwest Research Institute

D. M. Hurley

Johns Hopkins University Applied Physics Laboratory

P. D. Feldman

University of Baltimore

Jacques Gustin

University of Liège

Aikaterini Radioti

University of Liège

Cooperative Institutions

Southwest Research Institute

100

Jet Propulsion Laboratory

University of Colorado Boulder

Laboratory for Atmospheric and Space Physics

Johns Hopkins University Applied Physics Laboratory

Planetary Science Institute

California Institute of Technology

Goddard Space Flight Center

University of Arizona

Centre National de la Recherche Scientifique

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LRO-LAMP Observations of the LCROSS Impact Plume

Science (2010)

G. R. Gladstone D. M. Hurley K. D. Retherford P. D. Feldman W. R. Pryor

On 9 October 2009, the Lunar Crater Observation and Sensing Satellite (LCROSS) sent a kinetic impactor to strike Cabeus crater, on a mission to search for water ice and other volatiles expected to be trapped in lunar polar soils. The Lyman Alpha Mapping Project (LAMP) ultraviolet spectrograph onboard the Lunar Reconnaissance Orbiter (LRO) observed the plume generated by the LCROSS impact as far-ultraviolet emissions from the fluorescence of sunlight by molecular hydrogen and carbon monoxide, plus resonantly scattered sunlight from atomic mercury, with contributions from calcium and magnesium. The observed light curve is well simulated by the expansion of a vapor cloud at a temperature of ~1000 kelvin, containing ~570 kilograms (kg) of carbon monoxide, ~140 kg of molecular hydrogen, ~160 kg of calcium, ~120 kg of mercury, and ~40 kg of magnesium.

Mercury

Orbiter

Sunlight

Ultraviolet

10.1126/science.1186474

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Citations (160)

Models of CO 4th Positive Band Emissions on Venus

AAS/Division for Planetary Sciences Meeting Abstracts #25 (1993)

W. R. Pryor W. E. McClintock A. I. F. Stewart C. W. Hord C. A. Barth

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Saturn's Auroras from the Cassini Ultraviolet Imaging Spectrograph

AGU Spring Meeting Abstracts (2005)

W. R. Pryor R. A. West Iain A. Stewart D. E. Shemansky J. M. Ajello

Ultraviolet

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Auroral signatures of reconnection at Saturn: comparison with Earth

EPSC (2013)

Aikaterini Radioti Denis Grodent Jean‐Claude Gérard Bertrand Bonfond Jacques Gustin

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LRO Lamp: In-flight Performance, LCROSS Support, and Future Science

AAS/Division for Planetary Sciences Meeting Abstracts #41 (2009)

G. R. Gladstone S. A. Stern K. D. Retherford J. W. Parker D. C. Slater

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Cassini UVIS Auroral Observations in 2016

W. R. Pryor A. Jouchoux L. W. Esposito Aikaterini Radioti Denis Grodent

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Lunar swirls: Far-UV characteristics

Icarus (2016)

Amanda Hendrix T. K. Greathouse K. D. Retherford K. E. Mandt G. R. Gladstone

10.1016/j.icarus.2016.01.003

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Signatures of magnetospheric injections in Saturn's aurora

Journal of Geophysical Research Space Physics (2013)

Aikaterini Radioti E. Roussos Denis Grodent Jean‐Claude Gérard N. Krupp

We report on the evolution of auroral structures based on two 3 h sequences of Saturn's northern hemisphere obtained with the UVIS instrument on board Cassini, and we discuss their possible association with injections in the magnetosphere of Saturn. Simultaneously with the UV auroral structures, we observe Energetic Neutral Atom (ENA) enhancements which are indicative of a rotating heated plasma region possibly related to magnetospheric injections. We examine the possibility that the UV auroral structures reported here are triggered by energetic particle injections by investigating (a) the evolution of the longitudinal extent of an injection and (b) its energy density, properties that change with time due to dispersion and ion/electron losses. We simulate the auroral counterpart of an injection considering that the precipitating energy flux could be provided to the ionosphere by pitch angle diffusion and electron scattering by whistler‐mode waves. We compare the brightness and size evolution of the simulated ionospheric signature with the observed values, and we demonstrate that the UV auroral structure behaves as an auroral signature of an injection. This comparative study defines characteristics of the injections such as the spectral index and the electron energy range as well as the magnetospheric corotation rate. Additionally, based on the simultaneous ENA‐UV emissions, we discuss the possibility that pitch angle diffusion and electron scattering may not be the only mechanism responsible for the observed auroral emissions. Field‐aligned currents driven by the pressure gradients along the boundaries of the injected hot plasma cloud could be also considered to play a role on how injections create auroral emissions at Saturn.

Pitch angle

Electron precipitation

Plasmoid

10.1002/jgra.50161

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Advances on the magnetospheric dynamics of Saturn revealed from UVIS/Cassini auroral observations during the Grand finale phase of the mission

Aikaterini Radioti Denis Grodent Zhonghua Yao Jean‐Claude Gérard S. V. Badman

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Saturn's aurora seen by HST and UVIS

Denis Grodent Aikaterini Radioti Bertrand Bonfond Jacques Gustin Jean‐Claude Gérard

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