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The Search for Electrostatically Lofted Grains Above Themoon with The Geophysical Research Letters RESEARCH LETTER The search for electrostatically lofted grains above the Moon 10.1002/2015GL064324 with the Lunar Dust Experiment Key Points: 1,2,3 1,2,3 • The first in situ search for lofted lunar Jamey R. Szalay and Mihály Horányi terminator dust was performed 1 2 • The first in situ upper bound for this Department of Physics, University of Colorado Boulder, Boulder, Colorado, USA, Laboratory for Atmospheric and Space population is estimated as 100 m−3 Physics, University of Colorado Boulder, Boulder, Colorado, USA, 3Institute for Modeling Plasma, Atmospheres, and Cosmic • Without a height dependence, no Dust, University of Colorado Boulder, Boulder, Colorado, USA evidence for this putative population was found Abstract The Lunar Dust Experiment (LDEX) on board the Lunar Atmosphere and Dust Environment Correspondence to: Explorer mission was designed to make in situ dust measurements while orbiting the Moon. Particles with J. R. Szalay, radii a >∼0.3 μm were detected as single impacts. LDEX was also capable of measuring the collective signal [email protected] generated from dust impacts with sizes below its single-particle detection threshold. A putative population of electrostatically lofted grains above the lunar terminator with radii of approximately 0.1 μm has been Citation: suggested to exist since the Apollo era. LDEX performed the first search with an in situ dust detector for Szalay, J. R., and M. Horányi (2015), The search for electrostatically lofted such a population. Here we present the results of the LDEX observations taken over the lunar terminator grains above the Moon with the Lunar and report that within LDEX’s detection limits, we found no evidence of electrostatically lofted grains in the Dust Experiment, Geophys. Res. Lett., altitude range of 3–250 km above the lunar terminator. 42, doi:10.1002/2015GL064324. Received 22 APR 2015 1. Introduction Accepted 18 JUN 2015 Accepted article online 22 JUN 2015 Electrostatic dust mobilization on the lunar surface has remained a controversial topic since the Apollo era. In situ [Rennilson and Criswell, 1974; Severnyetal., 1975; Berg, 1978; Grün and Horányi, 2013] as well as remote sensing observations [McCoy, 1976; Glenar et al., 2011, 2014; Feldman et al., 2014] have potentially indicated the lofting of charged dust particles near the lunar terminators. For example, in images taken just after sunset by the Surveyors 5, 6, and 7 cameras, a horizon glow was observed due west [Rennilson and Criswell, 1974; Colwell et al., 2007]. This glow has been interpreted as forward scattered light from a cloud of dust particles levitating less than 1 m above the surface with particle radii on the order of 5 μm[Rennilson and Criswell, 1974]. However, as of yet, no mechanism capable of generating sufficiently large electric fields to levitate such heavy particles has been identified. The Lunar Ejecta and Meteorite (LEAM) experiment was deployed by Apollo 17 astronauts to monitor the interplanetary and interstellar dust flux and the secondary particles created due to their impacts [Berg, 1978]. This instrument registered a multitude of unexpected hits during lunar sunrise and sunset, possibly caused by slow moving and highly charged dust grains transported across the lunar surface [Bergetal., 1976; Grün and Horányi, 2013]. High-altitude observations also indicated the existence of lofted dust at tens of kilometers above the surface. The first high-altitude, remote-sensing optical observations were made during the Apollo 15–17 missions, which took a series of calibrated images to analyze the zodiacal light and the solar corona. Some of these images indicated an excess brightness that has been interpreted as forward scattered light from small grains with characteristic radii a ≃ 0.1 μm lofted over the terminator regions of the Moon. The density of such a dust population was first calculated to be on the order of 104 m−3 near the surface using Apollo data [McCoy, 1976; Glenar et al., 2011]. Recent remote sensing surveys by Clementine [Glenar et al., 2014] and Lyman-Alpha Mapping Project aboard the Lunar Reconnaissance Orbiter (LRO/LAMP) [Feldman et al., 2014] have signifi- cantly lowered the upper limit of the lofted dust density to ∼1m−3 near the surface. The LDEX instrument was designed to characterize the lunar dust environment, and it did discover a permanently present, asymmetric ejecta cloud engulfing the Moon, sustained by the continual bombardment of its surface by interplanetary micrometeoroids of cometary and asteroidal origin [Horányi et al., 2015]. Here we report on the LDEX obser- vations that were dedicated to identifying a population of small lofted dust particles. To maintain consistency and allow direct comparison with the previous literature, in the analysis of the LDEX measurements below we assume the putative population of small grains has a characteristic radius of a = 0.1 μm. We start with a brief ©2015. American Geophysical Union. summary of the LDEX instrument (section 2), followed by the description of the observations (section 3), and All Rights Reserved. our conclusions (section 4). SZALAY AND HORÁNYI TERMINATOR DUST 1 Geophysical Research Letters 10.1002/2015GL064324 Table 1. Current Definitions Current Definition JN Nominal current, taken 9 of every 10 s JS Switched current, taken 1 of every 10 s JD Dust current, desired science quantity J Photoelectron current JH High-energy ion current JL Low-energy ion current J Residual, low-energy current 2. Instrument Description NASA’s Lunar Atmosphere and Dust Environment Explorer (LADEE) mission was launched on 7 September 2013 (UTC) and reached lunar orbit a month later on 6 October 2013. Lunar Dust Experiment (LDEX) is an impact ionization dust detector designed to map the variability of the dust size and density distributions near the Moon [Horányi et al., 2014]. When dust particles with speeds greater than ≃ 1 km/s impact LDEX’s hemispherical target, they generate a plasma cloud. The electrons and negative ions are collected on the hemispherical target, and the positive ions are accelerated into a microchannel plate (MCP) ion detector. The impact ionization plasma charge (in number of electrons) produced by a dust grain (with mass m in kg) impact- . 17 . ing LDEX is determined by the calibration of the instrument qe− = Cmv , where C = 6 24 × 10 , = 4 76, and the characteristic orbital speed of LADEE v = 1.7 km/s. LDEX can individually detect impacts that gen- erate greater than approximately 3000 electrons, corresponding to a grain radius of a ≃ 0.3 μm. For a 0.1 μm 3 −3 radius grain with a density of d ≃ 3 × 10 kg/m [Lindsay, 1976], the expected impact charge is qe− ≃ 100 el [Dietzel et al., 1973; Horányi et al., 2014]. Since this impact plasma charge is below LDEX’s individual detection limit, a novel method is used to search for the putative population of such small grains. To enable the identification of regions with a high-number density of particles that are too small for individ- ual impact detection, the charge collected through the MCP is continuously integrated for periods of 0.1 s. A bias potential is set up between the hemispherical target and the MCP where the ions are collected. Charges are continuously collected alternating between two bias voltage settings with a cadence of 10 s. Every 9 out of 10 s, the bias voltage is set to −200 V, accelerating virtually all positive ions into the MCP, and a “nominal” current JN is collected. For the last second of every 10, the “switched" current, JS, is obtained by switching the polarity of the bias voltage to +30 V, blocking positive ions with energies less than approximately 30 eV from reaching the MCP. Since impact plasmas from dust impacts are low energy (≃ 1 eV), LDEX becomes blind to dust during these periods. This switched current gives a measure of the background contributions of photoelectrons, generated by UV photons reaching the MCP itself, and the high-energy ions of solar wind ori- gin entering LDEX, as neither of these will vary between the switched and unswitched (or nominal) periods. Hence, the difference between these two signals taken every 10 s yields the residual, low-energy ion current, J = JN − JS. The residual, low-energy ions in this current that LDEX measures come either from dust impacts, JD, the desired quantity, or from low-energy ions entering LDEX, JL. Furthermore, the small current that LDEX measured can come from a variety of sources, including (a) back-scattered solar wind protons with initial typ- ical energies of > 100 eV [Saito et al., 2008] loosing energy inside LDEX by multiple scattering, (b) sputtering the LDEX target by energetic neutral atoms [Saul et al., 2013; Allegrini et al., 2013], and (c) the lunar iono- sphere [Poppe et al., 2014]. See Horányi et al. [2014] for a more in-depth discussion of the instrument operating schemes. These currents, defined in Table 1, are summarized below: JN = JD + J + JH + JL JS = J + JH J = JN − JS = JD + JL “Current” for the remainder of this paper will refer to the residual, low-energy current, J. All impact plasma charges due to a flux of small grains to LDEX will be captured in this current if they exist. Hence, the current can be used to search for the putative population of grains with a ≃ 0.1 μm lofted over the sunrise terminator regions by and will be the focus for the remainder of this discussion. Additionally, SZALAY AND HORÁNYI TERMINATOR DUST 2 Geophysical Research Letters 10.1002/2015GL064324 unless otherwise stated, “terminator” will refer to the lunar sunrise terminator at 6:00 local time (LT). This terminator is the boundary on the lunar sur- face between sunlit and shadowed terrain assuming a smooth surface, hence ignoring the complexity of this boundary due to the topogra- phy.
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