The Kaguya Mission Overview

Kato, Manabu; Sasaki, Susumu; Takizawa, Yukio

doi:10.1007/s11214-010-9678-3

Cited by 95 publications

(47 citation statements)

References 54 publications

(25 reference statements)

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“…Figure 3 shows the results of the simulation of the solar wind plasma impacting a localized crustal magnetic field structure. The insert is a photograph of the Reiner Gamma lunar swirl taken by the Kaguya (Kato et al 2010) spacecraft. This particular image is at an inclined angle similar to the simulation image's orientation to the representative plane of the "lunar surface," allowing a comparison of the footprint deposition of protons (red) in the simulation and the "white" of the lunar swirl.…”

Section: The Simulationsmentioning

confidence: 99%

“…A 3D magnetized plasma collision with a surface magnetic dipole. Insert: a low-altitude, inclined angle photograph taken by the JAXA Kaguya (Kato et al 2010) spacecraft of the Reiner Gamma Formation (https://the-moon.wikispaces.com/Reiner+Gamma) as an example of a lunar swirl albedo anomaly located coincident with a localized crustal magnetic field. The solar wind plasma (flowing vertically downward) impacts a localized crustal magnetic field structure (blue lines).…”

Section: The Simulationsmentioning

confidence: 99%

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3d Pic Simulations of Collisionless Shocks at Lunar Magnetic Anomalies and Their Role in Forming Lunar Swirls

Bamford

Alves

Cruz

et al. 2016

ApJ

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Investigation of the lunar crustal magnetic anomalies offers a comprehensive long-term data set of observations of small-scale magnetic fields and their interaction with the solar wind. In this paper a review of the observations of lunar mini-magnetospheres is compared quantifiably with theoretical kinetic-scale plasma physics and 3D particlein-cell simulations. The aim of this paper is to provide a complete picture of all the aspects of the phenomena and to show how the observations from all the different and international missions interrelate. The analysis shows that the simulations are consistent with the formation of miniature (smaller than the ion Larmor orbit) collisionless shocks and miniature magnetospheric cavities, which has not been demonstrated previously. The simulations reproduce the finesse and form of the differential proton patterns that are believed to be responsible for the creation of both the "lunar swirls" and "dark lanes." Using a mature plasma physics code like OSIRIS allows us, for the first time, to make a side-by-side comparison between model and space observations. This is shown for all of the key plasma parameters observed to date by spacecraft, including the spectral imaging data of the lunar swirls. The analysis of miniature magnetic structures offers insight into multi-scale mechanisms and kinetic-scale aspects of planetary magnetospheres.

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Section: The Simulationsmentioning

confidence: 99%

Section: The Simulationsmentioning

confidence: 99%

3d Pic Simulations of Collisionless Shocks at Lunar Magnetic Anomalies and Their Role in Forming Lunar Swirls

Bamford

Alves

Cruz

et al. 2016

ApJ

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“…Evidence by in-situ measurements from space craft including Lunar Prospector (1998-1999) [6], Kaguya (2007Kaguya ( -2009 [7], Chandrayaan-1 (2008-2009) [8] and Nozomi (1998) spacecraft [9], are consistent with the presence of collisionless shocks and the formation of minimagnetospheres. Because the observational data derives from a sequence of case studies from different missions [1,[10][11][12][13][14][15][16], it is to be expected that there is some variation in consistency.…”

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confidence: 95%

Minimagnetospheres above the Lunar Surface and the Formation of Lunar Swirls

et al. 2012

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In this paper we present in-situ satellite data, theory and laboratory validation that show how small scale collisionless shocks and mini-magnetospheres can form on the electron inertial scale length. The resulting retardation and deflection of the solar wind ions could be responsible for the unusual "lunar swirl" patterns seen on the surface of the Moon.Miniature magnetospheres have been found to exist above the lunar surface [1] and are closely related to features known as "lunar swirls" [2]. Mini-magnetospheres exhibit features that are characteristic of normal planetary magnetospheres namely a collisionless shock. Here we show that it is the electric field associated with the small scale collisionless shock that is responsible for deflecting the incoming solar wind around the minimagnetosphere. These ions impacting the lunar surface resulting in changes to the appearance of the albedo of the lunar "soil" [2]. The form of these swirl patterns therefore, must be dictated by the shapes of the collisionless shock.Collisionless shocks are a classic phenomena in plasma physics, ubiquitous in many space and astrophysical scenarios [3]. Well known examples of collisionless shocks exist in the heliosphere, where the shock is formed by the solar wind interacting with a magnetised planet. What is a surprise is the size of the mini-magnetospheres, of the order of several 100 km; orders of magnitude smaller than the planetary versions. Results from various lunar survey missions have built up a good picture of these collisionless shocks.These collisionless shocks have a characteristic structure in which the ions are reflected from a rather narrow layer, of the order of the electron skin depth c/ω pe (where c is the speed of light and ω pe is the electron plasma frequency), by an electrostatic field that is a consequence of the magnetised electrons and unmagnetised ions. The narrow discontinuity in the shock structure produces a specular reflected ion component with a velocity equal to or greater than the incoming solar wind velocity. The reflected ions from a counter-propagating component to the solar wind flow that form the magnetic foot region, which extends about an ion Larmor orbit upstream from the shock. This occurs when the Mach number (the ratio of flow velocity to Alfvén velocity) is of the order 3 or less.We have carried out laboratory experiments using a plasma wind tunnel, to investigate mini-magnetospheres

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“…We mainly used the images and spectral data taken by the Terrain Camera (TC) and Multiband Imager (MI) onboard the SELENE spacecraft Kato et al 2010;Ohtake et al 2008). They uniformly cover the entire lunar surface.…”

Section: Datamentioning

confidence: 99%

Tectonic evolution of northwestern Imbrium of the Moon that lasted in the Copernican Period

et al. 2016

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The formation ages of tectonic structures and their spatial distributions were studied in the northwestern Imbrium and Sinus Iridum regions using images obtained by Terrain Camera and Multiband Imager on board the SELENE spacecraft and the images obtained by Narrow Angle Camera on board LRO. The formation ages of mare ridges are constrained by the depositional ages of mare basalts, which are either deformed or dammed by the ridges. For this purpose, we defined stratigraphic units and determined their depositional ages by crater counting. The degradation levels of craters dislocated by tectonic structures were also used to determine the youngest limits of the ages of the tectonic activities. As a result, it was found that the contractions to form mare ridges lasted long after the deposition of the majority of the mare basalts. There are mare ridges that were tectonically active even in the Copernican Period. Those young structures are inconsistent with the mascon tectonics hypothesis, which attributes tectonic deformations to the subsidence of voluminous basaltic fills. The global cooling or the cooling of the Procellarum KREEP Terrane region seems to be responsible for them. In addition, we found a graben that was active after the Eratosthenian Period. It suggests that the global or regional cooling has a stress level low enough to allow the local extensional tectonics.

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The Kaguya Mission Overview

Abstract: The Japanese lunar orbiter Kaguya (SELENE) was successfully launched by an H2A rocket on

Cited by 95 publications

References 54 publications

3d Pic Simulations of Collisionless Shocks at Lunar Magnetic Anomalies and Their Role in Forming Lunar Swirls

3d Pic Simulations of Collisionless Shocks at Lunar Magnetic Anomalies and Their Role in Forming Lunar Swirls

Minimagnetospheres above the Lunar Surface and the Formation of Lunar Swirls

Tectonic evolution of northwestern Imbrium of the Moon that lasted in the Copernican Period

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