000004667 001__ 4667
000004667 005__ 20200128114519.0
000004667 0247_ $$2DOI$$a10.1007/s11214-019-0613-y
000004667 037__ $$aSCART-2020-0037
000004667 100__ $$aGarcia, Raphael F. 
000004667 245__ $$aLunar Seismology: An Update on Interior Structure Models
000004667 260__ $$c2019
000004667 520__ $$aAn international team of researchers gathered, with the support of the International Space Science Institute (ISSI), (1) to review seismological investigations of the lunar interior from the Apollo-era and up until the present and (2) to re-assess our level of knowledge and uncertainty on the interior structure of the Moon. A companion paper (Nunn et al. in Space Sci. Rev., submitted) reviews and discusses the Apollo lunar seismic data with the aim of creating a new reference seismic data set for future use by the community. In this study, we first review information pertinent to the interior of the Moon that has become available since the Apollo lunar landings, particularly in the past ten years, from orbiting spacecraft, continuing measurements, modeling studies, and laboratory experiments. Following this, we discuss and compare a set of recent published models of the lunar interior, including a detailed review of attenuation and scattering properties of the Moon. Common features and discrepancies between models and moonquake locations provide a first estimate of the error bars on the various seismic parameters. Eventually, to assess the influence of model parameterisation and error propagation on inverted seismic velocity models, an inversion test is presented where three different parameterisations are considered. For this purpose, we employ the travel time data set gathered in our companion paper (Nunn et al. in Space Sci. Rev., submitted). The error bars of the inverted seismic velocity models demonstrate that the Apollo lunar seismic data mainly constrain the upper- and mid-mantle structure to a depth of ∼1200 km. While variable, there is some indication for an upper mantle low-velocity zone (depth range 100--250 km), which is compatible with a temperature gradient around 1.7 ∘C/km. This upper mantle thermal gradient could be related to the presence of the thermally anomalous region known as the Procellarum Kreep Terrane, which contains a large amount of heat producing elements.
000004667 594__ $$aNO
000004667 6531_ $$aMoon
000004667 6531_ $$aseismologie
000004667 6531_ $$ainterior structure
000004667 700__ $$aKhan, Amir 
000004667 700__ $$aDrilleau, Mélanie 
000004667 700__ $$aMargerin, Ludovic 
000004667 700__ $$aKawamura, Taichi 
000004667 700__ $$aSun, Daoyuan 
000004667 700__ $$aWieczorek, Mark A. 
000004667 700__ $$aRivoldini, Attilio 
000004667 700__ $$aNunn, Ceri 
000004667 700__ $$aWeber, Renee C. 
000004667 700__ $$aMarusiak, Angela G. 
000004667 700__ $$aLognonné, Philippe 
000004667 700__ $$aNakamura, Yosio 
000004667 700__ $$aZhu, Peimin
000004667 773__ $$n8$$pSpace Science Reviews$$v215$$y2019
000004667 8560_ $$fattilio.rivoldini@observatoire.be
000004667 8564_ $$s3028753$$uhttps://publi2-as.oma.be/record/4667/files/Garcia2019aa00.pdf
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000004667 905__ $$apublished in
000004667 980__ $$aREFERD