Crustal structure of Mars from gravity and topography

By G. Neumann, Maria T. Zuber, Mark A. Wieczorek, P. McGovern, F. LeMoine, D. E. Smith. 2004

379 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/57929a9fc032705edfaa6cdb6b87e4896f2d9772

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In Astronomy and Astrophysics

Citations in the corpus

Ages of very large impact basins on Mars: Implications for the late heavy bombardment in the inner solar system (2008, background): “Edgar and Frey [2008] showed that crustal thickness data [Neumann et al., 2004] reveal a large population of ‘‘Circular Thin Areas’’ (CTAs): thin crust surrounded by rings of thicker crust.”
Hydrovolcanic tuff rings and cones as indicators for phreatomagmatic explosive eruptions on Mars (2013, background): “It has also been speculated [cf. Zuber et al., 2000] that thick accumulations of volcanic material could explain the positive Bouguer anomalies along this part of the dichotomy boundary [Neumann et al., 2004].”
Sequence and timing of conditions on early Mars (2011, background): “…these two views can be reconciled in a scenario where the majority of the crust at Tharsis is constructed in the Noachian (crustal thickness 50–100 km; Neumann et al., 2004), but where extensive volcanic resurfacing persists through Hesperian and Amazonian times (see also Solomon and Head, 1982).”
Geologic history of Mars (2010, background): “The thickness of the crust is estimated to average 30 km north of the dichotomy boundary and approximately 60 km to the south (Neumann et al., 2004).”
Constraints on the Martian lithosphere from gravity and topography data and implication for volcanism and possible mantle heterogeneities (2005, background): “An estimate for the density of the southern highlands crust is lower [Neumann et al., 2004], and this seems to indicate that the northern hemisphere crust is more mafic in composition than the southern highlands.”
Rapid decrease in Martian crustal magnetization in the Noachian era: Implications for the dynamo and climate of early Mars (2008, background): “More recently, crustal thickness maps derived from gravity and topography [Neumann et al., 2004] have been used to identify circular thin-crust areas (CTAs) as possible additional buried impact structures >300 km in diameter.”
EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, background): “A smaller mean thickness would result in negative values beneath the large impact basins; Wieczorek & Zuber (2004) and Neumann et al. (2004) used this argument to find a lower bound on the mean crustal thickness of 32 and 45 km, respectively.”
Correction to “Localized gravity/topography admittance and correlation spectra on Mars: Implications for regional and global evolution” (2004, result): “The new density estimates more closely match the densities of Martian basaltic meteorites [e.g., Neumann et al., 2004] and agree with other recent estimates of densities for Martian volcanoes [Belleguic et al., 2004; Neumann et al., 2004 ].”
Large impact crater histories of Mars: The effect of different model crater age techniques (2013, background): “Given that Ladon and Prometheus are similarly sized basins with a similar topographic expression and crustal thickness (Neumann et al., 2004 ), it is reasonable to suggest that the stark difference in their magnetic field strengths is reflective of very different global magnetic environments…”
Possible formation of ancient crust on Mars through magma ocean processes (2005, background): “These estimates are roughly double the geophysical estimates of the current Martian crust of about 50 km [Neumann et al., 2004], but these estimates are probably maximum values.”
Heterogeneous distribution of H2O in the Martian interior: Implications for the abundance of H2O in depleted and enriched mantle sources (2016, methodology): “In order to compute the estimates, we use (1) a crustal thickness estimate of 57 km (Wieczorek and Zuber 2004), (2) a core radius of 1680 km (Taylor 2013), (3) an average crustal density of 2900 kg m 3 (Neumann et al. 2004), and an average mantle density of 3400 kg m 3 (Bertka and Fei 1997).”
Degree-1 convection in the Martian mantle and the origin of the hemispheric dichotomy (2006, background): “[3] MOLA gravity and topography data constrain the average crustal thickness to be 45 km, and 32 km and 58 km for northern lowlands and southern highlands, respectively [Zuber et al., 2000; Neumann et al., 2004; Wieczorek and Zuber, 2004].”
Mars high resolution gravity fields from MRO, Mars seasonal gravity, and other dynamical parameters (2011, background): “Turcotte et al. (2002) estimates crustal thickness of 92 ± 5 km, Konopliv et al. (2006) find the mean thickness of 72 ± 18 km while Neumann et al. (2004) estimate it to be 45 ± 5 km. Incidently, Khan and Connolly (2008) find that the preferred core size is about 1680 km (core density of 6.7 gm and…”