Localized gravity/topography admittance and correlation spectra on Mars: Implications for regional and global evolution

By P. McGovern, Sean C. Solomon, David E. Smith, Maria T. Zuber, Mark Simons, Mark A. Wieczorek, Roger J. Phillips, G. Neumann, Oded Aharonson, James W. Head III. 2002

337 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ad45a6cdecc076c45f58872b2836631ae75b69c6

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In Astronomy and Astrophysics

Citations in the corpus

Experimental petrology of the basaltic shergottite Yamato‐980459: Implications for the thermal structure of the Martian mantle (2006, result): “This produced a heat flux out of the mantle that is consistent with the mantle heat flux estimated by McGovern et al. (2002, 2004) on the basis of gravity modeling of the large volcanoes in Tharsis and Elysium.”
Conditions for the onset of plate tectonics on terrestrial planets and moons (2007, neutral): “Earth 2890 9.81 2.73E+08 1.000 40+/−20 (Schubert et al., 2001; Watts and Burov, 2003) Moon 1340 1.62 9.66E+05 0.164 100+/−50 (Konopliv et al., 1998; Aoshima and Namiki, 2001) Mars 1698 3.7278 7.26E+06 0.254 80+80/−60 (Folkner et al., 1997; McGovern et al., 2002 ) Io 835 1.80 – 0.151 20+/− 5( Segatz”
Mars high resolution gravity fields from MRO, Mars seasonal gravity, and other dynamical parameters (2011, background): “These admittance spectral amplitude and shape are very similar to those found by McGovern et al. (2002, 2004) and especially Belleguic et al. (2005), but now extend to degree and order of 87 (the local degree strength value, 122 km) from less than 60 previously.”
The composition of Mars (2019, background): “ically symmetric body divided into three layers (crust, mantle and core). The average crustal thickness of 50 km, which is consistent with geophysical and geochemical constraints (Zuber et al., 2000; McGovern et al., 2002, 2004; Wieczorek and Zuber, 2004; Ruiz et al., 2009), is adopted in the modeli”
Geologic history of Mars (2010, background): “Admittance data suggests that the densely cratered terrain of the southern highlands has surface densities of 2500–3000 kg m−3 (McGovern et al., 2002), significantly lower than the density of the”
Spatiospectral Concentration on a Sphere (2004, neutral): “This is really the essence of the spatiospectral concentration problem: the number of degrees of freedom is reduced from dim S L = ( L + 1) 2 to the Shannon number N = ( L + 1) 2 A/ (4 π ).”
EARLY CRUSTAL EVOLUTION OF MARS 1 (2005, methodology): “McGovern et al. (2002) obtained values of 50(+12, −42 km) for Noachis Terra, and Nimmo (2002) found a mean crustal thickness of <75 km in the area investigated.”
Thickness of the Martian crust: Improved constraints from geoid-to-topography ratios (2004, methodology): “[14] McGovern et al. [2002] has employed the former technique using the localization method of Simons et al. E01009 WIECZOREK AND ZUBER: THICKNESS OF THE MARTIAN CRUST”
Constraints on the Martian lithosphere from gravity and topography data and implication for volcanism and possible mantle heterogeneities (2005, methodology): “This is considerably larger than previously published values of about 2900 kg m−3 [McGovern et al., 2002; McKenzie et al., 2002], but is consistent with the corrected values of McGovern et al. [2004] (see Table 3 for a comparison).”
Constraints on the composition and petrogenesis of the Martian crust (2003, methodology): “[24] Using MGS MOLA data, new models of the relationship between gravity and topography [Turcotte et al., 2002] and admittance techniques [McGovern et al., 2002; McKenzie et al., 2002] suggest densities of 2.95–3.15 g/cm3 for parts of the elastic lithosphere of Mars.”
Crustal structure of Mars from gravity and topography (2004, background): “High topographic resolution and inadequate sampling of gravitational power at medium wavelengths can result in spurious features in the crustal thickness model [ Smith and Zuber , 2002].”
Have olivine, will gas: Serpentinization and the abiogenic production of methane on Mars (2005, background): “This is illustrated in Figure 1 where four potential geotherms (5, 10, 15 and 20 K km � 1 ) for the upper 50 km of crust are shown [ McGovern et al., 2002 ].”