Radar altimetry of Mercury: A Preliminary analysis

Harmon, J. K.; Campbell, D. B.; Bindschadler, D. L.; Head, J. W.; Shapiro, I. I.

doi:10.1029/jb091ib01p00385

Cited by 50 publications

(44 citation statements)

References 32 publications

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“…Topographic data obtained from Earth-based radar show that the smooth plains of northern Tir Planitia are located within a broad, approximately north-south-trending trough lying as much as 1 km below the adjacent intercrater plains (Harmon et al, 1986;Harmon and Campbell, 1988;Watters and Nimmo, in press). Wrinkle ridges on other terrestrial planets are often seen on volcanic plains units within topographic lows (e.g., Hesperia Planum, Mars) (Watters, 1993;Head et al, 2008).…”

Section: Basin-exterior Wrinkle Ridgesmentioning

confidence: 99%

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Watters

Murchie

Robinson

et al. 2009

Earth and Planetary Science Letters

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Section: Basin-exterior Wrinkle Ridgesmentioning

confidence: 99%

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Watters

Murchie

Robinson

et al. 2009

Earth and Planetary Science Letters

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“…Topographic profiles across these three scarps have been derived by applying the delay-Doppler method to the data obtained from the Arecibo antenna in the period 1978-1984(Harmon et al, 1986.…”

Section: Topographic Profilesmentioning

confidence: 99%

“…In this work we use a forward modeling procedure in order to analyze fault geometries and depths associated with a group of prominent lobate scarps located in the Kuiper region of Mercury for which Earth-base radar topographic profiles are available (Harmon et al, 1986): Santa Maria Rupes and two unnamed lobate scarps referred to as S_K3 and S_K4 scarps. Calculations of surface heat flow have been performed from the BOT depth beneath these lobate scarps (and beneath Discovery Rupes for comparison) by assuming heat sources homogeneously distributed in the crust.…”

Section: Introductionmentioning

confidence: 99%

Depth of faulting and ancient heat flows in the Kuiper region of Mercury from lobate scarp topography

Egea-González

Ruíz

Fernández

et al. 2012

Planetary and Space Science

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“…Earth-based radar observations from Arecibo and Goldstone have provided information on surface scattering properties, equatorial topography, deposits in permanently shadowed crater interiors, and preliminary information about the morphology and morphometry of portions of Mercury not observed by Mariner 10 (e.g., Harmon and Campbell 1988;Clark et al 1988;Harmon and Slade 1992;Anderson et al 1996;Harmon et al 1986, an 85-km-diameter crater whose radar ray system may be the most well-developed in the solar system (SC, same as transmitted sense polarization; i.e., same component transmitted and received). (b) Feature "B," a 95-km-diameter impact crater with a very bright halo but less distinct ray system.…”

Section: Radar Observationsmentioning

confidence: 99%

“…Quantitative data on equatorial topography have been very useful for the analysis of equatorial radius (∼2,439.7 km) and shape, the range of altitudes (∼7 km, from −2.4 to +4.6 km), and definition of the zero-altitude datum (+0.3 km), the most probable altitude as shown in the peak of the equatorial altimetric histogram (Harmon et al 1986). Radar altimetry provided high-resolution topographic profiles for major features on Mercury (Harmon et al 1986) showing a systematic difference in the depths of large craters between Mercury (shallower) and the Moon, and systematic differences between shadow measurements and radar measurements (17% lower) for large crater depths on Mercury. Other profiles documented the steep topography associated with major lobate fault systems (a 3 km drop in 70 km) and the rounded topography associated with arcuate scarps.…”

Section: Radar Observationsmentioning

confidence: 99%

The Geology of Mercury: The View Prior to the MESSENGER Mission

Head¹,

Chapman²,

Domingue³

et al. 2007

The Messenger Mission to Mercury

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Mariner 10 and Earth-based observations have revealed Mercury, the innermost of the terrestrial planetary bodies, to be an exciting laboratory for the study of Solar System geological processes. Mercury is characterized by a lunar-like surface, a global magnetic field, and an interior dominated by an iron core having a radius at least three-quarters of the radius of the planet. The 45% of the surface imaged by Mariner 10 reveals some distinctive differences from the Moon, however, with major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. Our current image coverage of Mercury is comparable to that of telescopic photographs of the Earth's Moon prior to the launch of Sputnik in 1957. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor (∼1 km), and as with many lunar telescopic photographs, much of the available surface of Mercury is distorted by foreshortening due to viewing geometry, or poorly suited for geological analysis and impact-crater counting for age determinations because of high-Sun illumination conditions. Currently available topographic information is also very limited. Nonetheless, Mercury is a geological laboratory that represents (1) a planet where the presence of a huge iron core may be due to impact stripping of the crust and upper mantle, or alternatively, where formation of a huge core may have resulted in a residual mantle and crust of potentially unusual composition and structure; (2) a planet with an internal chemical and mechanical structure that provides new insights into planetary thermal history and the relative roles of conduction and convection in planetary heat loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the global tectonic system; (4) a planet where volcanic resurfacing may not have played a significant role in planetary history and internally generated volcanic resurfacing may have ceased at ∼3.8 Ga; (5) a planet where impact craters can be used to disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry; (6) an environment where global impact crater counts can test fundamental concepts of the distribution of impactor populations in space and time; (7) an extreme environment in which highly radar-reflective polar deposits, much more extensive than those on the Moon, can be better understood; (8) an extreme environment in which the basic processes of space weathering can be further deduced; and (9) a potential end-member in terrestrial planetary body geological evolution in which the relationships of internal and surface evolution can be clearly assessed from both a tectonic and volcanic point of view. In the half-century since the launch of Sputnik, more than 30 spacecraft have been sent to the Moon, yet only now is a second spacecraft en route to Mercury. The MESSENGER mission will address key questions ...

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Radar altimetry of Mercury: A Preliminary analysis

Abstract: Measurements of Mercurian topography based on

Cited by 50 publications

References 32 publications

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Emplacement and tectonic deformation of smooth plains in the Caloris basin, Mercury

Depth of faulting and ancient heat flows in the Kuiper region of Mercury from lobate scarp topography

The Geology of Mercury: The View Prior to the MESSENGER Mission

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