Duration and extent of lunar volcanism: Comparison of 3D convection models to mare basalt ages

Ziethe, R.; Seiferlin, K.; Hiesinger, H.

doi:10.1016/j.pss.2009.02.002

Cited by 95 publications

(92 citation statements)

References 61 publications

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“…Other numerical solutions include time dependence to model the thermal evolution of terrestrial planets (e.g., Steinbach and Yuen 1994;Konrad and Spohn 1997;Conzelmann 1999;Spohn et al 2001c;Buske 2006;Nakagawa and Tackley 2004;Xie and Tackley 2004;Butler et al 2005;Costin and Butler 2006;Ziethe et al 2009;Keller and Tackley 2009). These models require some modifications with respect to steady-state models in the parameters and the boundary conditions, in particular, if the core is to be included.…”

Section: Convection Regimesmentioning

confidence: 99%

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Breuer¹,

Labrosse²,

Spohn³

2010

Space Sci Rev

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Of the terrestrial planets, Earth and Mercury have self-sustained fields while Mars and Venus do not. Magnetic field data recorded at Ganymede have been interpreted as evidence of a self-generated magnetic field. The other icy Galilean satellites have magnetic fields induced in their subsurface oceans while Io and the Saturnian satellite Titan apparently are lacking magnetic fields of internal origin altogether.

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Section: Convection Regimesmentioning

confidence: 99%

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Breuer¹,

Labrosse²,

Spohn³

2010

Space Sci Rev

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“…This rubble has impact and ejecta origin, and 52 covers the outer few meters-kilometers of a planet (e.g., Warren and Rasmussen, 1987; 53 Ziethe et al, 2009). Because megaregolith has a thermal conductivity much lower than 54 that of equivalent solid rock, it insulates the hot interior and slows down cooling.…”

mentioning

confidence: 99%

Influence of an insulating megaregolith on heat flow and crustal temperature structure of Mercury

Egea-González¹,

Ruíz²

2014

Icarus

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27Mercury is covered by a megaregolith layer, which constitutes a poor thermally 28 conducting layer that must have an influence on the thermal state and evolution of the 29 planet, although most thermal modeling or heat flow studies have overlooked it. In this 30 work we have calculated surface heat flows and subsurface temperatures from the depth 31 of thrust faults associated with several prominent lobate scarps on Mercury, valid for 32 the time of the formation of these scarps, by solving the heat equation and taking into 33 account the insulating effects of a megaregolith layer. We conclude that megaregolith 34 insulation could have been an important factor limiting heat loss and therefore interior 35 cooling and contraction of Mercury. As Mercurian megaregolith properties are not very 36well known, we also analyze the influence of these properties on the results, and discuss 37 the consequences of imposing the condition that the total radioactive heat production 38 must be lower than the total surface heat loss (this is, the Urey ratio, Ur, must be lower 39 than 1) in a cooling and thermally contracting planet such as Mercury at the time of 40 scarp emplacement. Our results show that satisfying the condition of Ur < 1 implies that 41 the average abundances of heat-producing elements silicate layer is 0.4 times or less the 42 average surface value, placing an upper bound on the bulk content of heat producing 43 elements in Mercury's interior. 44 45

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“…If the history of lunar mare volcanism is indicative for heat-piping in Mercury's past, then its evolution should be closer to the models in which heat pipes are neglected. The moon's secondary crust is widespread, but thin-its primary crust prevails [e.g., Hikida and Wieczorek, 2007;Ziethe et al, 2009].…”

Section: Resultsmentioning

confidence: 99%

Thermal evolution of Mercury: Effects of volcanic heat‐piping

Multhaup¹

2009

Geophysical Research Letters

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[1] A 1D thermal evolution model of Mercury is presented. It accounts for stagnant lid convection, mantle differentiation and inner core growth. Early MESSENGER results indicate that-contrary to prior conclusions drawn from Mariner 10 imagery-volcanism has indeed played a significant role in Mercury's past. To study the effects of mantle heat bypassing the stagnant lid by means of volcanic heat-piping, contrasting end-member models are considered. Results show how break-down of mantle convection and onset of inner core growth are influenced by the mode of heat removal. Structural models of present day Mercury are presented. Their dependence on the core sulphur contents predominates that on the choice of mantle heat removal. However, the latter clearly controls the timing of thermal history events.

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Duration and extent of lunar volcanism: Comparison of 3D convection models to mare basalt ages

Cited by 95 publications

References 61 publications

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Thermal Evolution and Magnetic Field Generation in Terrestrial Planets and Satellites

Influence of an insulating megaregolith on heat flow and crustal temperature structure of Mercury

Thermal evolution of Mercury: Effects of volcanic heat‐piping

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