Crater-Centered Laccoliths on the Moon: Modeling Intrusion Depth and Magmatic Pressure at the Crater Taruntius

Wichman, R. W.; Schultz, P. H.

doi:10.1006/icar.1996.0118

Cited by 36 publications

(19 citation statements)

References 5 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This interpretation is supported by studies of Schultz (1995, 1996) and by modeling of fl oor-fractured craters, which led Dombard, and Gillis (2001) to conclude that, compared to topographic relaxation, laccolith emplacement is the more viable formation process. Wichman and Schultz (1996) presented a model that allowed them to estimate the minimum depth of a 30 km wide and 1900 m thick intrusion beneath crater Tauruntius to be on the order of 1-5 km. The magma excess pressure was modeled to be on the order of 9 MPa.…”

Section: Volcanic Centers Several Areas Of the Moon Are Characterizementioning

confidence: 99%

New Views of Lunar Geoscience: An Introduction and Overview

Hiesinger

Head

2006

Reviews in Mineralogy and Geochemistry

197

139

View full text Add to dashboard Cite

Section: Volcanic Centers Several Areas Of the Moon Are Characterizementioning

confidence: 99%

New Views of Lunar Geoscience: An Introduction and Overview

Hiesinger

Head

2006

Reviews in Mineralogy and Geochemistry

197

139

View full text Add to dashboard Cite

“…The second stage consists of an expansion of the pressurized magmatic body in vertical direction, leading to flexure of the upper layer. During the third stage of laccolith formation, a "pistonlike uplift" of a piece of crustal material surrounded by faults may occur (Wichman and Schultz 1996). (Fig.…”

Section: Putative Intrusive Domesmentioning

confidence: 99%

Lunar Domes

Lena¹

2014

Encyclopedia of Lunar Science

View full text Add to dashboard Cite

“…This indicates that the Moon is not totally cold, or at least at the subsurface of the big Copernican craters. Wichman and Schultz (1996) used the piston model to illustrate the formation mechanism of crater floor fractures on the lunar surface [52]. These floor fractured craters (FFCs) are usually old and large impact craters.…”

Section: Significance To Future Studymentioning

confidence: 99%

Origin of pit chains in the floor of lunar Copernican craters

Xiao

Zeng

Xiao

et al. 2010

Sci. China Phys. Mech. Astron.

View full text Add to dashboard Cite

There are small pit chains in the floor of lunar Copernican craters. They are usually so small in scale that there are few lunar spacecrafts to detect their detailed morphology. Combining camera data from Lunar Orbiter, Lunar Reconnaissance Orbiter (LRO), Kaguya and Chang'e-1 missions, 5 representative large Copernican craters on various terrains of the lunar surface are chosen to study the origin of the pit chains in the crater floor. The morphology and distribution characteristic of the pit chains are referred by the high resolution images in this research. It is suggested that it is the magma activities from the subsurface magma layer combining with the existence of fractures and faults under the crater floor that leaded the formation of the pit chains. The model is further verified and discussed using the regolith thickness data in the crater floor. Our model suggests that the pit chains are still developing in the floor of the Copernican craters and the Moon may not be totally cold. Finally, the model limitation and potential future work are discussed based on available data. lunar, Copernican crater, pit chains, LRO, LROC, Kaguya, Chang'e-1 PACS: 96.15.Bc, 96.15.Lb, 96.15.Nd, 96.12.Xy

show abstract

Crater-Centered Laccoliths on the Moon: Modeling Intrusion Depth and Magmatic Pressure at the Crater Taruntius

Cited by 36 publications

References 5 publications

New Views of Lunar Geoscience: An Introduction and Overview

New Views of Lunar Geoscience: An Introduction and Overview

Lunar Domes

Origin of pit chains in the floor of lunar Copernican craters

Contact Info

Product

Resources

About