Difference between revisions of "Apennine Bench Formation"
| Line 13: | Line 13: | ||
[http://www.lpi.usra.edu/resources/mapcatalog/LAC/lac41/ LAC map] [http://www.lpi.usra.edu/resources/mapcatalog/usgs/I463/ Geologic Map I-463]<br /> <br /> | [http://www.lpi.usra.edu/resources/mapcatalog/LAC/lac41/ LAC map] [http://www.lpi.usra.edu/resources/mapcatalog/usgs/I463/ Geologic Map I-463]<br /> <br /> | ||
==Description== | ==Description== | ||
| − | This name was introduced by R. J. Hackman on ''Lunar Geologic Map I-463'' (1966, referenced above). He describes it as a smooth rolling topography of moderate albedo with many small craters. Based purely on telescopic observations, Hackman thought it represented old lava flows and ash beds, similar to, but older than the normal dark mare material. It was later proposed that this might be melt material from the Imbrium impact. Spudis (see reference below) rejected this idea, and suggested the Apennine Bench Formation consists of highland volcanic flows that formed after the Imbrium impact, but before the formation of the mare. <span class="membersnap">- | + | This name was introduced by R. J. Hackman on ''Lunar Geologic Map I-463'' (1966, referenced above). He describes it as a smooth rolling topography of moderate albedo with many small craters. Based purely on telescopic observations, Hackman thought it represented old lava flows and ash beds, similar to, but older than the normal dark mare material. It was later proposed that this might be melt material from the Imbrium impact. Spudis (see reference below) rejected this idea, and suggested the Apennine Bench Formation consists of highland volcanic flows that formed after the Imbrium impact, but before the formation of the mare. <span class="membersnap">- JimMosher</span><br /> <br /> |
==Additional Information== | ==Additional Information== | ||
* The coordinates given in the title line are for a representative sample of this material cited by Hackman and located about midway between [[Archimedes|Archimedes]] and [[Mons%20Huygens|Mons Huygens]]. According to Spudis, other sections of this relatively high albedo material may be found at several other locations ringing the eastern shore of [[Mare%20Imbrium|Mare Imbrium]]. | * The coordinates given in the title line are for a representative sample of this material cited by Hackman and located about midway between [[Archimedes|Archimedes]] and [[Mons%20Huygens|Mons Huygens]]. According to Spudis, other sections of this relatively high albedo material may be found at several other locations ringing the eastern shore of [[Mare%20Imbrium|Mare Imbrium]]. | ||
| Line 20: | Line 20: | ||
* Named by R. J. Hackman (see ''Description'') | * Named by R. J. Hackman (see ''Description'') | ||
| − | * [http://apollo.sese.asu.edu/LIW/20080219.html Apennine Bench Formation: Unique Lunar Volcanism], an Image of the Week on Arizona State University's growing ''Apollo Image Archive'', describes this formation in some detail. Rather than serving as a generic name for surfaces with similar characteristics, the authors imply the name applies only to the region pictured above, and within very specific boundaries. <span class="membersnap">- | + | * [http://apollo.sese.asu.edu/LIW/20080219.html Apennine Bench Formation: Unique Lunar Volcanism], an Image of the Week on Arizona State University's growing ''Apollo Image Archive'', describes this formation in some detail. Rather than serving as a generic name for surfaces with similar characteristics, the authors imply the name applies only to the region pictured above, and within very specific boundaries. <span class="membersnap">- JimMosher</span> |
<br /> | <br /> | ||
==LPOD Articles== | ==LPOD Articles== | ||
Latest revision as of 20:37, 16 April 2018
Contents
Apennine Bench Formation
(informal geologic name)
|
Lat: 24-25 N, Long: 2-4 W, Diameter: km, Depth: km, Rukl: 22 |
Peter Lloyd The large ring-shaped crater at the top is Archimedes and the diagonal line of shadow-casting peaks near the bottom is Montes Apenninus. The term Apennine Bench Formation was originally used to denote the diamond-shaped zone of relatively smooth light-gray material situated roughly midway between them and somewhat larger than Archimedes in size.
Images
LPOD Photo Gallery Lunar Orbiter Images
Maps
Description
This name was introduced by R. J. Hackman on Lunar Geologic Map I-463 (1966, referenced above). He describes it as a smooth rolling topography of moderate albedo with many small craters. Based purely on telescopic observations, Hackman thought it represented old lava flows and ash beds, similar to, but older than the normal dark mare material. It was later proposed that this might be melt material from the Imbrium impact. Spudis (see reference below) rejected this idea, and suggested the Apennine Bench Formation consists of highland volcanic flows that formed after the Imbrium impact, but before the formation of the mare. - JimMosher
Additional Information
- The coordinates given in the title line are for a representative sample of this material cited by Hackman and located about midway between Archimedes and Mons Huygens. According to Spudis, other sections of this relatively high albedo material may be found at several other locations ringing the eastern shore of Mare Imbrium.
Nomenclature
- Named by R. J. Hackman (see Description)
- Apennine Bench Formation: Unique Lunar Volcanism, an Image of the Week on Arizona State University's growing Apollo Image Archive, describes this formation in some detail. Rather than serving as a generic name for surfaces with similar characteristics, the authors imply the name applies only to the region pictured above, and within very specific boundaries. - JimMosher
LPOD Articles
Bibliography
Spudis, PD (1978). Composition and origin of the Apennine Bench Formation. Proc. Lunar Planet. Sci. Conf. 9th, 3379-3394.
