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Piccolornini to Theoph¡Ins 2004.09.20 -12:00 UT Agsßdays, 10-in f/6 Newtonian + 2.5X + ToUcam (Thumbnail is from 4X Bartow)

Piccolomini and Rupes Altai at Moon Age of 18 days

PiccoSomini and Rupes Altai 2006.08.12 21:30-21:41 UT Age 18.5days 10-inch 1/6 Newtonian 4 2.5X + 1.6X + ToUcam, 95% resized, (mosaic) The 2X enlargement shows a section of Rupes Altai with abrupt slope. Position A is roughly 1000 m higher than the toot of the cliff, Due to low surface gravity (1/6 that of Earth), a stone dropping from position A will take half minute to reach the ground.

PiccoSomini and Rupes Altai 2006.08.12 21:30-21:41 UT Age 18.5days 10-inch 1/6 Newtonian 4 2.5X + 1.6X + ToUcam, 95% resized, (mosaic) The 2X enlargement shows a section of Rupes Altai with abrupt slope. Position A is roughly 1000 m higher than the toot of the cliff, Due to low surface gravity (1/6 that of Earth), a stone dropping from position A will take half minute to reach the ground.

Remark: Distance dropped by a free-falling object on the lunar surface is equal to 1/2 • g • t2 , where g is the gravitational acceleration (= 1.62 m/s2) and t is the time of falling.

Mare Nectaris (Sea of Nectar) 35.50 E 15.20 S This is a small mare inside an impact basin, diameter about 330 km. The impact basin is traceable by a pattern of three concentric rings, as suggested in Image T008A. Rupes Altai lies on the outmost ring of the basin. Theophilus, Cyrillus and Catharina form a prominent crater trio between Ring 1 and Ring 2.

Theophilus 26.40 E 11.40 S A ring mountain, 110 km in diameter. Its massive terraced walls rise 4000 m above the interior. These huge walls appear as two to three concentric ring mountain ranges, each successively lower to the next until the floor is reached. At lower powers Theophilus appears to be circular while higher powers show the walls to be composed of linear segments. On the north-western wall is a small crater Theophilus B. Theophilus also contains magnificent multiple central mountains with one of the peaks rising 1400 m above the floor. Theophilus is a rayed center under high illumination.

Theophilus, Cyrillus & Catharina 2006.07,31 UT Ag«6.3 days- IWnitt Newtonian * 2.5X * ToUom[moss«;)
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Cyrillus 24.00 E 13.20 S A ring mountain with disintegrated wall and three central peaks, 98 km in diameter. It is obvious that the Theophilus impact destroyed a section of Cyrillus's walls. Cyrillus is therefore older than Theophilus. The southwest wall contains a small crater, Cyrillus A. The floor of Cyrillus does not appear smooth like the floor of Theophilus, but rough with ridges and depressions. The floor of Cyrillus F (diameter 44 km) also contains a shallow depression with central uplift. It casts a tortoise-shaped dark shadow during Moon age of 18~19 days. (Image T009 & T144).

Cyrillus & Cyrillus F 2006.06.12 21:43 UT Age 13 days 10-in ffS Newtonian + 4X + Toltcam The arrow points to an interesting crater trio (Beaumont A12 eraterlets} that resembtes a magnifying glass.

In the vicinity of Cyrillus F is an interesting trio of craters (Beaumont A + 2 craterlets) that resembles a magnifying glass.

Cyrillus & Cyrillus F 2006.06.12 21:43 UT Age 13 days 10-in ffS Newtonian + 4X + Toltcam The arrow points to an interesting crater trio (Beaumont A12 eraterlets} that resembtes a magnifying glass.

Catharina 23.40 E 18.10 S

A ring mountain with disintegrated wall, 104 km in diameter. Catharina is connected to Cyrillus by a broad valley, and is believed the oldest of the trio. It has been nearly obliterated by several impacts. There are big and small craters on its floor (the most prominent being Catharina P), but no sign of central peaks. The central peaks must have existed years ago but finally overwhelmed by Catharina P.

A 27-km crater. Its ejecta blanket is fan-like and relatively whitish. See also Map 7

Piccolomini 32.20 E 29.70 S

A prominent crater with terraced walls and central peaks, 87 km in diameter, 4500 m in depth. Rupes Altai 22.60 E 24.30 S

A sinuous mountain fault running between Piccolomini and Catharina, about 450 km in length. It is the remains of the rising rim of an impact basin in which the central part is Mare Nectaris. See also Image T008A. The slope of this fault toward Mare Nectaris drops 1000 m in average.

(Image T245, next page) Lindenau 24.90 E 32.30 S

A prominent terraced crater with multiple central peaks, 53 km in diameter, 2900 m in depth. Rabbi Levi 23.60 E 34.70 S

An 81-km crater with 5 smaller but prominent ones on the floor. Its eastern wall is heavily ruined by a cluster of impact craters.

Zagut 22.10 E 32.00 S

A crater adjoining Rabbi Levi, 84 km in diameter. Its floor contains a small central crater. Its southeastern wall looks linear and interrupted by a fairly large crater (Zagut E, diameter 35 km).

F raca s to ri us 2005.08.22 19:07 UT Ag e 17.5 days. 10-in f/6 Newtonian + 2.5X + 1,6X + ToUcam, 93 frames stacked.

Fracastorius 33.20 E 21.50 S (Image T229)

An incomplete walled plain, 112 km in diameter. Its bay-like floor opens to Mare Nectaris and contains a long narrow, unnamed rille that intersects Fracastorius M. This rille is rather elusive to spot unless the illumination angle is appropriate. The floor also contains a tiny rayed crater and dome-like hills. The western wall of Fracastorius is partially ruined by irregular craters Fracastorius Y, D and H. Note the interesting crater-trio formation (arrow in T229).

Messier, Censorinus, Taruntius, Cauchy

Hatfield 3

I Mare Smytbii i

Hatfield 3

I Mare Smytbii

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IV ~ <VA*JU 1¿MHMkXl J a ill' % KMRttX^UJV^ Messier A anri Censorinus 20M.1Q.21 -H:2fiUT Age 8 days. Libration I« 3.3° b * 6 .8°,10nn 1iB + ToUcam at prime focus (mosaic^

47.60 E

(Image T105) Messier

Messier A 47.0UE A pair of small impact craters in Mare Fecunditatis (Sea of Fertility), diameter 11 ~ 13 km. Messier looks oval in shape that is definitely not caused by foreshortening. Messier A is a double crater and hence looks somewhat elongated. Its ejecta splashs out as two long bright rays like a comet; each ray is over 100 km long towards the west. This crater pair probably formed simultaneously by a grazing binary or broken impactor.

Rima Messier 45.0° E 1.0° S An inconspicuous rille, length about 100 km.

Rimae Secchi 44.00 E 1.00 N An elusive short rille, length 35 km. It is in the south of Secchi (Label 13, T262 in next page).

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