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Montes Haemus
Montes Haemus is a mountain range that forms the southwestern edge of the Mare Serenitatis basin on the Moon. They form a less prominent mirror image of the Montes Apenninus range to the west, and curve up to nearly join at the northern end. The eastern edge terminates with the Promontorium Archerusia, to the northwest of the crater Plinius. This end reaches a gap where the Mare Serenitatis to the north joins the Mare Tranquillitatis to the south. The selenographic coordinates of this range are , and the length is 560 km. The tallest peaks in this range climb as high as 2.4 km. This range is named after Haemus Mons, an old Thracian name of the Balkan mountains. It appeared on the map of Moon due to Johannes Hevelius. But he assigned this name (in the form ''Mons Æmus'') to another feature – remains of the rim of crater Alexander, located on the other side of Mare Serenitatis. Later the name moved to the subject of this article. The same name, but with reversed ord ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Montes Haemus (GLD100)
Montes Haemus is a mountain range that forms the southwestern edge of the Mare Serenitatis basin on the Moon. They form a less prominent mirror image of the Montes Apenninus range to the west, and curve up to nearly join at the northern end. The eastern edge terminates with the Promontorium Archerusia, to the northwest of the crater Plinius. This end reaches a gap where the Mare Serenitatis to the north joins the Mare Tranquillitatis to the south. The selenographic coordinates of this range are , and the length is 560 km. The tallest peaks in this range climb as high as 2.4 km. This range is named after Haemus Mons, an old Thracian name of the Balkan mountains. It appeared on the map of Moon due to Johannes Hevelius. But he assigned this name (in the form ''Mons Æmus'') to another feature – remains of the rim of crater Alexander, located on the other side of Mare Serenitatis. Later the name moved to the subject of this article. The same name, but with reversed ord ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Montes Apenninus
Montes Apenninus are a rugged mountain range on the northern part of the Moon's near side. They are named after the Apennine Mountains in Italy. With their formation dating back about 3.9 billion years, Montes Apenninus are fairly old. Description This range forms the southeastern border of the large Mare Imbrium lunar mare and the northwestern border of the Terra Nivium highland region. It begins just to the west of the prominent crater Eratosthenes, which abuts against the southern face of the range. To the west of these mountains is a narrow gap where Mare Imbrium in the north joins Mare Insularum to the south. Further to the west are the Montes Carpatus mountains. From Eratosthenes, the mountains form an arcing chain that gradually bends from east to northeast, ending at Promontorium Fresnel at about latitude 29.5° N. Here is another gap where the Mare Imbrium to the west joins the Mare Serenitatis to the east. At the north end of this gap lie the Montes Caucasus. This ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Mountains On Io
More than 135 mountains have been identified on the surface of Jupiter's moon Io. Despite the extensive active volcanism taking place on Io, most mountains on Io are formed through tectonic processes. These structures average 6 km (4 mi) in height and reach a maximum of 17.5 ± 1.5 km (10.9 ± 1 mi) at South Boösaule Montes. Mountains often appear as large (the average mountain is 157 km (98 mi) long), isolated structures with no apparent global tectonic patterns outlined, in contrast to the situation on Earth. To support the tremendous topography observed at these mountains requires rock compositions consisting mostly of silicate, as opposed to sulfur. Mountains on Io (generally, structures rising above the surrounding plains) have a variety of morphologies. Plateaus are most common. These structures resemble large, flat-topped mesas with rugged surfaces. Other mountains appear to be tilted crustal blocks, with a shallow slope ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gdańsk
Gdańsk ( , also ; ; csb, Gduńsk;Stefan Ramułt, ''Słownik języka pomorskiego, czyli kaszubskiego'', Kraków 1893, Gdańsk 2003, ISBN 83-87408-64-6. , Johann Georg Theodor Grässe, ''Orbis latinus oder Verzeichniss der lateinischen Benennungen der bekanntesten Städte etc., Meere, Seen, Berge und Flüsse in allen Theilen der Erde nebst einem deutsch-lateinischen Register derselben''. T. Ein Supplement zu jedem lateinischen und geographischen Wörterbuche. Dresden: G. Schönfeld’s Buchhandlung (C. A. Werner), 1861, p. 71, 237.); Stefan Ramułt, ''Słownik języka pomorskiego, czyli kaszubskiego'', Kraków 1893, Gdańsk 2003, ISBN 83-87408-64-6. * , )Johann Georg Theodor Grässe, ''Orbis latinus oder Verzeichniss der lateinischen Benennungen der bekanntesten Städte etc., Meere, Seen, Berge und Flüsse in allen Theilen der Erde nebst einem deutsch-lateinischen Register derselben''. T. Ein Supplement zu jedem lateinischen und geographischen Wörterbuche. Dresden: G. Schönf ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lacus Lenitatis
Lacus Lenitatis (Latin ''lēnitātis'', for "Lake of Softness") is a small lunar mare in the Terra Nivium region on the Moon The Moon is Earth's only natural satellite. It is the fifth largest satellite in the Solar System and the largest and most massive relative to its parent planet, with a diameter about one-quarter that of Earth (comparable to the width of .... It is located at 14.3° N, 12.1° E and is 78 km in diameter. References External links Lacus Lenitatis at The Moon Wiki Lenitatis {{Moon-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lacus Hiemalis
Lacus Hiemalis (Latin ''hiemālis'', "Lake of Winter") is a small lunar mare in the Terra Nivium region on the Moon The Moon is Earth's only natural satellite. It is the fifth largest satellite in the Solar System and the largest and most massive relative to its parent planet, with a diameter about one-quarter that of Earth (comparable to the width of .... It is located at 15.0° N, 14.0° E and is 50 km in diameter. Heimalis {{Moon-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lacus Gaudii
Lacus Gaudii (Latin ''gaudiī'', "Lake of Joy") is a small lunar mare in the Terra Nivium region of the Moon The Moon is Earth's only natural satellite. It is the fifth largest satellite in the Solar System and the largest and most massive relative to its parent planet, with a diameter about one-quarter that of Earth (comparable to the width of ....Digital Lunar Orbiter Photographic Atlas of the Moon, Lunar and Planetary InstitutAnnotated Lunar Orbiter 4 Image 097 h2 based on Bowker and Hughes (NASA SP-206) It is located at 16.3° N, 12.3° E and is 89 km in diameter. References External linksLacus Gaudii at The Moon Wiki* Gaudii {{Moon-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lacus Doloris
Lacus Doloris (Latin ''dolōris'', "Lake of Sorrow") is a small lunar mare located in the Terra Nivium Terra Nivium (Latin for "Land of Snows") is a roughly triangular highland region on the Moon. In his ''Almagestum novum'', the notable selenographer Giovanni Riccioli named the various highland regions terrae. However, unlike his naming scheme for ... region at 16.8° N, 8.6° E. It is 103 km in diameter. References Doloris {{Moon-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lacus Odii
Lacus Odii (Latin ''odiī'', "Lake of Hate") is a small lunar mare in the Terra Nivium region on the Moon The Moon is Earth's only natural satellite. It is the fifth largest satellite in the Solar System and the largest and most massive relative to its parent planet, with a diameter about one-quarter that of Earth (comparable to the width of .... It is located at 19.0° N, 7.0° E and is 70 km in diameter. Odii {{Moon-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lava
Lava is molten or partially molten rock (magma) that has been expelled from the interior of a terrestrial planet (such as Earth) or a moon onto its surface. Lava may be erupted at a volcano or through a fracture in the crust, on land or underwater, usually at temperatures from . The volcanic rock resulting from subsequent cooling is also often called ''lava''. A lava flow is an outpouring of lava during an effusive eruption. (An explosive eruption, by contrast, produces a mixture of volcanic ash and other fragments called tephra, not lava flows.) The viscosity of most lava is about that of ketchup, roughly 10,000 to 100,000 times that of water. Even so, lava can flow great distances before cooling causes it to solidify, because lava exposed to air quickly develops a solid crust that insulates the remaining liquid lava, helping to keep it hot and inviscid enough to continue flowing. The word ''lava'' comes from Italian and is probably derived from the Latin word ''labes ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Basalt
Basalt (; ) is an aphanite, aphanitic (fine-grained) extrusive igneous rock formed from the rapid cooling of low-viscosity lava rich in magnesium and iron (mafic lava) exposed at or very near the planetary surface, surface of a terrestrial planet, rocky planet or natural satellite, moon. More than 90% of all volcanic rock on Earth is basalt. Rapid-cooling, fine-grained basalt is chemically equivalent to slow-cooling, coarse-grained gabbro. The eruption of basalt lava is observed by geologists at about 20 volcanoes per year. Basalt is also an important rock type on other planetary bodies in the Solar System. For example, the bulk of the plains of volcanism on Venus, Venus, which cover ~80% of the surface, are basaltic; the lunar mare, lunar maria are plains of flood-basaltic lava flows; and basalt is a common rock on the surface of Mars. Molten basalt lava has a low viscosity due to its relatively low silica content (between 45% and 52%), resulting in rapidly moving lava flo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lunar Mare
The lunar maria (; singular: mare ) are large, dark, basaltic plains on Earth's Moon, formed by ancient asteroid impacts on the far side on the Moon that triggered volcanic activity on the opposite (near) side. They were dubbed , Latin for 'seas', by early astronomers who mistook them for actual seas. They are less reflective than the "highlands" as a result of their iron-rich composition, and hence appear dark to the naked eye. The maria cover about 16% of the lunar surface, mostly on the side visible from Earth. The few maria on the far side are much smaller, residing mostly in very large craters. The traditional nomenclature for the Moon also includes one (ocean), as well as features with the names ('lake'), ('marsh'), and ('bay'). The last three are smaller than maria, but have the same nature and characteristics. The names of maria refer to sea features (Mare Humorum, Mare Imbrium, Mare Insularum, Mare Nubium, Mare Spumans, Mare Undarum, Mare Vaporum, Oceanus Procellarum ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
.jpeg/1200px-Brama_Zuraw_W_Gdansku_(153003103).jpeg "Click for more on -> Gdańsk")
