LE CRATÈRE PLATON PAR JAMES NASMYTH

 

JAMES NASMYTH  (1808-1890)
Le cratère Platon (2000m)
La Lune, Système solaire

In Plato Crater Moon, photographie retouchée sur appareil Nasmyth, 1855

Le relief
Platon (2000m de profondeur) est un cratère d'impact lunaire situé sur la face visible de la Lune. Il se trouve au nord-est de la Mare Imbrium et des Montes Teneriffe, à l'extrémité orientale des Montes Jura et à l'extrémité occidentale des Montes Alpes d'où partent des crevasses lunaires dénommées Rimae Platon. Au nord s'étend la Mare Frigoris. Le contour circulaire possède de nombreux pics qui donnent des ombres à l'intérieur du cratère. L'intérieur du cratère a un albédo, apparaissant lisse sans présence aucune d'impacts quelconques. Le cratère Platon est connu pour être un lieu de phénomène lunaire transitoire (PLT) consistant dans l'apparition d'une lumière ou d'une modification d'aspect de sa surface lunaire pendant une courte durée. 

L'artiste
James Nasmyth est un mécanicien et astronome écossais, au talent artistique certain,. Fils du peintre Alexander Nasmyth, il montra de bonne heure de grandes aptitudes pour les mathématiques et la mécanique, travailla de 1829 à 1831 chez le constructeur Henry Maudslay, puis fonda à Particroft, près de Manchester, un important établissement qui prospéra rapidement sous le nom de fonderie Bridgewater et qu'il pourvut d'un outillage perfectionné.
Parmi ses nombreuses inventions, il faut surtout citer le marteau-pilon, dont il paraît avoir eu l'idée en même temps que le Français François Bourdon. On lui doit également une cuiller de sûreté pour les fondeurs, un ventilateur pour les mines, un laminoir, une machine marine, etc.  Il s'était retiré en 1837 à Penshurst (comté de Kent), s'occupant avec passion d'astronomie et prenant, avec des appareils de sa construction, des photographies du Soleil et de la Lune, qui comptent parmi les plus remarquables qu'on ait jamais obtenues. Il a également inventé le télescope Nasmyth, une variante du Cassegrain.

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2024- Gravir les montagnes en peinture

Un blog de Francis Rousseau 

 

SIDONIA MENSAE / LE VISAGE DE MARS VU PAR NASA MARS GLOBAL SURVEYOR

MARS GLOBAL SURVEYOR (1996-2007)
Sidonia Mensae nd)
Planète Mars 

Le relief
Cydonia Mensae, connu aussi sous le nom de "Le Visage de Mars" est un relief martien situé dans le quadrangle de Mare Acidalium. Il est à l'origine d'un exemple de paréidolie. Le 25 juillet 1976, au cours de sa 35e orbite, l'orbiteur Viking 1 survole Mars autour du 41° de latitude nord. C'est lors de ce passage qu'est pris le fameux cliché du « visage de Mars ». Si les scientifiques y voient un banal jeu d'ombres et lumière sur le relief, à l'époque, certains passionnés de vie extraterrestre ont cru y déceler une structure artificielle. Depuis, de nouvelles photos du visage prises par la sonde Mars Global Surveyor avec une résolution bien supérieure ont montré qu'il s'agit d'une colline érodée. Dans la zone de Cydonia à proximité du « visage », un peu plus au sud-ouest, il y a une autre colline ressemblant à une pyramide à cinq faces, mise en évidence par Vincent DiPietro et Gregory Molenaar et nommée en conséquence D&M. Les spéculations autour de ce « visage » atteignent un tel niveau que la NASA en fait une des cibles prioritaires de son nouvel orbiteur, Mars Global Surveyor. Jim Garvin, chef scientifique du programme d'exploration de Mars de la NASA, déclare « nous avons photographié le « visage » dès que nous avons pu en avoir un bon aperçub ». Ainsi, le 5 avril 1998, soit 22 ans après les images prises par Viking 1, Mars Global Surveyor photographie la région avec une résolution dix fois supérieure à celle de Viking 1, grâce son imageur Mars Orbiter Camera. Comme attendu, le cliché ne dévoile qu'un massif montagneux classique et aucun signe d'un éventuel visage. 

La mission
Mars Global Surveyor (MGS) également désignée par son sigle MGS, est une mission spatiale développée par le centre JPL de la NASA qui a étudié de 1997 à 2006 l'atmosphère et la surface de la planète Mars en circulant sur une orbite héliosynchrone autour de celle-ci. La sonde spatiale devait répondre aux nombreuses interrogations soulevées par les données collectées dans le cadre du programme Viking lancé 20 ans auparavant portant sur l'histoire de la planète, la structure de sa surface et de son atmosphère ainsi que sur les processus dynamiques encore à l’œuvre. L'agence spatiale américaine lance la conception de Mars Global Surveyor en 1994 à la suite de l'échec de la mission martienne Mars Observer. MGS reprend les principaux objectifs de celle-ci, mais, afin de limiter son coût, la sonde spatiale réutilise les instruments et les équipements développés pour Mars Observer. Elle est construite et testée en un temps record puis lancée en novembre 1996. Pour se placer sur son orbite de travail autour de Mars, la sonde spatiale inaugure le recours à l'aérofreinage qui permet de réduire la quantité d'ergols transportée et donc d'abaisser les coûts. Le déploiement incomplet d'un panneau solaire rallonge la phase d'aérofreinage qui s'achève en février 1999, soit 15 mois après la date prévue. La phase de recueil des données scientifiques débute alors et se prolonge jusqu'en octobre 2006 établissant un nouveau record de longévité. Les découvertes réalisées grâce à la mission et les images spectaculaires prises par la caméra contribuent à renouveler l'intérêt des scientifiques mais également du grand public pour la planète Mars. L'altimètre laser de MGS dresse la première carte topographique de la planète mettant en évidence les différences spectaculaires entre les hémisphères nord et sud. Le spectromètre infrarouge TES découvre des régions où abonde l'hématite grise qui pourrait signaler la présence d'eau dans le passé et qui, à ce titre, fera l'objet d'investigations poussées par les missions spatiales suivantes. Le magnétomètre détecte un magnétisme rémanent présent dans la croute de certaines régions qui constitue sans doute le vestige d'un champ magnétique qui s'est éteint il y a 4 milliards d'années. Enfin, la caméra MOC fournit des images haute définition qui démontrent la complexité des paysages martiens, permettent de découvrir de nombreuses formations originales comme les traînées noires, les ravines associées potentiellement à la présence d'eau dans un passé lointain ou non, et plus généralement contribuent à reconstituer l'histoire de la planète. 

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2024 - Gravir les montagnes en peinture
Un blog de Francis Rousseau

OLYMPUS MONS / PLANÈTE MARS PHOTOGRAPHIÉ PAR NASA VIKING ORBITER 1

NASA VIKING ORBITER  (1975-1982)
Olympus Mons (21, 229 mètres soit 21, 2 km d'altitude)
Planète Mars (Voie Lactée)

D'après une photographie prise en 1979, à 5000 km de hauteur, retouchée par IA en 2020. 

Photo originale prise par la sonde NASA Viking Orbiter 1 en 1979.

Le  volcan
Olympus Mons (21, 2 km)  nom latin pour « mont Olympe », est un volcan bouclier de la planète Mars situé dans les quadrangles d'Amazonis et de Tharsis. C'est le plus haut relief connu du système solaire, culminant à 21 229 mètres au-dessus du niveau de référence martien selon les mesures très précises de l'altimètre laser de Mars Global Surveyor (ancienne mesure 22 500 mètres). Son impressionnant diamètre est de 648 km, c'est à dire qu'il couvrirait la plus grande partie du territoire français et Suisse s'étendant de Bordeaux à Genève et de Paris à Montélimar !
Il se trouve sur la bordure nord-ouest du renflement de Tharsis, immense soulèvement de la surface martienne, centré sur Noctis Labyrinthus et Syria Planum, dont l'extension occidentale concentre une douzaine de volcans majeurs..
L'édifice central s'élève à  deux fois et demie la hauteur de l'Everest par rapport au niveau de la mer et plus du double de celle du Mauna Kea (Hawaï) par rapport à sa base  Il possède à son sommet une caldeira complexe d'environ 80 × 60 kilomètres résultant de la coalescence d'au moins six cratères enchevêtrés, attestant de l'histoire mouvementée de la caldeira avec notamment la présence de grabens résultant de l'effondrement de la surface dans une faille.
Il est entouré d'une falaise formant un escarpement continu sur toute sa circonférence, d'une hauteur de 2 à 6 kilomètres. Au-delà de cet escarpement se trouve une zone souvent appelée « l'auréole » du volcan, constituée de crêtes et de grands blocs s'étendant jusqu'à un millier de kilomètres de la caldeira. Cela met en évidence l'expansion et la modification de la surface liées à l'activité glaciaire.
L'inclinaison des pentes du volcan est voisine de 5 degrés en moyenne, atteignant 30 degrés au niveau de l'escarpement périphérique.
À proximité de la caldeira se trouvent deux cratères d'impact. À une vingtaine de kilomètres au sud, le cratère Pangboche a un diamètre de 10,4 kilomètres. Il a été nommé par l'Union astronomique internationale en 2006 d'après une localité du Népal située à vingt kilomètres du sommet de l'Everest. C'est sur le rebord ouest de ce cratère que se trouve le point le plus haut d'Olympus Mons, à 21 229 mètres au-dessus du niveau de référence. Le cratère Karzok, situé à une quarantaine de kilomètres à l'est de la caldeira, a un diamètre de 15,6 kilomètres. Il a été nommé d'après une localité du Cachemire indien. D'autres cratères d'impact sont également visibles sur les flancs du volcan.
L'escarpement et l'auréole sont tous deux mal compris. La falaise résulterait de glissements de terrain, et l'auréole proviendrait des matériaux entassés au bas de ces glissements. Les coulées de lave s'étendent au-delà de l'escarpement. L'escarpement qui entoure la montagne à sa base aurait été formé par des glissements de terrain induits par une fonte massive du permafrost11 ou par un soulèvement tectonique. Les structures linéaires en forme de crêtes présentes autour du volcan au-delà de l'escarpement seraient, quant à elles, des dykes mis en place après les dernières coulées de lave ayant atteint la base du volcan. Son premier nom, Nix Olympica, en français « Neige de l'Olympe », lui avait été donné par l'astronome italien Giovanni Schiaparelli (1835-1910). 

La mission
NASA Viking Orbiter 1 était le premier des deux engins spatiaux (avec Viking 2) envoyés sur Mars dans le cadre du programme Viking de la NASA. Le 20 juillet 1976, il est devenu le deuxième vaisseau spatial à atterrir en douceur sur Mars, et le premier à réussir sa mission. (Le premier vaisseau spatial à atterrir en douceur sur Mars était le Mars 3 de l'Union soviétique le 2 décembre 1971, qui a cessé de transmettre après 14,5 secondes.) Viking 1 détenait le record de la plus longue mission de surface de Mars de 2307 jours (plus de 6 1⁄ 4 ans) ou 2245 jours solaires martiens, jusqu'à ce que ce record soit battu par le rover Opportunity le 19 mai 2010. Après le lancement à l'aide d'un lanceur Titan/Centaur le 20 août 1975 et une croisière de 11 mois vers Mars, l'orbiteur a commencé à renvoyer des images globales de Mars environ 5 jours avant l'insertion en orbite. L'orbiteur Viking 1 a été inséré dans l'orbite de Mars le 19 juin 1976 et ajusté à une orbite de certification de site de 1513 x 33 000 km, 24,66 h le 21 juin. L'atterrissage sur Mars était prévu pour le 4 juillet 1976, le bicentenaire des États-Unis, mais l'imagerie du site d'atterrissage principal a montré qu'il était trop difficile pour un atterrissage en toute sécurité. L'atterrissage a été retardé jusqu'à ce qu'un site plus sûr soit trouvé et a eu lieu à la place le 20 juillet, le septième anniversaire de l'alunissage d'Apollo 11. L'atterrisseur s'est séparé de l'orbiteur à 08:51 UTC et a atterri à Chryse Planitia à 11:53:06 UTC. C'était la première tentative des États-Unis d'atterrir sur Mars.
Les instruments de l'orbiteur se composaient de deux caméras vidicon pour l'imagerie (VIS), d'un spectromètre infrarouge pour la cartographie de la vapeur d'eau (MAWD) et de radiomètres infrarouges pour la cartographie thermique (IRTM). La mission principale de l'orbiteur s'est terminée au début de la conjonction solaire le 5 novembre 1976.
La mission prolongée a commencé le 14 décembre 1976, après la conjonction solaire. Les opérations comprenaient des approches rapprochées de Phobos en février 1977. Le périastre a été réduit à 300 km le 11 mars 1977. Des ajustements mineurs d'orbite ont été effectués occasionnellement au cours de la mission, principalement pour modifier le taux de marche - le taux auquel la longitude aréocentrique changé à chaque orbite, et le périastre a été porté à 357 km le 20 juillet 1979. Le 7 août 1980, Viking 1 Orbiter manquait de gaz de contrôle d'attitude et son orbite a été portée de 357 × 33943 km à 320 × 56000 km pour éviter l'impact avec Mars et une éventuelle contamination jusqu'en 2019. Les opérations ont pris fin le 17 août 1980, après 1485 orbites. Une analyse de 2009 a conclu que, même si la possibilité que Viking 1 ait eu un impact sur Mars ne pouvait être exclue, il était très probablement toujours en orbite. Plus de 57 000 images ont été renvoyées sur Terre.

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2023 - Gravir les montagnes en peinture...
Un blog de Francis Rousseau

 

IRESON HILL / MARS PHOTOGRAPHIÉE PAR NASA MARS CURIOSITY MISSION

 

NASA MARS CURIOSITY MISSION (depuis 2012)

Ireson Hill sur Aeolis Mons/Mount Sharp (5, 500 m - 18, 000 ft)

MARS

La colline
Ce monticule sombre, appelé "Ireson Hill", s'élève à environ 5 mètres au-dessus du matériau d'affleurement en couches plus rouge de la formation Murray sur le mont Sharp inférieur (5, 500 mètres d'altitude), sur  la planète Mars, près d'un endroit où le rover Curiosity de la NASA a examiné une dune de sable linéaire en février 2017.  Qu'est-ce qui a créé cette colline inhabituelle sur Mars ? Pas de réponse pour l'instant mais un sujet de recherche  pour plusieurs années tant il est vrai que sa forme et sa structure bicolore en font l'une des formations les plus inhabituelles que le robot Curiosity ait croisé dans son exploration de la planète. Surnommé  "Colline Ireson", le monticule s'étend sur environ 15 mètres de largeur. Ce panorama composé de 41 images a été compressé horizontalement pour inclure toute la colline. L'image a été prise le 2 février 2017.

La camera
Les chercheurs ont utilisé la Mast Camera (Mastcam) du rover le 2 février 2017, lors du 1 598e jour martien, ou sol, des travaux de Curiosity sur Mars, pour prendre les 41 images combinées dans cette scène. La mosaïque a été équilibrée en blanc afin que les couleurs des matériaux de roche et de sable ressemblent à ce qu'elles apparaîtraient dans des conditions d'éclairage diurne sur Terre. La vue s'étend de l'ouest-sud-ouest à gauche au nord-nord-ouest à droite. Le faible horizon au loin au-delà d'Ireson Hill fait partie du bord du cratère Gale. Malin Space Science Systems, San Diego, a construit et exploite le Mastcam. Le Jet Propulsion Laboratory de la NASA, une division de Caltech à Pasadena, en Californie, gère le projet de laboratoire scientifique sur Mars pour la direction des missions scientifiques de la NASA, à Washington. JPL a conçu et construit le rover Curiosity du projet.

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2023 - Wandering Vertexes ....
Errant au-dessus des Sommets Silencieux...
Un blog de Francis Rousseau

APOLLINARIS MONS PHOTOGRAPHIÉ PAR NASA MARS GLOBAL SURVEYOR

 

NASA MARS GLOBAL SURVEYOR (1996-2007)
Apollinaris Mons (5,500m)
MARS

Le volcan
Apollinaris Mons (5500 mètres), parfois appelé Apollinaris Patera bien que ce nom ne se réfère stricto sensu qu'à sa caldeira sommitale, est un volcan situé sur la planète Mars par 9,3° S et 174,4° E dans le quadrangle d'Aeolis (MC-23), à la frontière géologique matérialisant la dichotomie crustale martienne. Large de 295 km, il culmine à un peu plus de 3 000 m d'altitude au-dessus du niveau de référence martien et d'environ 5 500 m au-dessus d'Elysium Planitia. Ce volcan possède une caldeira à deux niveaux d'environ 85 km de diamètre et de l'ordre de 1 500 m de profondeur. 'est un volcan très ancien, formé au Noachien il y a au moins 3,8 milliards d'années — peut-être même 4 milliards d'années — et dont l'activité ne s'est pas prolongée au-delà du début de l'Hespérien, cessant au plus tard il y a 3,6 milliards d'années.
Il semble s'agir d'un stratovolcan dont la très vaste caldeira résulterait d'une éruption plinienne.

La photographie
En avril 1999, la caméra Mars Global Surveyor Mars Orbiter Camera (MOC) est passée au-dessus du volcan Apollinaris Patera et a capturé une nappe de nuages lumineux suspendus au-dessus de son sommet au début de l'après-midi martien. Cet ancien volcan est situé près de l'équateur et, d'après les observations des orbiteurs vikings des années 1970, on pense qu'il mesure jusqu'à 5 kilomètres (3 miles) de haut. La couleur de cette image est dérivée des systèmes de caméra grand angle rouge et bleu MOC et ne représente pas la vraie couleur telle qu'elle apparaîtrait à l'œil humain (c'est-à-dire si un humain était en mesure d'orbiter autour de la planète rouge) . L'éclairage vient du coin supérieur gauche.
Malin Space Science Systems et le California Institute of Technology ont construit le MOC en utilisant du matériel de rechange de la mission Mars Observer. MSSS exploite la caméra depuis ses installations de San Diego, en Californie. Le projet Mars Surveyor Operations du Jet Propulsion Laboratory exploite le vaisseau spatial Mars Global Surveyor avec son partenaire industriel, Lockheed Martin Astronautics, à partir d'installations à Pasadena, CA et Denver, CO. 

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2023 - Wandering Vertexes ....
Errant au-dessus des Sommets Silencieux...
Un blog de Francis Rousseau 

PHLEGRA MONTES PHOTOGRAPHED BY ESA MARS EXPRESS MISSION

ESA MARS EXPRESS MISSION ( 2004-2022)
Phlegra Montes (1,4km - 870 mi)
Mars (Solar system)

 

About that image
The High-Resolution Stereo Camera on ESA’s Mars Express collected the data for these images on 1 June 2011 during orbit 9465. This perspective view has been calculated from the Digital Terrain Model derived from the stereo channels.
Courtesey ESA/DLR/FU Berlin (G. Neukum),CC BY-SA 3.0 IGO

The mountains
The Phlegra Montes are a system of eroded Hesperian–Noachian-aged massifs and knobby terrain in the mid-latitudes of the northern lowlands of Mars, extending northwards from the Elysium Rise towards Vastitas Borealis for nearly 1,400 km (870 mi). The mountain ranges separate the large plains provinces of Utopia Planitia (west) and Amazonis Planitia (east), and were named in the 1970s after a classical albedo feature. The massif terrains are flanked by numerous parallel wrinkle ridges known as the Phlegra Dorsa. The mountain ranges were first mapped against imagery taken during NASA's Viking program in the 1970s, and the area is thought to have been uplifted due to regional-scale compressive stresses caused by the contemporary formations of the Elysium and Tharsis volcanic provinces. Recent research has unveiled the presence of extensive thrust faulting bounding the massif terrains. Since the 2010s, researchers have proposed the presence of a significant late Amazonian glaciation event along the Martian northern mid-latitudes, citing the presence of lineated valley fills, lobate debris aprons, and concentric crater fills. The presence of ring mold craters imply that significant stores of water ice may continue to persist in these terrains. Features interpreted as eskers have been observed in the southern Phlegra Montes. However, whether this glaciation was localized or of regional scale remains subject to debate in the scientific community.

About the mission
Mars Express is a space exploration mission being conducted by the European Space Agency (ESA). The Mars Express mission is exploring the planet Mars, and is the first planetary mission attempted by the agency. "Express" originally referred to the speed and efficiency with which the spacecraft was designed and built.However, "Express" also describes the spacecraft's relatively short interplanetary voyage, a result of being launched when the orbits of Earth and Mars brought them closer than they had been in about 60,000 years. Mars Express consists of two parts, the Mars Express Orbiter and Beagle 2, a lander designed to perform exobiology and geochemistry research. Although the lander failed to fully deploy after it landed on the Martian surface, the orbiter has been successfully performing scientific measurements since early 2004, namely, high-resolution imaging and mineralogical mapping of the surface, radar sounding of the subsurface structure down to the permafrost, precise determination of the atmospheric circulation and composition, and study of the interaction of the atmosphere with the interplanetary medium. Due to the valuable science return and the highly flexible mission profile, Mars Express has been granted several mission extensions. The latest was approved on 1 October 2020 and runs until 31 December 2022. Some of the instruments on the orbiter, including the camera systems and some spectrometers, reuse designs from the failed launch of the Russian Mars 96 mission in 1996 (European countries had provided much of the instrumentation and financing for that unsuccessful mission). The design of Mars Express is based on ESA's Rosetta mission, on which a considerable sum was spent on development. The same design was also used for ESA's Venus Express mission in order to increase reliability and reduce development cost and time. Because of these redesigns and repurposings, the total cost of the project was about $345 million- less than half of comparable U.S. missions. Arriving at Mars in 2003, 18 years, 9 months and 10 days ago (and counting), it is the second longest surviving, continually active spacecraft in orbit around a planet other than Earth, behind only NASA's still active 2001 Mars Odyssey.

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2022- Wandering Vertexes
A blog by Francis Rousseau

COPERNICUS CRATER AS SEEN BY J.A. GILLET AND W.J.ROLFE

JOSEPH ANTHONY GILLET ( 1837-1908)
WILLIAM JAMES ROLFE  (1827-1910)
Copernicus Crater (- 3800m / - 12467ft)
The Moon (Solar System)

In "Astronomy for the use of schools and academies", 1882,
Astronomical photography and ink
The Library of Congress

The site
Copernicus (- 3800m / - 12467ft) is a lunar impact crater located in eastern Oceanus Procellarum. It was named after the astronomer Nicolaus Copernicus (1473-1543). It typifies craters that formed during the Copernican period in that it has a prominent ray system. It may have been created by debris from the breakup of the parent body of asteroid 495 Eulalia 800 million years ago. Copernicus crater is visible using binoculars, and is located slightly northwest of the center of the Moon's Earth-facing hemisphere. South of the crater is the Mare Insularum, and to the south-south west is the crater Reinhold. North of Copernicus are the Montes Carpatus, which lie at the south edge of Mare Imbrium. West of Copernicus is a group of dispersed lunar hills. Due to its relative youth, the crater has remained in a relatively pristine shape since it formed.
The circular rim has a discernible hexagonal form, with a terraced inner wall and a 30 km wide, sloping rampart that descends nearly a kilometer to the surrounding mare. There are three distinct terraces visible, and arc-shaped landslides due to slumping of the inner wall as the crater debris subsided.
Most likely due to its recent formation, the crater floor has not been flooded by lava. The terrain along the bottom is hilly in the southern half while the north is relatively smooth. The central peaks consist of three isolated mountainous rises climbing as high as 1.2 km above the floor. These peaks are separated from each other by valleys, and they form a rough line along an east–west axis. Infrared observations of these peaks during the 1980s determined that they were primarily composed of the mafic form of olivine.
Copernicus H, a typical "dark-halo" crater, was a target of observation by Lunar Orbiter 5 in 1967. Dark-halo craters were once believed to be volcanic in origin rather than the result of impacts. The Orbiter image showed that the crater had blocks of ejecta like other craters of similar size, indicating an impact origin. The halo results from excavation of darker material (mare basalt) at depth. 

The author
William James Rolfe, Litt.D.was an American educator and Shakespearean scholar. Rolfe was born in Newburyport, Massachusetts. He attended Amherst College from 1845 through 1848, but left without graduating after three years due to financial hardship. Amherst, though, nonetheless later awarded him an honorary degree. Between 1852 and 1868, he served as headmaster of high schools at Dorchester, Lawrence, Salem, and Cambridge, Massachusetts. From 1882 to 1887, he served as president of Martha's Vineyard Summer Institute. Early in his career, he edited selections from Ovid and Virgil and (in collaboration) the Cambridge Course of Physics (six volumes, 1867–68). Rolfe's Shakespearean work began with an American edition of George Lillie Craik's English of Shakespeare (3rd revised ed., 1864, , which Crosby and Ainsworth published in 1867.This led to his preparation for Harper & Brothers of a complete edition of Shakespeare – the Friendly Edition (forty volumes, 1870–83; new edition, 1903–07). Rolfe's editions proved to be the best-selling versions in America (during a time of increased use of Shakespeare in high school classrooms) due both to his credentials as a high school administrator and to his use of Bowdlerization of the text in order to remove much of Shakespeare's lewd content. Rolfe also edited a complete edition of Tennyson (twelve volumes, 1898) and verse by many of the other great English poets. He wrote a very useful Satchel Guide to Europe, revised annually for 35 years, and at least five other books.

 
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2022 - Wandering Vertexes...
by Francis Rousseau

AEOLIS MONS OR MOUNT SHARP BY NASA CURIOSITY MISSION

 

NASA CURIOSITY MISSION (since 2012)
Aeolis Mons or Mount Sharp (5, 500 m - 18, 000 ft)
Mars

From "At the base of Aeolis Mons on Mars ", photo, 23 August 2012

The mountain
Aeolis Mons (5, 500 m - 18, 000 ft) also called Mount Sharp is a mountain on the surface of the planet Mars. It forms the central peak within Gale crater and is located around 5.08°S 137.85°E, rising 5.5 km (18,000 ft) high from the valley floor. Aeolis Mons is about the same height as Mons Huygens, the tallest lunar mountain, and taller than Mons Hadley visited by Apollo 15. The tallest mountain known in the Solar System is in Rheasilvia crater on the asteroid Vesta, which contains a central mound that rises 22 km or 22.000 m - 14 mi or 72,000 ft high.
Olympus Mons on Mars is nearly the same height, at 21.9 km (13.6 mi; 72,000 ft) high.
In comparison, Mount Everest / Chomolunga rises to 8.8 km -29,000 ft altitude above sea level, but is only 4.6 km - 15,000 ft base-to-peak. Africa's Mount Kilimanjaro is about 5.9 km - 19,000 ft altitude above sea level also 4.6 km base-to-peak. America's Denali, also known as Mount McKinley, has a base-to-peak of 5.5 km -18,000 ft. The Franco-Italian Mont Blanc/Monte Bianco is 4.8 km -16,000 ft in altitude above sea level. Mount Fuji, which overlooks Tokyo, Japan, is about 3.8 km -12,000 ft altitude. Compared to the Andes, Aeolis Mons would rank outside the hundred tallest peaks, being roughly the same height as Argentina's Cerro Pajonal; the peak is higher than any above sea level in Oceania, but base-to peak it is considerably shorter than Hawaii's Mauna Kea and its neighbors.
Discovered in the 1970s by NAS, the mountain remained nameless for perhaps 40 years. When it became a likely landing site, it was given various labels; for example, in 2010 a NASA photo caption called it "Gale crater mound". In March 2012, NASA unofficially named it "Mount Sharp", for American geologist Robert P. Sharp. The International Astronomical Union, which is responsible for planetary nomenclature for its participants, names large Martian mountains after the Classical albedo feature in which it is located, not for people. In May 2012 the IAU thus named the mountain Aeolis Mons, and gave the name Aeolis Palus to the crater floor plain between the northern wall of Gale and the northern foothills of the mountain. Despite the official name, NASA and the ESA continue to refer to the mountain as "Mount Sharp" in press conferences and press releases
Aeolis is the ancient name of the Izmir region in western Turkey.

The NASA mission
On August 6, 2012, Curiosity (the Mars Science Laboratory rover) landed in "Yellowknife" Quad of Aeolis Palus, next to the mountain. NASA named the landing site Bradbury Landing on August 22, 2012. Aeolis Mons is a primary goal for scientific study.
On June 5, 2013, NASA announced that Curiosity would begin a 8 km (5.0 mi) journey from the Glenelg area to the base of Aeolis Mons.
On November 13, 2013, NASA announced that an entryway Curiosity would traverse on its way to Aeolis Mons was to be named "Murray Buttes", in honor of planetary scientist Bruce C. Murray (1931–2013). The trip was expected to take about a year and would include stops along the way to study the local terrain.
On September 11, 2014, NASA announced that the Curiosity rover had reached Aeolis Mons, the rover mission's long-term prime destination.
On October 5, 2015, possible recurrent slope lineae, wet brine flows, were reported on Mount Sharp near Curiosity.
As of January 20, 2017, Curiosity has been on the planet Mars for 1585 sols (1628 days) since landing on August 6, 2012. 

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2022 - Wandering Vertexes...
by Francis Rousseau

OLYMPUS MONS (ON MARS) PHOTOGRAPHED BY NASA MARS GLOBAL SURVEYOR

NASA MARS GLOBAL SURVEYOR  (1996-2007)
Olympus Mons (21, 230m - 69,650ft)
Mars (Solar system)

The Volcano
Olympus Mons (21, 230m / 21, 2 km-  69,650 ft /1 3 mi) is a very large shield volcano located on the planet Mars,  the largest volcano in the solar system. The massive Martian mountain towers high above the surrounding plains of the red planet, and may be biding its time until the next eruption.By one measure, it has a height of nearly 22 km (13.6 mi). Olympus Mons stands about two and a half times as tall as Mount Everest's height above sea level. It is the youngest of the large volcanoes on Mars, having formed during Mars's Hesperian Period. It had been known to astronomers since the late 19th century as the albedo feature Nix Olympica (Latin for "Olympic Snow"). Its mountainous nature was suspected well before space probes confirmed its identity as a mountain.

The volcano is located in Mars's western hemisphere at approximately 18.65°N 226.2°E, just off the northwestern edge of the Tharsis bulge. The western portion of the volcano lies in the Amazonis quadrangle (MC-8) and the central and eastern portions in the adjoining Tharsis quadrangle (MC-9).

Two impact craters on Olympus Mons have been assigned provisional names by the International Astronomical Union. They are the 15.6 km (9.7 mi)-diameter Karzok crater (18°25′N 131°55′W) and the 10.4 km (6.5 mi)-diameter Pangboche crater (17°10′N 133°35′W). The craters are notable for being two of several suspected source areas for shergottites, the most abundant class of Martian meteorites. Olympus Mons and a few other volcanoes in the Tharsis region stand high enough to reach above the frequent Martian dust-storms recorded by telescopic observers as early as the 19th century. The astronomer Patrick Moore pointed out that Schiaparelli (1835–1910) "had found that his Nodus Gordis and Olympic Snow [Nix Olympica] were almost the only features to be seen" during dust storms, and "guessed correctly that they must be high". The Mariner 9 spacecraft arrived in orbit around Mars in 1971 during a global dust-storm. The first objects to become visible as the dust began to settle, the tops of the Tharsis volcanoes, demonstrated that the altitude of these features greatly exceeded that of any mountain found on Earth, as astronomers expected. Observations of the planet from Mariner 9 confirmed that Nix Olympica was not just a mountain, but a volcano. Ultimately, astronomers adopted the name Olympus Mons for the albedo feature known as Nix Olympica.

The mission
Mars Global Surveyor (MGS) was an American robotic spacecraft developed by NASA's Jet Propulsion Laboratory and launched November 7, 1996. Mars Global Surveyor was a global mapping mission that examined the entire planet, from the ionosphere down through the atmosphere to the surface. As part of the larger Mars Exploration Program, Mars Global Surveyor performed monitoring relay for sister orbiters during aerobraking, and it helped Mars rovers and lander missions by identifying potential landing sites and relaying surface telemetry.
It completed its primary mission in January 2001 and was in its third extended mission phase when, on 2 November 2006, the spacecraft failed to respond to messages and commands. A faint signal was detected three days later which indicated that it had gone into safe mode. Attempts to recontact the spacecraft and resolve the problem failed, and NASA officially ended the mission in January 2007.
The Mars Orbiter Camera (MOC) science investigation used 3 instruments: a narrow angle camera that took (black-and-white) high resolution images (usually 1.5 to 12 m per pixel) and red and blue wide angle pictures for context (240 m per pixel) and daily global imaging (7.5 km per pixel). MOC returned more than 240,000 images spanning portions of 4.8 Martian years, from September 1997 and November 2006.[6] A high resolution image from MOC covers a distance of either 1.5 or 3.1 km long. Often, a picture will be smaller than this because it has been cut to just show a certain feature. These high resolution images may cover features 3 to 10 km long. When a high resolution image is taken, a context image is taken as well. The context image shows the image footprint of the high resolution picture. Context images are typically 115.2 km square with 240 m/pixel resolution.

The Mars Orbiter Laser Altimeter, or MOLA, is an instrument on the Mars Global Surveyor (MGS), a spacecraft that was launched on November 7, 1996. The mission of MGS was to orbit Mars, and map it over the course of approximately 3 years, which it did sucessfully, completing 4 1/2 years of mapping.
Determining the height of surface features on Mars is important to mapping it. To this end, MGS carried a laser altimeter on board. This instrument, MOLA, collected altimetry data until June 30, 2001. MOLA then operated as a radiometer until October 7, 2006.
This website will explain what MOLA is and how it works, and share some of the important discoveries about Mars that have been made using MOLA data.

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2021 - Wandering Vertexes...
by Francis Rousseau

LUNAR CRATER COPERNICUS SKETCHED BY JAMES NASMYTH

JAMES NASMYTH (1808-1890)
Copernicus Crater (- 3800m / - 12467ft)
The Moon (Solar System)

In Drawing of the Copernicus crater on the surface of the Moon, between May 1856 and May 1890, Fitzwilliam Museum, University of Cambridge Nasmyth

The artist
Jamesall Nasmyth (sometimes spelled Naesmyth, Nasmith, or Nesmyth) was a Scottish engineer, artist and inventor famous for his development of the steam hammer. He was the co-founder of Nasmyth, Gaskell and Company manufacturers of machine tools. He retired at the age of 48, and moved to Penshurst, Kent where he developed his hobbies of astronomy and photography.
Nasmyth retired from business in 1856 as he said "I have now enough of this world's goods: let younger men have their chance". He renamed his retirement home "Hammerfield" and happily pursued his various hobbies. He built his own 20-inch reflecting telescope, in the process inventing the Nasmyth focus, and made detailed observations of the Moon. He co-wrote The Moon : Considered as a Planet, a World, and a Satellite with James Carpenter (1840–1899). This book contains an interesting series of "lunar" photographs: because photography was not yet advanced enough to take actual pictures of the Moon, Nasmyth built plaster models based on his visual observations of the Moon and then photographed the models. A crater on the Moon is named after him. In memory of his renowned contribution to the discipline of mechanical engineering, the Department of Mechanical Engineering building at Heriot-Watt University, in his birthplace of Edinburgh, is called the James Nasmyth Building.

The site
Copernicus (- 3800m / - 12467ft) is a lunar impact crater located in eastern Oceanus Procellarum. It was named after the astronomer Nicolaus Copernicus (1473-1543). It typifies craters that formed during the Copernican period in that it has a prominent ray system. It may have been created by debris from the breakup of the parent body of asteroid 495 Eulalia 800 million years ago.  Copernicus crater is visible using binoculars, and is located slightly northwest of the center of the Moon's Earth-facing hemisphere. South of the crater is the Mare Insularum, and to the south-south west is the crater Reinhold. North of Copernicus are the Montes Carpatus, which lie at the south edge of Mare Imbrium. West of Copernicus is a group of dispersed lunar hills. Due to its relative youth, the crater has remained in a relatively pristine shape since it formed.
The circular rim has a discernible hexagonal form, with a terraced inner wall and a 30 km wide, sloping rampart that descends nearly a kilometer to the surrounding mare. There are three distinct terraces visible, and arc-shaped landslides due to slumping of the inner wall as the crater debris subsided.
Most likely due to its recent formation, the crater floor has not been flooded by lava. The terrain along the bottom is hilly in the southern half while the north is relatively smooth. The central peaks consist of three isolated mountainous rises climbing as high as 1.2 km above the floor. These peaks are separated from each other by valleys, and they form a rough line along an east–west axis. Infrared observations of these peaks during the 1980s determined that they were primarily composed of the mafic form of olivine.
Copernicus H, a typical "dark-halo" crater, was a target of observation by Lunar Orbiter 5 in 1967. Dark-halo craters were once believed to be volcanic in origin rather than the result of impacts. The Orbiter image showed that the crater had blocks of ejecta like other craters of similar size, indicating an impact origin. The halo results from excavation of darker material (mare basalt) at depth. 


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2021 - Wandering Vertexes...
by Francis Rousseau

ELYSIUM MONS BY NASA VIKING PROGRAM (1975-1982)

NASA VIKING PROGRAM (1975-1982)
Elysium Mons (13, 900m / 13, 9km - 46,000 ft / 8,6 mi)
MARS

Image from camera B (541A44, 541A46). Red filter used . Resolution is about 144 m/pixel. 

Approximate north is at top. taken on 10 December 1977, USGS Astrogeology Science Center 

The Mountain
Elysium Mons (13,900m / 13, 9km - 46,000 ft / 8,6 mi) is a volcano on Mars located in the volcanic province Elysium, at 25.02°N 147.21°E, in the Martian eastern hemisphere. It stands about above the surrounding lava plains, and about 16 km (52,000 ft) above the Martian datum. Its diameter is about 240 km (150 mi), with a summit caldera about 14 km (8.7 mi) across. It is flanked by the smaller volcanoes Hecates Tholus to the northeast, and Albor Tholus to the southeast.
A 6.5 km diameter crater at 29.674 N, 130.799 E, in the volcanic plains to the northwest of Elysium Mons has been identified as a possible source for the nakhlite meteorites, a family of similar basaltic Martian meteorites with cosmogenic ages of about 10.7 Ma, suggesting ejection from Mars by a single impact event. This implies that Martian volcanism had slowed greatly by that point in history.


The Mission
NASA Viking Orbiter 1 was the first of two spacecraft (along with Viking 2) sent to Mars as part of NASA's Viking program. On July 20, 1976, it became the second spacecraft to soft-land on Mars, and the first to successfully perform its mission. (The first spacecraft to soft-land on Mars was the Soviet Union's Mars 3 on December 2, 1971, which stopped transmitting after 14.5 seconds.) Viking 1 held the record for the longest Mars surface mission of 2307 days (over 6​1⁄4 years) or 2245 Martian solar days, until that record was broken by the Opportunity rover on May 19, 2010. Following launch using a Titan/Centaur launch vehicle on August 20, 1975, and an 11-month cruise to Mars, the orbiter began returning global images of Mars about 5 days before orbit insertion. The Viking 1 Orbiter was inserted into Mars orbit on June 19, 1976, and trimmed to a 1513 x 33,000 km, 24.66 h site certification orbit on June 21. Landing on Mars was planned for July 4, 1976, the United States Bicentennial, but imaging of the primary landing site showed it was too rough for a safe landing. The landing was delayed until a safer site was found, and took place instead on July 20, the seventh anniversary of the Apollo 11 Moon landing. The lander separated from the orbiter at 08:51 UTC and landed at Chryse Planitia at 11:53:06 UTC. It was the first attempt by the United States at landing on Mars.
The instruments of the orbiter consisted of two vidicon cameras for imaging (VIS), an infrared spectrometer for water vapor mapping (MAWD) and infrared radiometers for thermal mapping (IRTM). The orbiter primary mission ended at the beginning of solar conjunction on November 5, 1976.
The extended mission commenced on December 14, 1976, after solar conjunction. Operations included close approaches to Phobos in February 1977. The periapsis was reduced to 300 km on March 11, 1977. Minor orbit adjustments were done occasionally over the course of the mission, primarily to change the walk rate — the rate at which the areocentric longitude changed with each orbit, and the periapsis was raised to 357 km on July 20, 1979. On August 7, 1980, Viking 1 Orbiter was running low on attitude control gas and its orbit was raised from 357 × 33943 km to 320 × 56000 km to prevent impact with Mars and possible contamination until the year 2019. Operations were terminated on August 17, 1980, after 1485 orbits. A 2009 analysis concluded that, while the possibility that Viking 1 had impacted Mars could not be ruled out, it was most likely still in orbit. More than 57,000 images were sent back to Earth. 

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2021 - Wandering Vertexes...
by Francis Rousseau

OZZA MONS PHOTOGRAPHED BY SOVIET VENERA PROGRAM

SOVIET VENERA 13 PROGRAM  (October 1981 - Mars 1982)

Ozza  Mons (No elevation data)

VENUS

The mountain 
Ozza Mons (No elevation data) is an inactive volcano on planet Venus near the equator.  Ozza mons is name after Uzza, a goddess of fertility and venerated femininity in pre-Islamic Arabia. She had her statue in the Kaaba where she was supposed to reside. Four temporally variable surface hotspots were discovered at the Ganiki Chasma rift zone near volcanoes Ozza Mons and Maat Mons in 2015, suggestive of present volcanic activity.  However, interpreting these types of observations from above the cloud layer correctly is a challenge.

The program 
Venera 13 (Венера) , meaning Venus 13) was a probe in the Soviet Venera program for the exploration of Venus. Venera 13 and 14 were identical spacecraft built to take advantage of the 1981 Venus launch opportunity and launched 5 days apart, Venera 13 on 30 October 1981 at 06:04 UTC and Venera 14 on 4 November 1981 at 05:31 UTC, both with an on-orbit dry mass of 760 kg (1,680 lb).As the cruise stage flew by Venus the bus acted as a data relay for the lander and then continued on into a heliocentric orbit. It was equipped with a gamma-ray spectrometer, UV grating monochromator, electron and proton spectrometers, gamma-ray burst detectors, solar wind plasma detectors, and two-frequency transmitters which made measurements before, during, and after the Venus flyby. The bus continued to provide data until at least 25 April 1983.
Leonid Ksanfomaliti of Space Research Institute of the Russian Academy of Sciences (a contributor to the Venera mission) and Stan Karaszewski of Karas, suggested signs of life in the Venera images in an article published in Solar System Research. According to Ksanfomaliti, certain objects resembled a "disk", a "black flap" and a "scorpion" which "emerge, fluctuate and disappear", referring to their changing location on different photographs and traces on the ground.
Engineers familiar with the probe have identified the moving "disk" as actually being the two lens caps ejected from the lander. Rather than a single object that had moved between two different places, they are simply two inanimate similar-looking objects in different places. The other "objects" are ascribed to image processing artifacts and do not appear in the original photography.
The editors of Solar System Research published an editorial comment and a number of commentary articles from other scientists in their September 2012 publication of Issue 5, Volume 46 of the journal. That issue also includes a second article from Ksanfomaliti, in which he claims to identify several other life forms and speculates regarding the apparent rich diversity of life around the landing site.
These claims have been refuted by the Live Science website.

______________________________

2019 - Wandering Vertexes...
by Francis Rousseau

MONS RÜMKER PHOTOGRAPHED BY APOLLO 15 MISSION

APOLLO 15 MISSION (July 26, 1971-August 7. 1971) 

Mons Rümker (1,100m -  3,609 ft) 

The Moon 

This picture of the Mons Rümker was taken from the NASA Apollo 15 mission while in lunar orbit. 

The mountain 
Mons Rümker (1,100m -  3,609 ft) is an isolated volcanic formation that is located in the northwest part of the Moon's near side, at selenographic coordinates 40.8° N, 58.1° W and is the planned landing site of the Chang'e 5 mission. The feature forms a large, elevated mound in the northern part of the Oceanus Procellarum. The mound has a diameter of 70 kilometres, and climbs to a maximum elevation of about 1,100 metres above the surrounding plain. It was named after the german astronomer Karl L. C. Rümker (1788-1822). 

Mons Rümker has a concentration of 30 lunar domes—rounded bulges across the top, some of which contain a small craterlet at the peak.  These are wide, circular features with a gentle slope rising in elevation a few hundred meters to the midpoint. Lunar domes are similar to shield volcanoes, and are the result of lava erupting from localized vents followed by relatively slow cooling.
Mons Rümker is surrounded by a scarp that separates it from the adjacent mare. The plateau rises to an altitude of 900 m in the west, 1,100 m in the south and 650 m in the east. The surface of Mons Rümker is relatively uniform, with a strong spectroscopic signature of lunar mare material. The estimated volume of lava extruded to create this feature is 1,800 km3.

The mission
Apollo 15 was the ninth manned mission in the United States' Apollo program, the fourth to land on the Moon, and the eighth successful manned mission. It was the first of what were termed
"J missions", long stays on the Moon, with a greater focus on science than had been possible on previous missions. It was also the first mission on which the Lunar Roving Vehicle was used.
The mission began on July 26, 1971, and ended on August 7. At the time, NASA called it the most successful manned flight ever achieved.
Commander David Scott and Lunar Module Pilot James Irwin spent three days on the Moon, including 18Ѕ hours outside the spacecraft on lunar extra-vehicular activity (EVA). The mission landed near Hadley rille, in an area of the Mare Imbrium called Palus Putredinus (Marsh of Decay). The crew explored the area using the first lunar rover, which allowed them to travel much farther from the Lunar Module (LM) than had been possible on missions without the rover. They collected 77 kilograms (170 lb) of lunar surface material. At the same time, Command Module Pilot Alfred Worden orbited the Moon, using a Scientific Instrument Module (SIM) in the Service Module (SM) to study the lunar surface and environment in great detail with a panoramic camera, a gamma-ray spectrometer, a mapping camera, a laser altimeter, a mass spectrometer, and a lunar sub-satellite deployed at the end of Apollo 15's stay in lunar orbit (an Apollo program first).
The mission successfully accomplished its objectives. Ironically, this mission was one of very few that had been honored with the issue of a commemorative US stamp, with this first use of a lunar rover happening one decade after the first Mercury astronaut launch.

___________________________________________
2019 - Wandering Vertexes...
by Francis Rousseau

RHEASILVIA PHOTOGRAPHED BY NASA DAWN MISSION (2007-2018)

NASA DAWN MISSION (2007-2018)

Rheasilvia (22,2500 m / 22.5 km - 73,8189 ft / 14 mi) 

Currently the tallest mountain known in the Solar System 

PROTOPLANET VESTA 

About this image

The black-and-white perspective view was made by laying a global image mosaic from Dawn's survey phase (1,700 miles or 2,750 kilometers in altitude) over a topographic shape model. 

The colorized view was made by laying a color-coded height map over the topography. Red indicates higher areas and blue indicates lower areas. 

A still image showing the black-and-white view from the Rheasilvia rim, with the corresponding colorized topography image, is also included here. 

The images used to create these vistas were obtained by Dawn's framing camera from Aug. 11 to Nov. 2, 2011.

The Mountain

Rheasilvia (22,2500 m / 22.5 km - 73,8189 ft / 14 mi) is the tallest mountain known in the Solar System and the most prominent surface feature on the asteroid/ proto planet Vesta. 

Rheasilvia is thought to be an impact crater. It is 505 km (314 mi) in diameter, which is 90% the diameter of Vesta itself, and is 95% the mean diameter of Vesta. However, the mean is affected by the crater itself. It is 89% the mean equatorial diameter of 569 km (354 mi), making it one of the largest craters in the Solar System.  The crater partially obscures an earlier crater, named Veneneia, that at 395 km (245 mi) is almost as large.
Rheasilvia was discovered in Hubble Space Telescope images in 1997, but was not named until the arrival of the Dawn spacecraft in 2011.
It is named after Rhea Silvia, a mythological vestal virgin and mother of the founders of Rome, Romulus and Remus.

The Mission
Dawn is a retired space probe launched by NASA in September 2007 with the mission of studying two of the three known protoplanets of the asteroid belt, Vesta and Ceres. 

It was retired on 1 November 2018 and it is currently in an uncontrolled orbit around its second target, the dwarf planet Ceres. 

Dawn is the first spacecraft to orbit two extraterrestrial bodies, the first spacecraft to visit either Vesta or Ceres, and the first to visit a dwarf planet, arriving at Ceres in March 2015, a few months before New Horizons flew by Pluto in July 2015.
Dawn entered orbit around Vesta on July 16, 2011, and completed a 14-month survey mission before leaving for Ceres in late 2012.It then entered orbit around Ceres on March 6, 2015.

NASA considered, but decided against, a proposal to visit a third target.

On October 19, 2017, NASA announced that the mission would be extended until the probe's hydrazine fuel supply was used up

On November 1, 2018, NASA announced that the Dawn spacecraft had finally exhausted all of its hydrazine fuel, thus ending its mission. The satellite is currently in an uncontrolled state about Ceres.
The Dawn mission was managed by NASA's Jet Propulsion Laboratory, with spacecraft components contributed by European partners from Italy, Germany, France, and the Netherlands. It was the first NASA exploratory mission to use ion propulsion, which enabled it to enter and leave the orbit of two celestial bodies. Previous multi-target missions using conventional drives, such as the Voyager program, were restricted to flybys.

___________________________________________

2019 - Wandering Vertexes...

by Francis Rousseau 

ARSIA MONS BY NASA MARS GLOBAL SURVEYOR

NASA MARS GLOBAL SURVEYOR (1996-2007) 

Arsia Mons (17, 761 m  17 / - 58, 721ft / 11 mi)

MARS 

1. In Arsia Mons Spiral Cloud, June 19, 2001 

2. In Possible caves of Arsia Mons, HiRISE image, Laszlo P. Keszthelyi, August 9, 2007  

The mountain
Arsia Mons (20,000 m / 20 km - 63, 360ft / 12mi) is the southernmost of three volcanos with Ascraeus Mons, and Pavonis Mons (collectively known as Tharsis Montes) on the Tharsis bulge near the equator of the planet Mars, the tallest volcano in the solar system, Olympus Mons, is to its northwest. Arsia Mons was named by Giovanni Schiaparelli after the legendary Roman forest of Arsia Silva.
Arsia Mons is a shield volcano with a relatively low slope and a massive caldera at its summit. It is  large enough to cover the state of New Mexico.

The caldera of Arsia Mons was formed when the mountain collapsed in on itself after its reservoir of magma was exhausted. There are many other geologic collapse features on the mountain's flanks.
The caldera floor formed around 150 millions years ago.
One of the benefits of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) Extended Mission is the opportunity to observe how the planet's weather changes during a second full martian year. The picture  of Arsia Mons  (photo 1 above) was taken June 19, 2001  southern spring equinox occurred the same day. On this particular day (the first day of Spring), the MOC wide angle cameras documented an unusual spiral-shaped cloud within the 110 km (68 mi) diameter caldera- the summit crater- of the giant volcano. Because the cloud is bright both in the red and blue images acquired by the wide angle cameras, it probably consisted mostly of fine dust grains. The cloud's spin may have been induced by winds off the inner slopes of the volcano's caldera walls resulting from the temperature differences between the walls and the caldera floor, or by a vortex as winds blew up and over the caldera. Similar spiral clouds were seen inside the caldera for several days; we don't know if this was a single cloud that persisted throughout that time or one that regenerated each afternoon. Sunlight illuminates this scene from the left/upper left.

Dark pits on some of the Martian volcanoes have been speculated to be entrances into caves . A HiRISE image (cf. photo 2 above), looking essentially straight down, saw only darkness in this pit. This time the pit was imaged from the west. Since the picture was taken at about 2:30 p.m. local (Mars) time,  August 9, 2007, the sun was also shining from the west. We can see the eastern wall of the pit catching the sunlight. This confirms that this pit is essentially a vertical shaft cut through the lava flows on the flank of the volcano. Such pits form on similar volcanoes in Hawaii and are called "pit craters." They generally do not connect to long open caverns but are the result of deep underground collapse. From the shadow of the rim cast onto the wall of the pit NASA could calculate that the pit is at least 178 meters - 584 feet deep. The pit is 150 x 157 meters (492 x 515 feet) across. 

The mission
Mars Global Surveyor (MGS) was an American robotic spacecraft developed by NASA's Jet Propulsion Laboratory and launched November 7, 1996. Mars Global Surveyor was a global mapping mission that examined the entire planet, from the ionosphere down through the atmosphere to the surface. As part of the larger Mars Exploration Program, Mars Global Surveyor performed monitoring relay for sister orbiters during aerobraking, and it helped Mars rovers and lander missions by identifying potential landing sites and relaying surface telemetry.
It completed its primary mission in January 2001 and was in its third extended mission phase when, on 2 November 2006, the spacecraft failed to respond to messages and commands. A faint signal was detected three days later which indicated that it had gone into safe mode. Attempts to recontact the spacecraft and resolve the problem failed, and NASA officially ended the mission in January 2007.
The Mars Orbiter Camera (MOC) science investigation used 3 instruments: a narrow angle camera that took (black-and-white) high resolution images (usually 1.5 to 12 m per pixel) and red and blue wide angle pictures for context (240 m per pixel) and daily global imaging (7.5 km per pixel). MOC returned more than 240,000 images spanning portions of 4.8 Martian years, from September 1997 and November 2006.[6] A high resolution image from MOC covers a distance of either 1.5 or 3.1 km long. Often, a picture will be smaller than this because it has been cut to just show a certain feature. These high resolution images may cover features 3 to 10 km long. When a high resolution image is taken, a context image is taken as well. The context image shows the image footprint of the high resolution picture. Context images are typically 115.2 km square with 240 m/pixel resolution.

___________________________________________

2019 - Wandering Vertexes...

by Francis Rousseau 

ANSERIS MONS BY NASA MARS RECONNAISSANCE ORBITER

NASA MARS RECONNAISSANCE ORBITER (2005-2015)

Anseris Mons (6,200 m -20,300 ft)

MARS 

The mountain

Anseris Mons (6,200 m -20,300 ft) is an isolated massif of mountains in the southern highlands of Mars, located at the northeastern edge of Hellas Planitia at longitude 86.65°E and latitude 29.81°S. The mountain is 58 km (36 mi) in diameter and lies in the southeastern quarter of the Iapygia quadrangle (MC-21), straddling the boundary with the adjoining Hellas quadrangle (MC-28) to the south.,Anseris Mons is named from Anseris Fons, a telescopic albedo feature mapped by Greek astronomer E. M. Antoniadi in 1930. The name was approved by the International Astronomical Union (IAU) in 1991.
Anseris Mons is not a volcano. Geologically, the massif is thought to be the eroded remnant of an ancient crustal block uplifted from depths of several kilometers in the formation of the Hellas impact basin during the period of heavy bombardment. Anseris Mons is the type area for a large set of rugged mountain blocks (>25 km across) that occur in a relatively continuous band 200 to 500 km wide around the western, northeastern, eastern, and southeastern rim of the Hellas basin. Many of the blocks, particularly along the western rim, are concentric with the basin and bounded by faults.
Rocks making up Anseris Mons and other massifs around Hellas are mapped as Noachian in age. However, work by Herbert Frey at NASA’s Goddard Spaceflight Center using Mars Orbital Laser Altimeter (MOLA) data indicates that the southern highlands of Mars contain numerous buried impact basins that are older than the visible Noachian-aged surfaces and which pre-date the Hellas impact. He suggests that the Hellas impact should mark the beginning of the Noachian period (base of the Noachian system). If Frey is correct, then Anseris Mons bedrock is actually pre-Noachian in age, perhaps dating back to over 4.1 billion years ago.
The Anseris Mons massif has undergone a significant amount of erosion since it was uplifted. The flanks of the mountain have huge triangular re-entrants and associated spurs, which give the massif a broad, pyramidal shape. The re-entrants were likely produced through a variety of mass-wasting and periglacial/glacial processes. A large cirque-like re-entrant with channelized debris aprons or fans is present on the south side of the mountain.

USHAS MONS BY NASA MAGELLAN MISSION

MAGELLAN MISSION (1989-1994)

Ushas Mons (2,000 m / 2 km - 6,561ft/1.25 mile)  

VENUS

The mountain 
Ushas Mons (2,000 m / 2 km - 6,561ft/1.25 mile) is a volcano in the southern hemisphere of Venus at 25 degrees south latitude, 323 degrees east longitude. Its name is derived from vedic goddess of dawn Ushas .The volcano is marked by numerous bright lava flows and a set of north-south trending fractures, many of which appear to have formed after the lavas were erupted onto the surface. In the central summit area, however, younger flows remain unfractured. An impact crater can be seen among the fractures in the upper center of the image. The association of faulting and volcanism is common on this type of volcano on Venus, and is believed to result from a large zone of hot material upwelling from the Venusian mantle, a phenomenon known on Earth as a "hotspot."


The mission
Magellan was launched on May 4, 1989, at 18:46:59 UTC by the National Aeronautics and Space Administration from KSC Launch Complex 39B at the Kennedy Space Center in Florida, aboard Space Shuttle Atlantis during mission STS-30. Once in orbit, the Magellan and its attached Inertial Upper Stage booster were deployed from Atlantis and launched on May 5, 1989 01:06:00 UTC, sending the spacecraft into a Type IV heliocentric orbit where it would circle the Sun 1.5 times, before reaching Venus 15 months later on August 10, 1990.
Originally, the Magellan had been scheduled for launch in 1988 with a trajectory lasting six months. However, due to the Space Shuttle Challenger disaster in 1986, several missions, including Galileo and Magellan, were deferred until shuttle flights resumed in September 1988. Magellan was planned to be launched with a liquid-fueled, Centaur-G upper-stage booster, carried in the cargo bay of the Space Shuttle. However, the entire Centaur-G program was canceled after the Challenger disaster, and the Magellan probe had to be modified to be attached to the less-powerful Inertial Upper Stage. The next best opportunity for launching occurred in October 1989.
Further complicating the launch however, was the launching of the Galileo mission to Jupiter, one that included a fly-by of Venus. Intended for launch in 1986, the pressures to ensure a launch for Galileo in 1989, mixed with a short launch-window necessitating a mid-October launch, resulted in replanning the Magellan mission. Weary of rapid shuttle launches, the decision was made to launch Magellan in May, and into an orbit that would require one year, three months, before encountering Venus.
On August 7, 1990, Magellan encountered Venus and began the orbital insertion maneuver which placed the spacecraft into a three-hour, nine minute, elliptical orbit that brought the spacecraft 295-kilometers from the surface at about 10 degrees North during the periapsis and out to 7762-kilometers during apoapsis
On September 9, 1994, a press release outlined the termination of the Magellan mission. Due to the degradation of the power output from the solar arrays and onboard components, and having completed all objectives successfully, the mission was to end in mid-October. The termination sequence began in late August 1994, with a series of orbital trim maneuvers which lowered the spacecraft into the outermost layers of the Venusian atmosphere to allow the Windmill experiment to begin on September 6, 1994.

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2019 - Wandering Vertexes...
by Francis Rousseau 

NEREIDUM MONTES BY ESA MARS EXPRESS

ESA MARS EXPRESS (2003-2020?) 

Nereidum Mons (no elevation data)  

 MARS  (Argyre quadrangle) 

The Mountains 
The Nereidum Montes is a mountain range on planet Mars. It stretches 3,677 km, northeast of Argyre Planitia. It is in the Argyre quadrangle. The mountains are named after a Classical albedo feature.
There is a crater at 45.1°S, 55.0°W on the Nereidum Montes that is similar to Galle in that it also has a smiley face pattern on the crater. However, it is much smaller than Galle itself.
A hummocky relief resembling Veiki moraines has been found in Nereidum Montes. The relief is hypothesized to result very much like Veiki moraines from the melting of a martian glacier.

The mission 
Mars Express is a space probe of the European Space Agency (ESA) launched on June 2, 2003 to study the planet Mars. This is the first exploration mission of another planet in the solar system launched by the European Agency.  Mars Express is developed in a relatively short period of time by partially taking over the architecture of the Rosetta probe while five of the seven instruments were developed for the Soviet Mars 96 probe.
It was launched on June 2, 2003 by a Soyuz rocket and is in orbit around Mars on December 25 of the same year.  Mars Express has obtained many scientific results: determination of the nature of polar ice caps and estimation of the volume of stored water, composition of the Martian atmosphere and its interactions with the solar wind, observation of the seasonal cycle of water , three-dimensional mapping of the reliefs, detection of hydrated minerals proving the presence of water in the past over long periods on the surface and mapping of the regions concerned, detection of the presence of water in the liquid state under the ice cap of the South Pole . The mission of an initial duration of 23 months has been extended several times and must now be completed by the end of 2020.

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2019 - Wandering Vertexes...
by Francis Rousseau 

SOUTH MASSIF BY NASA APOLLO 17 MISSION (1972)

NASA APOLLO 17 MISSION (1972)

 South Massif (2, 300 m - 75, 46ft)

The Moon

1.  In Astronaut Harrison Schmitt next to a large boulder in the Taurus–Littrow valley on the Apollo 17 mission . The South massif is visible to the right. Original NASA caption. 1972

2.  In  South Massif - North facing slope of South Massif, with the 3.6 km diameter Ching-Te crater in the background, Original NASA caption, 1972

The mountain 
South Massif  (2, 300 m - 75, 46ft)  is, according to lunar standards, a relatively modest mountain, but with a rich history (geologic and exploration).  South Massif is located at the edge of the Serenitatis impact basin on the Moon's nearside and borders the Taurus Littrow Valley where the Apollo 17 astronauts landed and explored.
The oblique view (n°2 above) dramatically shows the north-facing slope of South Massif, with the 3.6 km diameter Ching-Te crater in the background. From summit to base, the massif's relief exceeds that of the Grand Canyon.
The distinct high reflectance deposit that spreads across the Taurus Littrow valley floor formed as a giant landslide from the north face of South Massif. Apollo era scientists proposed that the landslide was caused by ejecta from Tycho crater landing on the summit and south side of the massif. The resulting seismic jolt sent regolith sliding down the steep north slope resulting in the distinctive landslide we see today. Look closely at the summit, you can see what appears to be dark and blocky material that may be a deposit of now solidifed impact melt from the Tycho event.  Sampling the landslide was an objective of the Apollo 17 mission. By  determining how long rocks had sat on the surface of the slide scientists could know the timing of the formation of Tycho crater, which is more than 2000 kilometers to the southwest.
As it turns out, the exposure ages of the samples brought back from the landslide were about 110 million years - thus Tycho crater was assigned that age. However, new mapping and analysis of the area brought forward a second hypotheisis, reported this spring at the 49th Lunar and Planetary Science Conference. The alternative idea is that the landslide was caused by motion along the Lee Lincoln fault. It is certainly logical that seismic shaking along such a massive fault could cause a landslide. In fact, the paper (authored by Apollo 17 astronaut Harrison Schmitt) proposes that there were actually two large quakes and thus two landslides, the younger covering most of the older. The older deposit (smaller lobe on the right) is distinguished by its lower reflectance relative to the brighter younger slide (left side). If Dr. Schmitt is correct then we do not know the age of Tycho crater which in turn has implications for how scientists estimate the ages of other young craters across the Moon (and other inner Solar System bodies).

The mission 
Apollo 17 was the final mission of NASA's Apollo program.
Launched at 12:33 a.m. Eastern Standard Time (EST) on December 7, 1972, with a crew made up of Commander Eugene Cernan, Command Module Pilot Ronald Evans, and Lunar Module Pilot Harrison Schmitt, it was the last use of Apollo hardware for its original purpose; after Apollo 17, extra Apollo spacecraft were used in the Skylab and Apollo–Soyuz programs.
Apollo 17 was the first night launch of a U.S. human spaceflight and the final manned launch of a Saturn V rocket. It was a "J-type mission" which included three days on the lunar surface, extended scientific capability, and the third Lunar Roving Vehicle (LRV). While Evans remained in lunar orbit in the Command/Service Module (CSM), Cernan and Schmitt spent just over three days on the Moon in the Taurus–Littrow valley and completed three moonwalks, taking lunar samples and deploying scientific instruments. Evans took scientific measurements and photographs from orbit using a Scientific Instruments Module mounted in the Service Module.
The landing site was chosen with the primary objectives of Apollo 17 in mind: to sample lunar highland material older than the impact that formed Mare Imbrium, and investigate the possibility of relatively new volcanic activity in the same area.  Cernan, Evans and Schmitt returned to Earth on December 19 after a 12-day mission.
Apollo 17 is the most recent manned Moon landing and the most recent time humans travelled beyond low Earth orbit.  It was also the first mission to have no one on board who had been a test pilot; X-15 test pilot Joe Engle lost the lunar module pilot assignment to Schmitt, a scientist.
The mission broke several records: the longest moon landing, longest total extravehicular activities (moonwalks),  largest lunar sample, and longest time in lunar orbit.
Astronaut Eugene A. Cernan, commander, makes a short checkout of the Lunar Roving Vehicle (LRV) during the early part of the first Apollo 17 Extravehicular Activity (EVA-1) at the Taurus-Littrow landing site.

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2019 - Wandering Vertexes...

by Francis Rousseau