View allAll Photos Tagged Chryse
The Mars Pathfinder (MESUR Pathfinder), later renamed the Carl Sagan Memorial Station, is an American spacecraft that landed the first roving probe deployed on another planet. It consisted of a lander and a lightweight (10.6 kilograms/23 pounds) wheeled robotic rover named Sojourner.
Launched on December 4, 1996 by NASA aboard a Delta II booster a month after the Mars Global Surveyor was launched, it landed on July 4, 1997 on Mars' Ares Vallis, in a region called Chryse Planitia in the Oxia Palus quadrangle. The lander then opened, exposing the rover which conducted many experiments on the Martian surface.
The mission carried a series of scientific instruments to analyze the Martian atmosphere, climate, geology and the composition of its rocks and soil. It was the second project from NASA's Discovery Program, which promotes the use of low-cost spacecraft and frequent launches under the motto "cheaper, faster and better" promoted by the then administrator, Daniel Goldin. The mission was directed by the Jet Propulsion Laboratory (JPL), a division of the California Institute of Technology, responsible for NASA's Mars Exploration Program. The project manager was JPL's Tony Spear.
This mission, besides being the first of a series of missions to Mars that included rovers (robotic exploration vehicles), was the most important since the Vikings landed on the red planet in 1976. Although the Soviet Union successfully sent rovers to the Moon as part of the Lunokhod program in the 1970s, its two attempts to send rovers in its Mars probe program failed.
In addition to scientific objectives, the Mars Pathfinder mission was also a "proof-of-concept" for various technologies, such as airbag-mediated touchdown and automated obstacle avoidance, both later exploited by the Mars Exploration Rovers. The Mars Pathfinder was also remarkable for its extremely low price relative to other unmanned space missions to Mars. Originally, the mission was conceived as the first of the Mars Environmental Survey (MESUR) program.
Smithsonian National Air and Space Museum Steven F. Udvar-Hazy Center Virginia
This false color image shows a tributary channel that empties into the main Ares Vallis channel. This tributary channel is located east of Ares Vallis. Located in Margaritifer Terra, Ares Vallis is part of a large system of channels that arise from Vallis Marineris and empty into Chryse Planitia.
The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image.
This martian scene spans 18 x 65 kilometers (11 x 40 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20191216a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
This is the proof test model of the Viking Mars Lander. For exploration of Mars, Viking represented the culmination of a series of exploratory missions that had begun in 1964. The Viking mission used two identical spacecraft, each consisting of a lander and an orbiter. Launched on August 20, 1975 from the Kennedy Space Center in Florida, Viking 1 spent nearly a year cruising to Mars, placed an orbiter in operation around the planet, and landed on July, 20 1976 on the Chryse Planitia. Highlighted in this image is the antenna of the Viking Mars Lander.
For more photography highlights, check out the Air and Space Photo project airandspace.si.edu/albums/air-and-space-photo
This photo is subject to Smithsonian Terms of Use: si.edu/termsofuse
Ipê-amarelo
Classificação científica
Reino: Plantae
Divisão: Magnoliophyta
Classe: Magnoliopsida
Subclasse: Asteridae
Ordem: Lamiales
Família: Bignoniaceae
Género: Tabebuia
Espécie: ver texto
Nome binomial: Tabebuia spp
Ipê-amarelo é o nome popular de algumas espécies de árvores da região Sul e Sudeste do Brasil, pertencentes à família botânica Bignoniaceae, gênero Tabebuia, que também compreende espécies com flores de cor branca, roxa, rosa ou lilás. Em outras regiões brasileiras, os ipês recebem outras denominações.O nome científico Tabebuia, de origem tupi-guarani, significa pau ou madeira que flutua. É denominada, pelos índios, de caxeta, árvore que nasce na zona litorânea do Brasil, cuja madeira íntegra (inatacável) resiste ao apodrecimento.
Entre as epécies conhecidas pelo nome popular Ipê Amarelo estão:
Tabebuia alba, da Mata Atlântica, considerada a árvore símbolo do Brasil.
T. aurea, do cerrado, da caatinga e do Pantanal
T. chrysotricha, da Mata Atlântica
T. ochracea. do cerrado
T. serratifolia, da Amazônia e da Mata Atlântica
T. umbellata, das matas ciliares da Mata Atlântica
T. vellosoi, da Mata Atlântica
T. caraiba Ipê-amarelo-do-cerrado, caroba-do-campo, craibeira
Algumas destas espécies estão ameaçadas:
OUTRAS ESPECIES DE IPES
IPÊ-ROXO ou IPÊ-roxo-da-mata(tabebuia avellandae)
É o primeiro dos Ipês a florir no ano, inicia a floração em Junho, e pode durar até Agosto, conforme a árvore. Esta espécie se confunde bastante com outras também de flor roxa, como a Tabebuia impetiginosa e a Tabebuia heptaphylla, sendo considerado por alguns autores que a T. avellanedae e a T. impetiginosa seriam a mesma espécie. São muito utilizadas no paisagismo urbano, por sua beleza e desenvolvimento
Ipê-Roxo Bola (Tabebuia impetiginosa)
Recebe este nome em razão da forma de seus cachos de flores. Chega a atingir cerca de 8 a 12 metros de altura, dotada de copa alongada, tronco ereto de 60-90 cm de diâmetro com folhas compostas 5-folioladas e quando florido perde suas folhas. É encontrado desde o Piauí até Minas Gerais, Goiás e São Paulo, em geral nas regiões de cerrado e caatinga. Floresce nos meses de maio a agosto. Existem, ainda, outras espécies de ipê roxo, como o T. heptaphylla. Sua Madeira é muito pesada (densidade 0,96g/cm3) muito dura ao corte, resistente ao ataque de organismos xilófagos.
Utilidades
A madeira é apropriada para construções externas, como dormentes, postes etc. Trabalhos de torno, acabamentos internos, como tacos e tábuas para assoalhos, degraus de escada, carrocerias, instrumentos musicais entre outros usos. A Árvore é extremamente ornamental quando em floração prestando-se admiravelmente bem para o paisagismo em geral. Esta é uma das espécies de ipê-roxo mais cultivada para arborização urbana. É também ótima para compor reflorestamentos destinados a recomposição vegetal de áreas degradadas de preservação permanente. Floresce principalmente durante os meses de maio-agosto com a planta totalmente despida de folhagem! Os frutos amadurecem a partir de outubro.
Ipê-rosa(tabebuia pentaphilla)
De crescimento bem rápido em regiões livres de geadas, (em 2 anos ela atinge 3,5 metros), podendo atingir até 35 m. a Tabebuia impetiginosa é originária da Bacia do Paraná. Floresce abundantemente de Junho a Agosto, e prefere climas mais quentes, porem num Inverno seco e ameno, ela oferece também uma linda florada no começo da Primavera. Ideal para áreas isoladas, ou paisagismo de grandes avenidas, o Ipê Rosa prefere solos férteis e bem drenados. Sabe-se que o ipê-roxo é a Tabebuia avellanedae, porém é muito comum haver confusão com a Tabebuia pentaphylla (ipê-rosa).
Totalizam-se 246 espécies de Ipês:
T. acrophylla ,T. actinophylla ,T. acunana ,T. affinis ,T. alba ,T. anafensis ,T. angustata ,T. anisophylla ,T. apiculata ,T. aquatilis ,T. araliacea ,T. arenicola ,T. argentea ,T. arianeae ,T. arimaoensis ,T. aesculifolia ,T. atrovirens ,T. aurea ,T. avellanedae ,T. bahamensis ,T. barbata ,T. berterii ,T. beyeri ,T. bibracteolata ,T. billbergii ,T. botelhensis ,T. brevipes ,T. brigandina ,T. brooksiana ,T. buchii ,T. bullata ,T. bureauvii ,T. bureavii ,T. calcicola ,T. calderoni ,T. calderonii ,T. caleticana ,T. camagueyensis ,T. candicans ,T. capitata ,T. capotei ,T. caraiba ,T. cassinoides ,T. catarinensis ,T. chapadensis ,T. chrysantha ,T. chrysea ,T. chrysotricha ,T. citrifolia ,T. clementis ,T. coartata ,T. conferta ,T. coralibe ,T. cordata ,T. cowellii ,T. crassifolia ,T. crispiflora ,T. cristata ,T. cuneifolia ,T. curtissii ,T. del ,T. densifolia ,T. dentata ,T. dictyophyllaT. diluvialis T. dolichopoda T. domingensis T. dominicensis T. donnell T. donell-smithii T.dracocephaloides T. dubia T. dugandii T. dura T. ecuadorensis T. ekmanii T. elegansT. ellipticaT. eT. fallax T. flavescens T. floccosa T. fluviatilis T. furfuraceaT. fuscata T. gemmifloraT. geroT. glaucescens T. globiflora T. glomerata T. gonavensisT. gracilipes T. grisebachiiT. guayacan T. haemantha T. heptaphylla T. heterophylla T. heteropoda T. heterotricha T. hotteana T. hypodictyon T. hypolepra T. hypoleuca T. ilicifolia T. impetiginosaT. inaequipes T. incana T. insignis T. ipe T. jackiana T. jamaicensisT. japurensis T. jaucoensis T. jojoana T. lanceolata T. lapacho T. latifolia T. lapacho T. latifolia T. leonis T. lepidophylla T. lepidota T. leptoneura T. leptopoda T. leucoxyla T. libanensis T. lindahlii T. linearis T. litoralis T. longiflora T. longpes T. lopezii T. lucida T. magnolioides T. mansoana T. maestrensis T. maxonii T. mexicana T. micrantha T. microphylla T. millsii T. moaensis T. mogotensis T. multinervis T. myrtifolia T. neochrysantha T. nervosa T. neurophylla T. nicaraguensis T. nigripes T. nipensis T. nivea T. nodosa T. obovata T. obscura T. obtusifolia T. ochracea T. odontodiscus T. oligolepis T. ophiolithica T. ophiticola T. orinocensis T. ostenfeldii T. ovatifolia T. pachyphylla T. pallida T. palmeri T. palustris T. paniculata T. papyrophloios T. pedicellata T. pentaphylla T. perelegans T. perfae T. pergracilis T. petrophila T. picotensis T. pilosa T. pinetorum T. pisoniana T. piutinga T. platyantha T. polyantha T. polymorpha T. potamophila T. pulcherrima T. pulverulenta T. pumila T. punctatissima T. pyramidata T. reticulata T. revoluta T. ricardii T. richardiana T. rigida T. riodocensis T. riparia T. roraimae T. rosea T. roseo-alba T. rubriflora T. rufescens T. rufinervis T. rugosa T. sagraei T. samanensis T. sanguinea T. sauvallei T. savannarum T. saxicola T. schumanniana T. schunkevigoi T. selachidentata T. serratifolia T. sessifolia T. sessilifolia T. setulosa T. shaferi T. simplicifolia T. speciosa T. spectabilis T. spongiosa T. stenocalyx T. striata T. subcordata T. suberosa T. subsessilis T. subtilis T. tortuensis T. trachycarpa T. trinitensis T. triorbicularis T. triphylla T. truncata T. turquinensis T. uleana T. uliginosa T. umbellata T. vellosoi T. vinosa T. wrightii T. xanthophylla T. zanonii T. zolyomiana
O ipê e a Lei, no Brasil
Embora o ipê seja considerado árvore símbolo do Brasil, pela Lei 6.607 de 7 de Dezembro de 1978 o pau-brasil foi declarado Árvore Nacional.
Pelos projetos de lei PL-2293/1974 e PL-882/1975, tentou-se instituir a flor do ipê como flor nacional do Brasil. Ambos os projetos foram arquivados na Câmara dos Deputados. O projeto de lei PL-3380/1961 visava declarar o pau-brasil e o ipê-amarelo, respectivamente, Árvore e Flor Nacionais, mas este projeto não foi aprovado.
Created by Wikipedia's Ittiz and taken from Wikimedia, this is the artist's conception of a terraformed Mars. This portrayal is approximately centered on the prime meridian and 30° North latitude, and a hypothesized ocean with a sea level at approximately two kilometers below average surface elevation. The ocean submerges what are now Vastitas Borealis, Acidalia Planitia, Chryse Planitia, and Xanthe Terra; the visible landmasses are Tempe Terra at the left, Aonia Terra at the bottom, Terra Meridiani at the lower right, and Arabia Terra at the upper right. Rivers that feed the ocean at the lower right occupy what are now Valles Marineris and Ares Vallis, while the large lake at the lower right occupies what is now Aram Chaos.
Today's VIS image shows a portion of Kasei Valles. Kasei Valles is one of the largest outflow channel systems on Mars, in places up to 482 km (300 miles) wide and 1580 km (982 miles) long. For comparison, the Grand Canyon in Arizona is is only 29 km (18 miles) at its widest and only 446 km (277 miles) long. Kasei Valles flows eastward through Lunae Planum and empties into Chryse Planitia.
This martian scene spans 19 x 283 kilometers (12 x 176 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20210810a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Today's VIS image shows a portion of Kasei Valles. Kasei Valles is one of the largest outflow channel systems on Mars, in places up to 482 km (300 miles) wide and 1580 km (982 miles) long. For comparison, the Grand Canyon in Arizona is is only 29 km (18 miles) at its widest and only 446 km (277 miles) long. Kasei Valles flows eastward through Lunae Planum and empties into Chryse Planitia.
This martian scene spans 19 x 280 kilometers (12 x 174 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20220216a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Agamemnon gathered the reluctant Greek forces to sail for Troy. Preparing to depart from Aulis, which was a port in Boeotia, Agamemnon's army incurred the wrath of the goddess Artemis. There are several reasons throughout myth for such wrath: in Aeschylus' play Agamemnon, Artemis is angry for the young men who will die at Troy, whereas in Sophocles' Electra, Agamemnon has slain an animal sacred to Artemis, and subsequently boasted that he was Artemis's equal in hunting. Misfortunes, including a plague and a lack of wind, prevented the army from sailing. Finally, the prophet Calchas announced that the wrath of the goddess could only be propitiated by the sacrifice of Agamemnon's daughter Iphigeneia. Classical dramatizations differ on how willing either father or daughter were to this fate, some include such trickery as claiming she was to be married to Achilles, but Agamemnon did eventually sacrifice Iphigeneia. Her death appeased Artemis, and the Greek army set out for Troy. Several alternatives to the human sacrifice have been presented in Greek mythology. Other sources claim that Agamemnon was prepared to kill his daughter, but that Artemis accepted a deer in her place, and whisked her to Taurus in Crimea. Hesiod said she became the goddess Hecate.
Agamemnon was the commander-in-chief of the Greeks during the Trojan War. During the fighting, Agamemnon killed Antiphus. Agamemnon's teamster, Halaesus, later fought with Aeneas in Italy. The Iliad tells the story of the quarrel between Agamemnon and Achilles in the final year of the war. Agamemnon took an attractive slave and spoil of war Briseis from Achilles. Achilles, the greatest warrior of the age, withdrew from battle in revenge and nearly cost the Greek armies the war.
Although not the equal of Achilles in bravery, Agamemnon was a dignified representative of kingly authority. As commander-in-chief, he summoned the princes to the council and led the army in battle. He took the field himself, and performed many heroic deeds until he was wounded and forced to withdraw to his tent. His chief fault was his overwhelming haughtiness. An over-exalted opinion of his position led him to insult Chryses and Achilles, thereby bringing great disaster upon the Greeks.
After the capture of Troy, Cassandra, doomed prophetess and daughter of Priam, fell to Agamemnon's lot in the distribution of the prizes of war.
From en.wikipedia.org/
Today's VIS image shows a section of Bahram Vallis. This channel is located in northern Lunae Planum, south of Kasei Valles. Bharam Vallis drains from the higher elevations of Lunae Planum towards the Chryse Planitia basin. This channel is over 300km long (186miles).
This martian scene spans 19 x 66 kilometers (12 x 41 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20220331a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Light-Toned Fan-Like Features in a Crater in Chryse Chaos
NASA/JPL/University of Arizona (Less than 5 km across; www.uahirise.org/ESP_013256_1885)
This is the proof test model of the Viking Mars Lander. For exploration of Mars, Viking represented the culmination of a series of exploratory missions that had begun in 1964. The Viking mission used two identical spacecraft, each consisting of a lander and an orbiter. Launched on August 20, 1975 from the Kennedy Space Center in Florida, Viking 1 spent nearly a year cruising to Mars, placed an orbiter in operation around the planet, and landed on July, 20 1976 on the Chryse Planitia. Highlighted in this image is the gas chromatograph — mass spectrometer of the Viking Mars Lander.
For more photography highlights, check out the Air and Space Photo project airandspace.si.edu/albums/air-and-space-photo
This photo is subject to Smithsonian Terms of Use: si.edu/termsofuse
“VIKING 1 PRIMARY LANDING SITE”
“The ellipse above indicates the planned primary landing site for Viking Lander 1 when it touches down on Mars in the summer of 1976 to begin a detailed scientific examination of the planet, including a search for life. The site is in a region of Mars called Chryse, at the mouth of a 3,000 mile (4,800 km) long rift canyon. The target ellipse is approximately 300 x 80 kilometers (180 x 48 miles). The target coordinates are 19.5 degrees North and 34 degrees West. The photograph is of a 1:1,000,0-00 scale topographic map.”
Interestingly, the ellipse encompasses the 1997 Mars Pathfinder landing site.
NASA has selected an ancient flood plain on Mars as the landing site for the 1996 mission of Mars Pathfinder, one of the first in a new generation of small, low-cost spacecraft. Eons ago, when water flowed on Mars, great floods inundated the landing site, located on a rocky plain in an area known today as Ares Vallis. The site is 850 kilometers (527 miles) southeast of the location of Viking Lander 1, which in 1976 became the first spacecraft to land on Mars. Pathfinder will be the first to land on Mars since the twin Viking landers arrived almost 20 years ago. The spacecraft, scheduled to arrive at Mars on July 4, 1997, will parachute down to Ares Vallis at the mouth of an ancient outflow channel chosen for the variety of rock and soil samples it may present. The target landing site, at the center of the landing ellipse, is 19.5 N, 32.8 W.
From the indomitable LPI:
The Mars Pathfinder spacecraft landed near the center of this ellipse, as planned, on July 4, 1997. The ellipse is the original target area, 300 kilometers long and 200 kilometers wide. Mars Pathfinder landed only 50 kilometers from the ellipse center. This landing site is outside the mouth of the huge water-cut channel of Ares Vallis (19.33°N, 33.55°W) that empties into the lowlands of Chryse Planitia near the Viking 1 lander site. At its landing site, Pathfinder and its rover were able to see and analyze rocks that were washed down Ares Vallis during its floods. These rocks could come from the ancient southern highlands and from plains that are huge basalt lava flows.
This landing site was chosen in April 1994, when 60 scientists gathered at the Lunar and Planetary Institute in Houston. Their goal was to find sites where Mars Pathfinder could land and survive (flat surface, low elevation, latitude between 5° and 20°N), and return important information. Each scientist had a favorite site, and the Pathfinder program managers considered them all. Ares Vallis was chosen because it seemed relatively safe (flat and low), was known fairly well (the Viking spacecraft had taken detailed images of the area), and probably would provide important rock samples for Pathfinder to view and analyze.
Also:
nssdc.gsfc.nasa.gov/planetary/image/marspsite.gif
www.lpi.usra.edu/publications/slidesets/marslife/slide_36...
Dramatic flood events carved this impressive channel system on Mars covering 1.55 million square kilometers, shown here in a stunning new mosaic from ESA’s Mars Express. The mosaic, which features the spectacular Kasei Valles, comprises 67 images taken with the spacecraft’s high-resolution stereo camera and is released during the week of the 10th anniversary of the spacecraft’s launch to the Red Planet.
Kasei Valles is one of the largest outflow channel systems on Mars – from source to sink, it extends some 3000 km and descends by 3 km in altitude. The scene covered in the mosaic spans 987 km north–south (19–36°N) and 1550 km east–west (280–310°E). The channel originates beyond the southern edge of this image near Valles Marineris, and empties into the vast plains of Chryse Planitia to the east (right).
Today's VIS image shows part of Maja Valles, a large channel system in Lunae Planum. The main part of the channel is visible at the upper left in this image. The lower part of the image is located within an old crater called Stege Crater. The channel in the central part of the image is flowing along the inner rim of the crater and into the main Maja Valles channel just off the image to the left. Maja Valles in 1600 km (1000 miles) long. Like most outflow channels in the region, Maja Valles arises from Valles Marineris and drains into Chryse Planitia. Maja Valles starts in Juventae Chasma.
This martian scene spans 18 x 65 kilometers (11 x 40 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20191129a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
This spectacular picture of the Martian landscape by the Viking 1 Lander shows a dune field with features remarkably similar to many seen in the deserts of Earth. The dramatic early morning lighting - 7:30 a.m. local Mars time--reveals subtle details and shading. Taken 3 August 1976 by camera number 1, the picture covers 100 degrees, looking northeast at left and southeast at right. Viking scientists have studied areas very much like the one in this view in Mexico and in California (Kelso, Death Valley, Yuma). The sharp dune crests indicate the most recent wind storms capable of moving sand over the dunes in the general direction from upper left to lower right. Small deposits downwind of rocks also indicate this wind direction. Large boulder at left, nicknamed ‘Big Joe’, is about eight meters (25 feet) from the spacecraft and measures about one by three meters (3 by 10 feet). The meteorology boom, which supports Viking s miniature weather station, cuts through the picture’s center. The sun rose two hours earlier and is about 30 degrees above the horizon near the center of the picture. Features on the horizon are about 3 kilometers (1.86 miles) away.
photojournal.jpl.nasa.gov/catalog/PIA00393
Credit: JPL/NASA
My 1st Mars with surface detail, mediocre seeing, Questar 3.5, 16 mm Brandon, Sony NEX-5N eyepiece projection. 20 images stacked and sharpened. Diameter is 13 arc seconds. The north polar ice cap is the slightly brighter spot at the bottom around 5 o’clock. The globe is centered on about 40W. The lighter area cutting from 1 to 8 o’clock is centered on Chryse, with Mare Acidalium adjoining the north ice cap, and Mare Erythraeum, the dark area in the south (11 o’clock). The large area of glare (sun on high clouds?) near 1 o’clock is to the right of the location of Valles Marineris (not resolved here - the grand canyon of Mars).
Today's VIS image shows part of Lobo Vallis and Kasei Valles. This image is located where Kasei Valles splits to circle around Sharonov Crater, creating Lobo Vallis. Lobo Vallis flows around the northern side of the crater, with the main Kasei Valles channel flowing along the south side. The two channel segments recombine prior to emptying into Chryse Basin.
This martian scene spans 19 x 282 kilometers (12 x 175 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20251016a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Closeup of Viking 1 lander's surface sampler collector head.
See also:
photojournal.jpl.nasa.gov/catalog/PIA00395
Credit: JPL Photojournal website
The worship of Apollo Smintheus (or Apollo Sminthius) extended only to Asia Minor and not the Greek mainland. Alexandria in Troas was the center of this cult. This is one of the strongest arguments for the thesis that the origin of the Apollo cult was Asia minor.
After the fall of Troy the Greeks start to spread to the East. They settled on the Aegean islands and the western coast of Asia Minor. The worship of Apollo in this region had a curious origin. When the old Teukri under their king Teucer came from Crete to the coast of Asia Minor, the oracle told them to stay there where they could see their enemies creeping out of the ground. When they came to Hamaxitos, a city in this region, the mice creeping out of the ground gnawed on their shields during the night. So they saw the oracle of the god fulfilled, settled down and erected a statue of Apollo with a mouse laying at his feet, which in the Aeolian dialect was called Smintha. (Ovid Met. II, 5685)
There are known two different versions of Apollo Smintheus depictions:
1. A cult statue where he stands facing front holding a mouse in his hand. This version is characteristic of Alexandria in Troas. The fact that the statue is held by the Genius of the city may be an allusion that the temple of Apollo got governmental benefits. (Pat Lawrence)
2. A cult statue where Apollo is standing left and has a mouse under his foot. In Chryse there was a statue made by Scopas, showing exactly this position. This statue is depicted on coins.
The meaning of the epithet 'Smintheus' is interpreted different ways:
1. The origin of the name is the city of Sminthe in Troas, where Apollo was worshippedin pre-Hellenic times. So Apollo Smintheus = Apollo from Sminthe.
2. In the Aeolian dialect 'smintha' means 'mouse'. So Apollo Smintheus = the mice-god. The mouse in ancient times was a symbol of prophetic power because it was thought mice were inspired by the exhaling coming out of the ground.
3. Apollo the mice-killer. The Greek already had recognized the mice as vermin and worshipped Apollo as protector against mice.
The second explanation seems the most probable. It is unlikely the Greeks might have identified mice as carriers of plagues because they would have been incorrect. It is the rat flea that carries plague. The mouse is innocent.
The first mention of Apollo Smintheusis found in Homer's Ilias I, 39. The beginning of the Ilias describes how Apollo strikes the Greeks with a plague because Agamemnon has raped Chrysis, the daughter of Apollo's priest Chryses, and so has humiliated his priest.
The old man, afraid, obeyed his words, walked off in silence,
along the shore by the tumbling, crashing surf.
Some distance off, he prayed to Lord Apollo,
Leto's fair-haired child:
"God with the silver bow,
protector of Chryse, sacred Cilla, 40
mighty lord of Tenedos, Sminthean Apollo,
hear my prayer: If I've ever pleased you
with a holy shrine, or burned bones for you— [40]
bulls and goats well wrapped in fat—
grant me my prayer. Force the Danaans
to pay full price for my tears with your arrows."
So Chryses prayed. Phoebus Apollo heard him.
He came down from Olympus top enraged,
carrying on his shoulders bow and covered quiver,
his arrows rattling in anger against his arm. 50
So the god swooped down, descending like the night.
He sat some distance from the ships, shot off an arrow—
the silver bow reverberating ominously.
First, the god massacred mules and swift dogs, [50]
then loosed sharp arrows in among the troops themselves.
Thick fires burned the corpses ceaselessly.
Every day, a camera on board the Mars Reconnaissance Orbiter captures a view of the planet’s global weather patterns.
For the last week of August, this report came in from Martian meteorologists (well, they’re Earthlings who study Martian weather): “While the early part of this past week on Mars continued with the dusty pattern of the previous few weeks, storm activity died down later in the week. A large dust storm occurred over Chryse on the 22nd, along with smaller dust storms over Utopia and Elysium and dust activity over the Phlegra Montes/Arcadia/Northern Amazonis region. By the next day, these storms had diminished to dust haze. Water ice clouds remained concentrated predominantly over Tempe and Acidalia early in the week, becoming more diffuse and streaking across much of the northern mid-latitudes as the week progressed.”
See a movie of weather during this time period.
Sent by: Mars Reconnaissance Orbiter | From: Mars | Released: August, 2011 | Credit: NASA/JPL/Malin Space Science Systems | Image source | Added to Riding with Robots on September 6, 2011
Viking 1 orbiter photo, probably taken prior to the landing, as part of final site reconnaissance, suitability evaluation/determination and confirmation. The region is approximately 80 kilometers due west of the actual landing site, in the Xanthe Dorsa region within Chryse Planitia. North is roughly to the upper left of the photo.
For context, see:
history.nasa.gov/SP-441/p162.htm
The crater at the top of the photo is the crater to the right of the "H" in "XANTHE DORSA" (at the above link).
Today's VIS image shows a portion of Kasei Valles. Kasei Valles is one of the largest outflow channel systems on Mars, in places up to 482 km (300 miles) wide and 1580 km (982 miles) long. For comparison, the Grand Canyon in Arizona is is only 29 km (18 miles) at its widest and only 446 km (277 miles) long. Kasei Valles flows eastward through Lunae Planum and empties into Chryse Planitia.
This martian scene spans 19 x 278 kilometers (12 x 173 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20251013a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Today's VIS image shows a small portion of Lobo Vallis near where it recombines with Kasei Valles and empties into Chryse Planitia. Kasei Valles is a huge channel system that drained the higher elevations of Tharsis into the low of Chryse Planitia.
The streamlines in the image are scour marks left by the giant floods that poured down the channel.
This martian scene spans 19 x 68 kilometers (12 x 42 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20180420a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu.
This image is in the public domain and may be republished free of charge, but if used it should be credited as NASA/JPL-Caltech/Arizona State University.
Today's VIS image shows a small section of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. This channel, and all others in this region, drain into Chryse Planitia.
This martian scene spans 18 x 65 kilometers (11 x 40 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200416a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Similar HiRISE images of mounds around Chryse Planitia have revealed stunning and complex meter and decameter-scale stratigraphy, indicative of widespread, regional-scale processes. These mounds share characteristics with those landforms, so it is important to document.
Image cutout is less than 5 km (3 mi) across and the spacecraft altitude was 289 km (180 mi). For full observation details including images with scale bars, visit the source link.
www.uahirise.org/ESP_074074_2040
NASA/JPL-Caltech/UArizona
Edited Mars Reconnaissance Orbiter image of a small mound (for unmeasured amounts of "small") mound in Chryse Planitia. Inverted grayscale variant (which makes it a lot easier to make out the details).
This VIS image shows a section of Shalbatana Vallis. Shalbatana Vallis is located in Xanthe Terra and is one of many channels that empty into Chryse Planitia.
This martian scene spans 18 x135 kilometers (11 x 84 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200217a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
Today's VIS image shows a section of Bahram Vallis. This channel is located in northern Lunae Planum, south of Kasei Valles. Bharam Vallis drains from the higher elevations of Lunae Planum towards the Chryse Planitia basin. This channel is over 300km long (186miles). In this image Bahram Vallis enters Waspam Crater (right side of image) and then exits the crater (top right corner).
This martian scene spans 19 x 66 kilometers (12 x 41 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200622a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.
"The patch of dark material toward the top of this picture (arrow) taken by the Viking 1 Lander is the debris kicked up by the impact of a protective cover ejected from the spacecraft at 1 a.m. today. The cylindrical cover, which bounced out of view of the camera, protects the scoop at the end of the soil sampler arm. (The scoop will dig into the Martian surface for the first time on July 28). Dust and debris atop the footpad remains as it was seen in the Lander's first picture taken immediately after landing two days ago. No wind modification is apparent. On the surface, a variety of block sizes, shapes and tones are seen, and some rocks are partially buried."
Also at:
photojournal.jpl.nasa.gov/catalog/PIA00384
Credit: JPL Photojournal website
The brighter region at the bottom of this VIS image is the relative highlands of Arabia Terra, while the rest of the image shows Chryse Plainitia. The boundary between the two regions is a large change in elevation as well as differences in surface texture.
The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image.
This martian scene spans 19 x 283 kilometers (12 x 176 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20190226a
See the Red Planet Report at redplanet.asu.edu for updates on Mars research and exploration. For more about Mars geology, check out the Mars-ePedia: marsed.asu.edu/marsepedia
For the latest THEMIS Mars images as received by mission scientists, see themis.asu.edu/livefrommars. To learn more about the THEMIS camera and its Mars images, see themis.asu.edu.
This image is in the public domain and may be republished free of charge. If used, please credit it as NASA/JPL-Caltech/Arizona State University.