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A tiny stuffed mouse serves time in the museum at the temple of Apollo Smintheus at ancient Chryse in the Troad. The temple of Apollo Smintheus is most famous as the scene of the first action in Homer's Iliad. The temple is situated on the southwestern corner of the Biga peninsula and was constructed in the 2nd century. The temple is an 8 x 14 Ionic pseudodipteros . The exposed stylobate measures 24 x 43 meters and the temple is elevated on an 11 step krepidoma.
Smintheus is an epithet of Apollo which means "lord of mice". Teucer, a legendary Cretan hero, left the island with his father (Scamander) and a band of followers during a period of famine. An oracle told them they should settle at the place where they were attacked by "sons of the earth." When they woke up one morning and found that their armor had been eaten by mice, they decided that they must have arrived. They built a settlement and erected a temple to Apollo Smintheus.
Chapim-de-poupa
Serra do Mendro-Portel-Portugal
1.12.2007
Com um abraço ao operacional Duriense dos GOEF Jorge Monteiro , que hoje andou todo o dia á chuva por terras de Chrysea...
Viking 1 landed near two outflow channels that emptied into Chryse Planitia. Floodwaters from these channels probably flowed over this site. Later the martian winds formed dunes in the area. This corrected version of the scene allows the viewer to scan most of the scene in front of the lander. Several small ridges now stand out sharply in the middle foreground. This view exaggerates the relief. In some areas, the horizon may actually appear nearer than the foreground objects.
Mars, London UK, 28 March 2012, ~00:30 hours. Animation of 11 frames
taken over ~ 45 minutes
FoV: North Polar cap at the 11 o'clock position.
North hemisphere features are the Mare Acidalium (large dark patch), and
Tempe (circular orange patch at the 9 o'clock position).
South hemisphere features are the Mare Erythraeum (5 o'clock). The spike
pointing up toward the Mare Acidalium is the Oxia Palus.
The orange bit separating the Mare Acidalium and Mare Erythraeum is Chryse.
The large orange expanse to the upper right of Chryse is Eden.
Scope - 15cm newtonian, 3x barlow, 25mm eyepiece projection, ~10cm
projection length
Camera - Samsung SDC435, IR block filter, 1/100 sec exposure
Processing - about 3,000 frames stacked each pic (from a 2-3 minute video avi) using Registax 6, wavelets-histogram-colour balance. Post processing in Photoshop Elements (high pass masking, gausian blur, levels)
Today's false-color VIS image is located in the plains between Chryse and Acidalia Planitias.
Dark blue tones in this false color combination are usually created by basaltic sands. There appears to be surface sands in the middle of the image. The "orange" tail behind the crater towards the top of the image is created by wind action.
Wind will both erode and deposit fine materials. The wind tail is the downward side of the crater. These features are termed windstreaks, and they help to understand the direction of wind.
Both the windstreak and the surface sands indicate a dusty/sandy region confined to the central part of this image.
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 290 kilometers (12 x 180 miles). To see where on Mars this area lies, and to download high-resolution versions of the image, go to themis.asu.edu/zoom-20190412a
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.
Day 25 of 365 - March 29th, 2012
I set up my refractor this evening to take a glimpse at Mars in the Constellation Leo. The seeing was not the best, but I was able to bump up the power to 220x magnification and take in views of Acidalia, Chryse, Valles Marineris and the North Polar Ice Cap during periods of steady seeing. Mars really takes high magnification well and is my favorite planet to observe next to Jupiter. The picture shows my favorite planetary eyepieces (University Optics Orthoscopics) setting on my Pocket Atlas sky chart. There is nothing more relaxing after a long day at work than kicking back and observing the night sky.
Olympus OM Zuiko 50mm f1.8 (1/25, f2.8, ISO 100)
A sign at the Temple of Apollo Smintheus at ancient Chryse in the Troad proclaims the sponsorship of Efes beer. The temple is an 8 x 14 Ionic pseudodipteros . The exposed stylobate measures 24 x 43 meters, and the remains are surrounded by fragments of sculpture, inscriptions, and Turkish tombstones.
Smintheus is an epithet of Apollo which means "lord of mice". Teucer, a legendary Cretan hero, left the island with his father (Scamander) and a band of followers during a period of famine. An oracle told them they should settle at the place where they were attacked by "sons of the earth." When they woke up one morning and found that their armor had been eaten by mice, they decided that they must have arrived. They built a settlement and erected a temple to Apollo Smintheus.
This photo mosaic displays an area of typical outflow channel terrain in the Chryse Plain region of Mars. Landforms such as streamlined islands indicate that the flow here was generally from south to north. The overlay of southern California is shown at the same scale. Prepared for NASA by Stephen Paul Meszaros.
This photo mosaic displays an area of typical outflow channel terrain in the Chryse Plain region of Mars. Landforms such as streamlined islands indicate that the flow here was generally from south to north. The overlay of the State of California is shown at the same scale. Prepared for NASA by Stephen Paul Meszaros.
Today's VIS image shows part of Hydaspis Chaos, one of many regions of chaos in Margaritifer Terra. Chaos terrain is typified by mesas and valleys. The initial breakup of the surface can be due to tectonic forces, although on Mars it is thought that the mode of formation involves release of melted subsurface ice. With time and erosion the valleys widen and the mesas grow smaller. Hydaspis Chaos is is part of the huge outflow system flowing from Valles Marineris to Chryse Planitia. The channel in the center of the image becomes part of the larger Tiu Valles channel.
This martian scene spans 18 x 271 kilometers (11 x 169 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20220406a
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 photo mosaic displays an area of typical outflow channel terrain in the Chryse Plain region of Mars. Landforms such as streamlined islands indicate that the flow here was generally from south to north. The overlay of the State of Arizona is shown at the same scale. Prepared for NASA by Stephen Paul Meszaros.
Edited Mars Reconnaissance Orbiter image of mounds in Chryse Planitia. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA22682
Original caption: This image was acquired on May 15, 2018 by NASA's Mars Reconnaissance Orbiter. This observation shows relatively bright mounds scattered throughout darker and diverse surfaces in Chryse Planitia. These mounds are hundreds of meters in size. The largest of the mounds shows a central pit, similar to the collapsed craters found at the summit of some volcanoes on Earth. The origins of these pitted mounds or cratered cones are uncertain. They could be the result of the interaction of lava and water, or perhaps formed from the eruption of hot mud originating from beneath the surface.
These features are very interesting to scientists who study Mars, especially to those involved in the ExoMars Trace Gas Orbiter mission. If these mounds are indeed mud-related, they may be one of the long sought after sources for transient methane on Mars.
The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 60.5 centimeters (23.8 inches) per pixel (with 2 x 2 binning); objects on the order of 181 centimeters (71.3 inches) across are resolved.] North is up.
The University of Arizona, Tucson, operates HiRISE, which was built by Ball Aerospace & Technologies Corp., Boulder, Colorado. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the Mars Reconnaissance Orbiter Project for NASA's Science Mission Directorate, Washington.
Image Credit:
NASA/JPL-Caltech/Univ. of Arizona
Image Addition Date:
2018-09-04
Image taken in fair seeing, cloud over Olympus Mons centre and Tharsis volcanoes and Chryse extreme right.
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. Today's false color image shows a small section of Mawrth Vallis (near the top of the image). Of all the channels carved by flowing water on Mars, one of the more unusual is Mawrth Vallis, whose name comes from the Welsh word for Mars. Mawrth winds through northwest Arabia Terra for some 640 kilometers (400 miles) before emptying into Acidalia Planitia on the edge of the vast northern lowlands. Unlike many outflow channels that start in regions of chaotic terrain, Mawrth Vallis just appears and then grows deeper as it heads downstream, holding a width of approximately 15 km (9 mi) until it widens near its mouth at 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-20200827a
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 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. Shalbatana Vallis is 1029km long (639 miles).
This martian scene spans 18 x 274 kilometers (11 x 170 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20200917a
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 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-20260102a
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 Kasei Valles. This complex channel arose in the Tharsis voclanic region and flowed eastward into Chryse Planitia. Chryse Planitia is a large circular basin, probably formed by a meteor impact.
This martian scene spans 19 x 68 kilometers (11 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-20200429a
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, just at the region where the northward flow of the channel turns eastward towards it's eventual end in Chryse Planitia. 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.
This martian scene spans 19 x 67 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-20200311a
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 (186 miles) long.
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-20230731a
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.
These thick clouds in the western Chryse Planitia region of Mars are dust clouds. Most northern hemisphere storms spread only a few hundred kilometers, but occasionally dust storms can encircle the entire planet.
The partially reconstructed stylobate, 11 step krepidoma, and columns of the temple of Apollo Smintheus at ancient Chryse in the Troad. The temple is an 8 x 14 Ionic pseudodipteros . The exposed stylobate measures 24 x 43 meters, and the remains are surrounded by fragments of sculpture, inscriptions, and Turkish tombstones.
Smintheus is an epithet of Apollo which means "lord of mice". Teucer, a legendary Cretan hero, left the island with his father (Scamander) and a band of followers during a period of famine. An oracle told them they should settle at the place where they were attacked by "sons of the earth." When they woke up one morning and found that their armor had been eaten by mice, they decided that they must have arrived. They built a settlement and erected a temple to Apollo Smintheus.
Today's VIS image shows a streamlined island in a broad channel in Chryse Planitia. The channel is part of the outflow region of Lobo Vallis, a northern branch of Kasei Valles. To see where on Mars this area lies, and to download high-resolution versions of the image, bit.ly/1hFPKHo
The scene here spans 19 x 67 kilometers (12 x 42 miles).
See the Red Planet Report at bit.ly/14KXe4O for updates on Mars research.
For the latest THEMIS Mars images as received by mission scientists, see bit.ly/1d6HA7o . To learn more about the THEMIS camera and its Mars images, see bit.ly/13YOfgm .
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.
Huge regions of complex valleys and chaos are located in Xanthe and Margaritifer Terras. Rising from Valles Marineris, outflow channels like Ares, Tiu and Shalbantana valles empty into Chryse Planitia. This VIS image shows part of Chryse Chaos, located within Masursky Crater, along the Tiu Valles channel. Chaos forms from erosion of the surface into mesa features. With time the valleys expand creating the jumble of hills seen in the image.
This martian scene spans 19x 67 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-20191211a
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 channels, both large and small, in this image are part of Kasei Valles near its terminus in Chryse Planitia. For more about Kasei Valles, see bit.ly/PqadEy. To see where on Mars this area lies, and to download high-resolution versions of the image, bit.ly/1fdZ1Hg
The scene here spans 19 x 67 kilometers (12 x 42 miles).
See the Red Planet Report at bit.ly/14KXe4O for updates on Mars research.
For the latest THEMIS Mars images as received by mission scientists, see bit.ly/1d6HA7o . To learn more about the THEMIS camera and its Mars images, see bit.ly/13YOfgm .
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.
Multiple overlapping lobes of ejected debris are visible in the VIS image of an unnamed crater in Chryse Planitia. To see where on Mars this area lies, and to download high-resolution versions of the image, bit.ly/1cBWUGr
The scene here spans 19 x 68 kilometers (12 x 42 miles).
See the Red Planet Report at bit.ly/14KXe4O for updates on Mars research.
For the latest THEMIS Mars images as received by mission scientists, see bit.ly/1d6HA7o. To learn more about the THEMIS camera and its Mars images, see bit.ly/13YOfgm.
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.
The large mesa in this VIS image is called Nilokeras Mensae. It is located where Kasei Valles empties into Chryse Planitia.
This martian scene spans 19 x 285 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-20251223a
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 Ares Vallis. Ares Vallis is a large channel that arises in Iani Chaos, passes through Margaritifer Terra, and then empties 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-20200422a
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 VIS image shows Xanthe Chaos, located within the channel of Shalbatana Vallis. Chaos terrain is typified by regions of blocky, often steep sided, mesas interspersed with deep valleys. With time and erosion the valleys widen and the mesas become smaller. It has been proposed that a catastrophic outflow of subsurface water creates the chaos and provides the surface flow creating the channel. Chaos terrain is also found along the course of most of channels in this region and may occur where the channel flow fluid warms the subsurface ice creating additional release points for melted subsurface ice. 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. Shalbatana Vallis is 1029km long (639 miles).
This martian scene spans 19 x 221 kilometers (12 x 137 miles). To see where on Mars this area lies, and to download high-resolution versions of the image go to themis.asu.edu/zoom-20251203a
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.