View allAll Photos Tagged Complexity
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. Inverted grayscale variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. Color/processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
Scholars gathered together at the Pequot Museum on Friday & Saturday, Oct. 18 & 19, for the 17th Century American Northeast Conference to reexamine the complexity of a changing cultural landscape and the consequences of colonization and warfare.
Un sistema complesso è un insieme in cui gli elementi subiscono continue modifiche singolarmente prevedibili, ma di cui non è possibile, o è molto difficile, prevedere uno stato futuro.
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. This image shows a close-up of one crest in the rings.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. This image shows a close-up of one crest in the rings. Processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
ci sono parentesi
in cui una curva
di pensiero
è tangente
alla prospettiva
la linea
del fondo
diviene residuo
sottile
si perde
nella sostanza
-luz-
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. This image shows a close-up of one crest in the rings. Processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
women+traditional alger city veil+islamic veil+cig =
a smashing variety of greys....algeria isn't a country in black and white only.
hijab+'jar+garo....
Edited Cassini montage of PR images of the scalloped edges of a gap in the rings of Saturn where the moon Daphnis is making things complex. This image shows a close-up of one crest in the rings. Processing variant.
Image source: photojournal.jpl.nasa.gov/catalog/PIA23167
Original caption: This enhanced-color image mosaic shows Daphnis, one of the moons embedded in Saturn's rings, in the Keeler gap on the sunlit side of the rings. Daphnis is seen kicking up three waves in the gap's outer edge. Three wave crests of diminishing sizes trail the moon. In each successive crest, the shape of the wave changes as the ring particles within the crest interact and collide with each other. A thin strand of ring material to the lower left of Daphnis is newly visible in this image, and there are intricate features that also hadn't been previously observed in the third wave crest downstream (see Figure 1).
Cassini was at a very shallow angle above the rings (only about 15 degrees) when this image was taken. The resulting foreshortening makes it difficult to tell the difference in this image between features representing vertical structure and those representing radial, or outward from Saturn, structure within the ring plane. Nonetheless, Cassini imaging scientists have determined that the waves in the gap are largely vertical; compare this to the shadows that they were seen to cast during equinox (see PIA11547, PIA11653, PIA11655 and PIA11656). The thin strand of material is also probably vertical. Daphnis itself is actually five times smaller than the width of the gap, but it looks bigger here because of the foreshortening.
The color in this image comes from using Imaging Science Subsystem images obtained by applying different filters to "paint" color onto the black-and-white version of this view previously released as PIA17212. The color of the ring region outward of the Keeler Gap (the "trans-Keeler region," in the lower portion of this image) is noticeably different from the color inward from the gap (upper portion of this image). In visible light, this color difference sharply coincides with the gap, while near-infrared Visible and Infrared Mapping Spectrometer (VIMS) images show some bleeding of the trans-Keeler region into the region inward from the gap. The reasons for the sharp change in color are mysterious, but they probably have more to do with a change in particle sizes and other properties than with a change in composition.
The images in this mosaic were taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 17,000 miles (28,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 71 degrees (for the color images, 58 degrees). Image scale is 550 feet (170 meters) per pixel.
The image was produced by Tilmann Denk at Freie Universität in Berlin.
Figure 1 shows a closeup of the third wave crest (toward the far left in the color image) focusing on detail scientists hadn't seen before, with multiple strands of ring material visible. The image shows how the ring material behaves after losing the structure Daphnis triggered and goes back to interacting with itself.
The ribbon of material that appears to be protruding into the gap in the right-hand portion of the image is probably actually soaring above the ring plane. Toward the left-hand part of the image, that same ribbon of material dives below the ring plane and becomes obscured by the main part of the rings, which is why it disappears from view.
The image shown in Figure 1 was taken in visible light, using the Cassini spacecraft narrow-angle camera at a distance of approximately 15,000 miles (23,000 kilometers) from Daphnis and at a Sun-Daphnis-spacecraft angle, or phase angle, of 94 degrees. Image scale is 520 feet (160 meters) per pixel. Unlike the main image, the image in Figure 1 was taken on the unlit side of the rings.
The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of Caltech in Pasadena, manages the mission for NASA's Science Mission Directorate in Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.
For more information about the Cassini-Huygens mission visit solarsystem.nasa.gov/cassini. The Cassini imaging team homepage is at ciclops.org.
Several months ago, I was trying very hard to bring these qualities out of this holga shot of a storefront window on Mississippi Street in Portland OR.
I got sidetracked, and instead created something completely different. While I still enjoy that version, I think this one says more about the camera and the moment of capture.
Here's this version Large.
Entry in category 3. Locations and instruments; Copyright: CC-BY-NC-ND: Yves Suter
My complexity image is shot on a Zeiss Ikon rangefinder camera, with a 35mm lens on analog Kodak Film (ISO 200) Material, at afternoon daylight. In my complexity work, I try to show raw jungle. Not like a tourist agency would show it, just how it really is. Pure, untouched jungle. I tried to set range in a very complex environment, showing the complexity and dense mixture of flora and fauna far from human civilization. By focusing like this, you can stare and catch a glimpse of this somewhat barbarian wildness. The bigger you print this picture and the longer you watch it, the more you can get lost in the complexity of nature.
Camera: Pentax Spotmatic SP, f3.5 28mm SMC Takumar lens. Plus-X, pulled to ISO 40 because it expired in 1977. Hamilton and Spencer, Ottawa, ON.
'Food Security, Livelihoods and Livestock in the Developing World' slide presentation in 2010 by Mario Herrero: 'Addressing complexity' (figure credit: ILRI/Herrero).
The complexity of the Swithland Sidings lay-out is highlighted in this telephoto view from the signal box as Southern Railway Schools 4-4-0 925 Cheltenham heads tender-first out of the sun towards Loughborough. 925 is running under clear signals with the Swithland Down Home & Down Inner Distant both cleared. What is not obvious is the fact that 4-6-0 777 Sir Lamiel is running light engine alongside 925 on the Up line.
On the left the double slip out of the Up Loop/Up sidings can be seen together with the Swithland Up Main Starter above the Rothley Up Outer Distant plus the Backing Signal to control "wrong road" movements on the Up lines. The catch point at the south end of the Down Loop is seen on the far right.
By Laura Lindow (Sawdust & Stardust and Your Aunt Fanny)
Directed by Anna Ryder
I say, I say, I say. What happens when a hospital clown meets a 17 year old transplant patient who wants to be anywhere but here? Will there be balloons? Juggling? Acrobatics? Not likely!
Outside the hospital all Arran wants is a break from his family. And some peace and quiet. Not a whole load of bad jokes! But there may be more to Dr Charlie Dander’s red nose than first meets the eye.
This short play opens a small window into the complexities of a simple exchange. A true heart to heart with the potential for the ultimate magic trick. It looks at the weight of dealing with illness and recovery, and the indefinable space in between.
Cast:
Dean Bone
Phil Corbitt
Karen Traynor
Stretching more than 300 metres along the north dock, the above ground scheme designed by Foster + Partners includes four levels of shops, cafes and restaurants, as well as extensive public gardens, which are densely planted with trees and plants, and interspersed with seating and pavilions – all partially enclosed by a timber lattice roof, which wraps around the building like a protective shell.
The gardens are accessible from ground level via two connecting bridges. The roof opens in the centre to draw in light and rain for natural irrigation, and opens along the sides and at either end to allow views of the water and surrounding streets. The spruce beams are sustainably sourced and provide a warm, natural counterpoint to the glass and steel towers of Canary Wharf. Between the beams there are air-filled plastic cushions. The partial enclosure of the space creates a comfortable environment for people to enjoy all year round, as well as providing a gentle microclimate for some of the plant species that first entered Britain through the docks.
The design of the lattice itself is a fusion of architecture and engineering. Remarkably, despite the smooth curve of the enclosure, there are only four curved timber beams in the whole structure. To seamlessly connect the straight beams, which rotate successively along the diagonals, the design team developed an innovative system of steel nodes, which resolve the twist. The visual simplicity of the smooth curving timber lattice belies the geometric complexity of the structure, which is made up of 1,418 beams and 564 nodes, 364 of which are unique. Foster + Partners’ specialist modelling group helped to develop an innovative system to enable the roof components to be rapidly fabricated and accurately assembled on site. At night the structure is illuminated, creating a welcoming civic gateway to London’s growing commercial district.
[Foster+Partners]
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