View allAll Photos Tagged complexity
Complexity rules,
the scent of aged forest,
pine cones ready the fall.
Photographer Notes: This is your typical grab shot while hiking in Yosemite Valley. Aperture setting, f/6.3, 1/125, 45mm. I was reading from Ansel's book the other day and interestingly he stated that most people believed his work to be "realistic" but he contended that he manipulated photographic controls in his prints to "evoke what I saw and felt." At first I thought this way too saturated but this is what I saw and felt. I want this level of color, detail, complexity in this image!
Blog Oxherding is Fun ~~ on Twitter ~~ Oxherder Arts Gallery
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.
Croton Plant. Botanical Name: Codiaeum variegatum pictum.
Taken at The Regency, Laguna Woods, California. © 2013 All Rights Reserved.
My images are not to be used, copied, edited, or blogged without my explicit permission.
Please!! NO Glittery Awards or Large Graphics...Buddy Icons are OK. Thank You!
Have a terrific new week, my Flickr friends! Thanks so much for coming by!
From the brief, odd stretch when PopPhoto were billing the title as Photography: the Magazine of Popular Photography.
My tags include the rival publications which apparently they had hoovered up, based on other fine print below this.
OpTic Gaming get in the action early Saturday morning to test out the systems and get a feel for the sound proof booths.
Complexity Group Grapes On a Train 2013
Left to right:
Nautilus Sauvignon Blanc, Marlborough 2012
Cloudy Bay Sauvignon Blanc, Marlborough 2012
Mud House The Woolshed Vineyard, Sauvignon Blanc, Marlborough 2013
Villa Maria Reserve Wairau, Sauvignon Blanc, Marlborough 2012
Nautilus "Winemakers Selection" Sauvignon Blanc, Marlborough 2009
Nautilus "Winemakers Selection" Sauvignon Blanc, Marlborough 2012
To read more about this trip, please CLICK HERE
© 2013 Tina Wong; The Wandering Eater. All Rights Reserved. Images may not be reproduced, copied, or used in any way without written permission.
Why do you need to do 2 actions when switching modi? If I checkin at GVB can't I be automatically checked out of NS and vice versa?
Not to mention the forest of consoles greeting you when you get on the platform. Some of these will be removed in due time, but still not very KISS.
Uploaded with AirMe
How many deal with complexity - detail of a Graphic Recording by Mathias Weitbrecht
www.IntegralInformationArchitecture.com
Bild / image: (c) All Rights Reserved
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.
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.
Congratulations to Kate Rivers, who beat out thousands of artists to appear in the West edition of New American Paintings 2014. An excerpt from her artist statement:
"My work is abstract, focused on color and texture. All the work is structurally dense, complex, and layered—a metaphor for the complexity of obsession. Collage is the fundamental medium. Frequently, the collage is combined with oil stick, painting, and machine-and hand-stitching. Scale is extremely important. While many pieces are small, my goal is to construct mural-size works created from either books or merchandise tags..."
Read more here- www.thematthewsgallery.com/Images/Files/Kate-Rivers-New-A...
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.
Work is well underway on Sky Waka, the new high-speed gondola at Whakapapa on New Zealand’s North Island, with the team facing ever-changing logistical challenges with engineering specifications, getting materials on-site, and the physical construction process.
Lack of access over unique volcanic terrain adds to the complexity of this project. Even transporting concrete from the truck to the construction site has required some out of the box thinking.
“Conventional concrete trucks drive part way up the mountain and are then replaced with a trailer concrete mixing bowl with a 3.5 cubic metre capacity” says Whakapapa General Manager, Jono Dean.
“The concrete is then transferred onto a purpose built aerial material ropeway system that then transfers the loads to the locations required in the mid mountain. To date, 400 of the 1100 tonnes required for this project has been transported.”
The Swiss engineered ropeway can transport up to 5 tonnes of equipment and materials without relying on helicopter use, which can be restricted due to weather conditions. At over 1000m in length with towers up to 34m tall, it is the first of its kind in NZ to be constructed for the purpose of building a passenger ropeway on a ski field.
“We’ve had amazing luck with weather this summer, which has got the project off to a great start but being up a mountain conditions could change rapidly and affect the project timeline.”
The construction of the 14 tower foundations to support the new Sky Waka gondola line are nearly complete and work is underway on the terminal stations where people will get on and off the gondola.
Italian based company Leitner is supplying and installing the gondola, and General Manager David Ratcliffe says he’s excited to be involved in New Zealand’s largest gondola installation. “This project has presented unique challenges but work is progressing well and it’s exciting to be a part of such an iconic project.”
The fifty Sky Waka gondola cabins will feature floor to ceiling glass for breathtaking views, internal ski racks, audio and lighting and individual leather seats offering business-class luxury to passengers befitting of the UNESCO Dual World Heritage status of Whakapapa Ski Area. Each cabin accommodates 10 passengers and even the tallest skiers will be able to stand upright in the cabin with more than 2m of internal clearance.
The Sky Waka will run from the Top of the Bruce base area directly to the award-winning Knoll Ridge Café. It will transport 2,400 people per hour over the 1.8km in approximately 5 minutes.
Social and economic indicators for the gondola project are compelling, with a team of about 35 hands on people working on the project and another estimated 100 people contributing to the project behind the scenes, including a strong contingent of local employment from the area.
The gondola project has involved working closely with Ngati Tuwharetoa and DOC which has seen a significant reduction in the number of structures on the mountain, the new installation having less than half of the structures it replaces.
As a public benefit entity RAL invests its proceeds back into developing the mountain’s facilities and the new gondola forms part of the $100m reinvestment strategy announced by the RAL board in 2015.
Les travaux vont bon train sur Sky Waka, la nouvelle télécabine à haute vitesse de Whakapapa, sur l’île du Nord de la Nouvelle-Zélande. L’équipe est confrontée à des défis logistiques en constante évolution: spécifications techniques, mise en place des matériaux et processus de construction.
Le manque d'accès sur un terrain volcanique unique ajoute à la complexité de ce projet. Même le transport du béton du camion sur le chantier a nécessité une réflexion originale.
«Les camions en béton conventionnels roulent en partie sur la montagne et sont ensuite remplacés par un bol à béton d'une remorque d'une capacité de 3,5 mètres cubes», a déclaré Jono Dean, directeur général de Whakapapa.
«Le béton est ensuite transféré sur un système de remontée mécanique sur matériaux aériens spécialement conçu à cet effet, qui transfère ensuite les charges aux emplacements requis en moyenne montagne. À ce jour, 400 des 1 100 tonnes requises pour ce projet ont été transportées. ”
Les remontées mécaniques suisses peuvent transporter jusqu'à 5 tonnes d'équipements et de matériaux sans recourir à l'utilisation d'hélicoptères, ce qui peut être limité en raison des conditions météorologiques. Avec plus de 1000 m de long et des tours atteignant 34 m de haut, il s'agit du premier du genre en Nouvelle-Zélande à être construit dans le but de construire un téléphérique pour passagers sur un domaine skiable.
"Nous avons eu une chance incroyable avec la météo de cet été, ce qui a donné un bon départ au projet, mais être dans les conditions montagneuses pourrait changer rapidement et avoir une incidence sur le calendrier du projet."
La construction des 14 fondations de la tour pour soutenir la nouvelle gondole Sky Waka est presque terminée et des travaux sont en cours sur les gares terminales où les gens pourront monter et descendre de la télécabine.
Leitner, société italienne, fournit et installe la gondole. Le directeur général, David Ratcliffe, se dit ravi de participer à la plus grande installation de gondoles de Nouvelle-Zélande. "Ce projet a présenté des défis uniques, mais le travail avance bien et c’est excitant de faire partie d’un projet aussi emblématique."
Les cinquante cabines de la télécabine Sky Waka comprendront des baies vitrées offrant une vue époustouflante, des porte-skis internes, un système audio et d'éclairage ainsi que des sièges individuels en cuir offrant un luxe de classe affaires aux passagers, digne du statut de domaine de ski de Whakapapa classé au double patrimoine mondial de l'UNESCO. Chaque cabine peut accueillir 10 passagers et même les plus grands skieurs pourront se tenir debout dans la cabine avec plus de 2 m de dégagement interne.
Le Sky Waka ira de la base de Top of the Bruce au Knoll Ridge Café, un établissement primé. Il transportera 2 400 personnes par heure sur 1,8 km en 5 minutes environ.
Les indicateurs sociaux et économiques du projet de gondole sont convaincants, avec une équipe d'environ 35 personnes travaillant sur le projet et environ 100 personnes contribuant au projet en coulisse, y compris un fort contingent d'emplois locaux de la région.
Le projet de télécabine a impliqué une collaboration étroite avec Ngati Tuwharetoa et DOC, qui a enregistré une réduction significative du nombre de structures en montagne, la nouvelle installation remplaçant moins de la moitié des structures.
En tant qu’entité d’intérêt public, RAL réinvestit ses recettes dans le développement des installations de la montagne. La nouvelle télécabine fait partie de la stratégie de réinvestissement de 100 millions de dollars annoncée par le conseil d’administration de RAL en 2015.