NASA's New Mars Images Hint at Ancient Life on Wet Planet,
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Tue Dec 07, 2010 12:55 am » by Savwafair2012
Newly released images from 340 recent observations of Mars by the High Resolution Imaging Science Experiment (HiRISE) camera aboard NASA's Mars Reconnaissance Orbiter show details of a wide assortment of Martian environments. The new gallery is found here.
Dark Rimless Pits in the Tharsis Region
Two dark, rimless pits are located to the northwest of Ascraeus Mons in the Tharsis volcanic region of Mars. These pits are approximately 180 meters (591 feet) and 310 meters (1,017 feet) in diameter. They are situated in the midst of a wispy, dark, boomerang-shaped deposit
Strewn boulders and rippled sand lie on the floors of two shadowy, steep-walled pits. Mounds in another region appear to be mud volcanoes, which may have brought fine-grained material to the surface from deep underground. In the Tharsis volcanic region, the intersection of a lava flow with a trough caused by ground collapse allows seeing whether the flow happened before or after the collapse.
The pits are aligned with what appear to be larger, degraded depressions. The wispy deposit may consist of dark material blown out of the pits or from some other source.
Figure A and Figure B are close-ups of the two pits. These images have been highly processed to reveal the surface details within each pit. The eastern and smaller of the two pits (A) contains boulders and sediment along its walls and brighter, wind-shaped dune sediments on its floor. The larger, western pit (B) contains sediment and boulders with faint dune-like patterns visible on the deepest part of thefloor. Both pits have steep eastern walls and more gently sloped western walls that transition gradually into the pit floor. Steep, resistant ledges containing boulders that overhang and obscure the pit floorsform the eastern walls
Careful study of the walls and floors of the pits, as well as of the surrounding terrain, will help unravel the complicated series of processes that must have been responsible for their formation and subsequent modification.
This image covers an area about 6 kilometers (4 miles) wide. It is one product from a Nov. 1, 2010, HiRISE observation catalogued as ESP_019997_1975, of an area centered at 17.2 degrees north latitude, 247.6 degrees east longitude. Other image products from this observation are available at `LINK
Terrain Model of Mars' Mojave Crater
A digital terrain model generated from a stereo pair of images provides this synthesized, oblique view of a portion of the wall terraces of Mojave Crater in the Xanthe Terra region of Mars. This view (above), in which the vertical dimension is exaggerated three-fold compared with horizontal dimensions, shows the ponding of material backed up behind massive wall-terrace blocks of bedrock. Hundreds of impact craters on Mars have similarly ponded features with pitted surfaces. These "pitted ponds" are thought to result when material melted by the crater-causing impacts is captured behind the wall terraces.
Mojave Crater is approximately 60 kilometers (37 miles) in diameter, centered at 327.0 degrees east latitude, 7.5 degrees north latitude. The portion of its northwestern edge shown here spans about 3.5 kilometers (about 2.5 miles) in width halfway between the bottom and top of the image. The above view is toward the north.
http://www.nasa.gov/images/content/4618 ... 00-600.jpg
Mojave is one of the freshest large craters on Mars. A survey of its features indicates very few overprinting craters on them, and an analysis of that infrequency suggests the crater may be as young as about 10 million years, very young for a crater of this size. The depth of the crater -- about 2.6 kilometers (1.6 miles) -- also demonstrates that Mojave has experienced little infilling or erosion.
Sand Dunes and Ripples in Proctor Crater, Mars
This view from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's MarsReconnaissance Orbiter shows two classes of aeolian bedforms within Proctor Crater. The relatively bright, small ridges are ripples. From their study on Earth, and close-up examination by the MER rovers (roving elsewhere on Mars), we know that ripples are composed of fine sand (less than 200 microns in diameter) or fine sand coated with coarser sand and granules.
The larger, darker bedforms are dunes composed of sand, most likely of fine size. Ripples tend to move slower than dunes. Because of this, over time, ripples get covered with dust, possibly explaining the bright tone visible here. The dunes are dark probably because they are composed of basaltic sand (derived from dark, volcanic rock) that is blown by the wind enough that dust does not sufficiently accumulate to change their color.
http://www.nasa.gov/images/content/4620 ... 00-600.jpg
Mars Volcanic Cone with Hydrothermal Deposits
This volcanic cone in the Nili Patera caldera on Mars has hydrothermal mineral deposits on the southern flanks and nearby terrains. Light-toned patches on the closest flank of the cone, and the entire field of light-toned material on the left of the cone (see annotated image) are hydrothermal deposits. The cone is about 5 kilometers (3 miles) in diameter at the base. The deposits are evidence for a past local environment that was warm and wet or steamy, possibly hospitable to microbial life, as reported in a November 2010 Nature Geoscience paper by J.R. Skok, of Brown University, Providence, R.I., and co-authors.
http://www.nasa.gov/images/content/4939 ... 00-600.jpg
Spectrometer for Mars (CRISM) on NASA's Mars Reconnaissance Orbiter. The CRISM spectral data is overlaid on imagery from the Context Camera on that orbiter. A stereo pair of Context Camera images provided topographic information for a digital terrain model produced with NASA Ames Stereo Pipeline software. The image uses no vertical exaggeration.
This image is in false color derived from observation in infrared wavebands with the Compact Reconnaissance Imaging
Exposed Ice in a Fresh Crater
At the center of this view of an area of mid-latitude northern Mars, a fresh crater about 6 meters (20 feet) in diameter holds an exposure of bright material, blue in this false-color image. The High-Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter made this observation on June 20, 2010.
http://www.nasa.gov/images/content/4732 ... 00-600.jpg
This image spans a distance of about 170 meters (about 560 feet) and is presented in false color, whichaids in distinguishing among surface materials and textures. It is a portion of the HiRISE observation catalogued as ESP_018273_2245, of an area at 44 degrees north latitude, 180 degrees east longitude. Other image products from this observation are available at `LINK.
Dune Symmetry Inside Martian Crater
Dunes of sand-sized materials have been trapped on the floors of many Martian craters. This is one example, from a crater in Noachis Terra, west of the giant Hellas impact basin.
http://www.nasa.gov/images/content/4619 ... 00-600.jpg
This image covers a swath of ground about 1.2 kilometers (three-fourth of a mile) wide, centered at 42.7 degreessouth latitude, 38.0 degrees east longitude. It is one product from HiRISE observation ESP_016036_1370. The season on Mars is southern-hemisphere autumn. Other image products from this observation are available at `LINK
Light-Toned Deposits in Noctis Labyrinthus
Layers in the lower portion of two neighboring buttes within the Noctis Labyrinthus formation on Mars are visible in this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. The view covers an area about 1 kilometer (0.6 mile) wide.
Dune fields blanket the ground in the upper left of the image and a portion of the ground between the buttes. Exposures of brighter and darker materials are also visible in the portion of that area not covered by the dunes.
Observations of this region of Noctis Labyrinthus by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on the Mars Reconnaissance Orbiter have shown indications of iron-bearing sulfates and phyllosilicate (clay) minerals.
http://www.nasa.gov/images/content/4619 ... 00-600.jpg
This view is a portion of a HiRISE observation taken on Aug. 18, 2009, at 11.2 degrees south latitude, 261.8 degrees east longitude. The full-frame image is available; `LINK.
Image Credit: NASA/JPL-Caltech/University of Arizona
Bright Layered Deposits with Clues of Acidic Water
This view shows color variations in bright layered deposits on a plateau near Juventae Chasma in the Valles Marineris region of Mars. A brown mantle covers portions of the bright deposits. The view covers an area about 1.2 kilometers (three-fourths of a mile) across.
http://www.nasa.gov/images/content/4619 ... 00-600.jpg
Researchers have found that these bright layered deposits contain opaline silica and iron sulfates, consistent with low-temperature, acidic aqueous alteration of basaltic materials. They conclude that aqueous activity affected this plateau after formation of the nearby canyons. Although the source of water and sediment remains uncertain, the strong correlation between fluvial landforms and bright layered deposits in this region argues for sustained precipitation, surface runoff, and fluvial deposition occurring during
Mars' Hesperian Era on the plateaus adjacent to Valles Marineris and along portions of canyon walls.
This image is one product from HiRISE observation PSP_003579_1755, centered at 4.7 degrees south latitude, 296.4 degrees east longitude. Other image products from this observation are available at `LINK
These and thousands of other images from HiRISE observations between Oct. 1 and Nov. 1, 2010, are now available on NASA's Planetary Data System (pds.jpl.nasa.gov/) and the camera team's website (hirise.lpl.arizona.edu).
The camera is one of six instruments on NASA's Mars Reconnaissance Orbiter, which reached Mars in 2006. It has made more than 17,000 observations. Each observation covers an area of several square miles on Mars and reveals details as small as desks.
This enhanced image shows the inside of a rimless pit about 180 meters (591 feet) in diameter, northwest of the mountain Ascraeus Mons in the northern hemisphere of Mars. The pit has a very steep eastern wall (on the right) and a more gently sloped western wall. Shadows and overhangs obscure some of the interior, but this stretched-brightness image shows boulders and sand ripples on the floor.
The image is part of an observation made by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter on Nov. 1, 2010. The terrain covered in the observation includes two dark pits apparently aligned with larger, degraded depressions. Other image products from this observation are available at hirise.lpl.arizona.edu/ESP_019997_1975.
Careful study of the walls and floors of the pits, as well as of the surrounding terrain, will help unravel the complicated series of processes that must have been responsible for their formation and subsequent modification.
NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace & Technologies Corp., Boulder, Colo.
Branched Features on the Floor of Antoniadni Crater
In this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter, the dark branched features in the floor of Antoniadi Crater look like giant ferns, or fern casts. However, these ferns would be several miles in size and are composed of rough rocky materials.
http://www.nasa.gov/images/content/4620 ... 00-600.jpg
A more likely hypothesis is that this represents a channel network that now stands in inverted relief. The channels may have been lined or filled by indurated materials, making the channel fill more resistant to erosion by the wind than surrounding materials. After probably billions of years of wind erosion the resistant channels are now relatively high-standing. The material between the branched ridges has a fracture pattern and color similar to deposits elsewhere on Mars that are known to be rich in hydrated minerals such as clays.
The inverted channels have short, stubby branches characteristic of formation by groundwater sapping. Spring water seeps into the channels and undercuts overlying layers, which collapse, so the channels grow headward. These images tell the story of an ancient wet environment on Mars, where life could have been possible. Ancient Martian life, if it existed, would most likely consist of microorganisms rather than giant tree ferns.
This image, covering an area about 1 kilometer (0.6 mile) across, is a portion of the HiRISE observation catalogued as ESP_012435_2015, taken on March 22, 2009.
Image Credit: NASA/JPL-Caltech/University of Arizona
Northern Hemisphere Gullies on West-Facing Crater Slope, Mars
This image shows the west-facing side of an impact crater in the mid-latitudes of Mars' northern hemisphere. The High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter took the image on April 13, 2010. It is one of 600 recent HiRISE observations newly released to NASA's Planetary Data System.
Dark Rimless Pits in the Tharsis Region
Two dark, rimless pits are located to the northwest of Ascraeus Mons in the Tharsis volcanic region of Mars. These pits are approximately 180 meters (591 feet) and 310 meters (1,017 feet) in diameter. They are situated in the midst of a wispy, dark, boomerang-shaped deposit
Strewn boulders and rippled sand lie on the floors of two shadowy, steep-walled pits. Mounds in another region appear to be mud volcanoes, which may have brought fine-grained material to the surface from deep underground. In the Tharsis volcanic region, the intersection of a lava flow with a trough caused by ground collapse allows seeing whether the flow happened before or after the collapse.
The pits are aligned with what appear to be larger, degraded depressions. The wispy deposit may consist of dark material blown out of the pits or from some other source.
Figure A and Figure B are close-ups of the two pits. These images have been highly processed to reveal the surface details within each pit. The eastern and smaller of the two pits (A) contains boulders and sediment along its walls and brighter, wind-shaped dune sediments on its floor. The larger, western pit (B) contains sediment and boulders with faint dune-like patterns visible on the deepest part of thefloor. Both pits have steep eastern walls and more gently sloped western walls that transition gradually into the pit floor. Steep, resistant ledges containing boulders that overhang and obscure the pit floorsform the eastern walls
Careful study of the walls and floors of the pits, as well as of the surrounding terrain, will help unravel the complicated series of processes that must have been responsible for their formation and subsequent modification.
This image covers an area about 6 kilometers (4 miles) wide. It is one product from a Nov. 1, 2010, HiRISE observation catalogued as ESP_019997_1975, of an area centered at 17.2 degrees north latitude, 247.6 degrees east longitude. Other image products from this observation are available at `LINK
Terrain Model of Mars' Mojave Crater
A digital terrain model generated from a stereo pair of images provides this synthesized, oblique view of a portion of the wall terraces of Mojave Crater in the Xanthe Terra region of Mars. This view (above), in which the vertical dimension is exaggerated three-fold compared with horizontal dimensions, shows the ponding of material backed up behind massive wall-terrace blocks of bedrock. Hundreds of impact craters on Mars have similarly ponded features with pitted surfaces. These "pitted ponds" are thought to result when material melted by the crater-causing impacts is captured behind the wall terraces.
Mojave Crater is approximately 60 kilometers (37 miles) in diameter, centered at 327.0 degrees east latitude, 7.5 degrees north latitude. The portion of its northwestern edge shown here spans about 3.5 kilometers (about 2.5 miles) in width halfway between the bottom and top of the image. The above view is toward the north.
http://www.nasa.gov/images/content/4618 ... 00-600.jpg
Mojave is one of the freshest large craters on Mars. A survey of its features indicates very few overprinting craters on them, and an analysis of that infrequency suggests the crater may be as young as about 10 million years, very young for a crater of this size. The depth of the crater -- about 2.6 kilometers (1.6 miles) -- also demonstrates that Mojave has experienced little infilling or erosion.
Sand Dunes and Ripples in Proctor Crater, Mars
This view from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's MarsReconnaissance Orbiter shows two classes of aeolian bedforms within Proctor Crater. The relatively bright, small ridges are ripples. From their study on Earth, and close-up examination by the MER rovers (roving elsewhere on Mars), we know that ripples are composed of fine sand (less than 200 microns in diameter) or fine sand coated with coarser sand and granules.
The larger, darker bedforms are dunes composed of sand, most likely of fine size. Ripples tend to move slower than dunes. Because of this, over time, ripples get covered with dust, possibly explaining the bright tone visible here. The dunes are dark probably because they are composed of basaltic sand (derived from dark, volcanic rock) that is blown by the wind enough that dust does not sufficiently accumulate to change their color.
http://www.nasa.gov/images/content/4620 ... 00-600.jpg
Mars Volcanic Cone with Hydrothermal Deposits
This volcanic cone in the Nili Patera caldera on Mars has hydrothermal mineral deposits on the southern flanks and nearby terrains. Light-toned patches on the closest flank of the cone, and the entire field of light-toned material on the left of the cone (see annotated image) are hydrothermal deposits. The cone is about 5 kilometers (3 miles) in diameter at the base. The deposits are evidence for a past local environment that was warm and wet or steamy, possibly hospitable to microbial life, as reported in a November 2010 Nature Geoscience paper by J.R. Skok, of Brown University, Providence, R.I., and co-authors.
http://www.nasa.gov/images/content/4939 ... 00-600.jpg
Spectrometer for Mars (CRISM) on NASA's Mars Reconnaissance Orbiter. The CRISM spectral data is overlaid on imagery from the Context Camera on that orbiter. A stereo pair of Context Camera images provided topographic information for a digital terrain model produced with NASA Ames Stereo Pipeline software. The image uses no vertical exaggeration.
This image is in false color derived from observation in infrared wavebands with the Compact Reconnaissance Imaging
Exposed Ice in a Fresh Crater
At the center of this view of an area of mid-latitude northern Mars, a fresh crater about 6 meters (20 feet) in diameter holds an exposure of bright material, blue in this false-color image. The High-Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter made this observation on June 20, 2010.
http://www.nasa.gov/images/content/4732 ... 00-600.jpg
This image spans a distance of about 170 meters (about 560 feet) and is presented in false color, whichaids in distinguishing among surface materials and textures. It is a portion of the HiRISE observation catalogued as ESP_018273_2245, of an area at 44 degrees north latitude, 180 degrees east longitude. Other image products from this observation are available at `LINK.
Dune Symmetry Inside Martian Crater
Dunes of sand-sized materials have been trapped on the floors of many Martian craters. This is one example, from a crater in Noachis Terra, west of the giant Hellas impact basin.
http://www.nasa.gov/images/content/4619 ... 00-600.jpg
This image covers a swath of ground about 1.2 kilometers (three-fourth of a mile) wide, centered at 42.7 degreessouth latitude, 38.0 degrees east longitude. It is one product from HiRISE observation ESP_016036_1370. The season on Mars is southern-hemisphere autumn. Other image products from this observation are available at `LINK
Light-Toned Deposits in Noctis Labyrinthus
Layers in the lower portion of two neighboring buttes within the Noctis Labyrinthus formation on Mars are visible in this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter. The view covers an area about 1 kilometer (0.6 mile) wide.
Dune fields blanket the ground in the upper left of the image and a portion of the ground between the buttes. Exposures of brighter and darker materials are also visible in the portion of that area not covered by the dunes.
Observations of this region of Noctis Labyrinthus by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on the Mars Reconnaissance Orbiter have shown indications of iron-bearing sulfates and phyllosilicate (clay) minerals.
http://www.nasa.gov/images/content/4619 ... 00-600.jpg
This view is a portion of a HiRISE observation taken on Aug. 18, 2009, at 11.2 degrees south latitude, 261.8 degrees east longitude. The full-frame image is available; `LINK.
Image Credit: NASA/JPL-Caltech/University of Arizona
Bright Layered Deposits with Clues of Acidic Water
This view shows color variations in bright layered deposits on a plateau near Juventae Chasma in the Valles Marineris region of Mars. A brown mantle covers portions of the bright deposits. The view covers an area about 1.2 kilometers (three-fourths of a mile) across.
http://www.nasa.gov/images/content/4619 ... 00-600.jpg
Researchers have found that these bright layered deposits contain opaline silica and iron sulfates, consistent with low-temperature, acidic aqueous alteration of basaltic materials. They conclude that aqueous activity affected this plateau after formation of the nearby canyons. Although the source of water and sediment remains uncertain, the strong correlation between fluvial landforms and bright layered deposits in this region argues for sustained precipitation, surface runoff, and fluvial deposition occurring during
Mars' Hesperian Era on the plateaus adjacent to Valles Marineris and along portions of canyon walls.
This image is one product from HiRISE observation PSP_003579_1755, centered at 4.7 degrees south latitude, 296.4 degrees east longitude. Other image products from this observation are available at `LINK
These and thousands of other images from HiRISE observations between Oct. 1 and Nov. 1, 2010, are now available on NASA's Planetary Data System (pds.jpl.nasa.gov/) and the camera team's website (hirise.lpl.arizona.edu).
The camera is one of six instruments on NASA's Mars Reconnaissance Orbiter, which reached Mars in 2006. It has made more than 17,000 observations. Each observation covers an area of several square miles on Mars and reveals details as small as desks.
This enhanced image shows the inside of a rimless pit about 180 meters (591 feet) in diameter, northwest of the mountain Ascraeus Mons in the northern hemisphere of Mars. The pit has a very steep eastern wall (on the right) and a more gently sloped western wall. Shadows and overhangs obscure some of the interior, but this stretched-brightness image shows boulders and sand ripples on the floor.
The image is part of an observation made by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter on Nov. 1, 2010. The terrain covered in the observation includes two dark pits apparently aligned with larger, degraded depressions. Other image products from this observation are available at hirise.lpl.arizona.edu/ESP_019997_1975.
Careful study of the walls and floors of the pits, as well as of the surrounding terrain, will help unravel the complicated series of processes that must have been responsible for their formation and subsequent modification.
NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Mars Reconnaissance Orbiter for NASA's Science Mission Directorate, Washington. Lockheed Martin Space Systems, Denver, built the spacecraft. The High Resolution Imaging Science Experiment is operated by the University of Arizona, Tucson, and the instrument was built by Ball Aerospace & Technologies Corp., Boulder, Colo.
Branched Features on the Floor of Antoniadni Crater
In this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter, the dark branched features in the floor of Antoniadi Crater look like giant ferns, or fern casts. However, these ferns would be several miles in size and are composed of rough rocky materials.
http://www.nasa.gov/images/content/4620 ... 00-600.jpg
A more likely hypothesis is that this represents a channel network that now stands in inverted relief. The channels may have been lined or filled by indurated materials, making the channel fill more resistant to erosion by the wind than surrounding materials. After probably billions of years of wind erosion the resistant channels are now relatively high-standing. The material between the branched ridges has a fracture pattern and color similar to deposits elsewhere on Mars that are known to be rich in hydrated minerals such as clays.
The inverted channels have short, stubby branches characteristic of formation by groundwater sapping. Spring water seeps into the channels and undercuts overlying layers, which collapse, so the channels grow headward. These images tell the story of an ancient wet environment on Mars, where life could have been possible. Ancient Martian life, if it existed, would most likely consist of microorganisms rather than giant tree ferns.
This image, covering an area about 1 kilometer (0.6 mile) across, is a portion of the HiRISE observation catalogued as ESP_012435_2015, taken on March 22, 2009.
Image Credit: NASA/JPL-Caltech/University of Arizona
Northern Hemisphere Gullies on West-Facing Crater Slope, Mars
This image shows the west-facing side of an impact crater in the mid-latitudes of Mars' northern hemisphere. The High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter took the image on April 13, 2010. It is one of 600 recent HiRISE observations newly released to NASA's Planetary Data System.
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- Kalinsaast
-
- Posts: 588
- Joined: Thu Aug 12, 2010 1:15 am
- Location: Halling UK
Tue Dec 07, 2010 1:08 am » by Kalinsaast
Awesome info Sav. 
"Mojave Crater is approximately 60 kilometers (37 miles) in diameter"
That is fucking huge lol.
"Mojave Crater is approximately 60 kilometers (37 miles) in diameter"That is fucking huge lol.
"People spend all their lives worrying that something will happen to them. Eventually they end up in their final days of life. When suddenly they realize they've spent so much time worrying. They infact never lived at all". -Myself
- Wretchfossil
- Posts: 49
- Joined: Thu Dec 02, 2010 4:06 pm
Wed Dec 08, 2010 10:20 am » by Wretchfossil
Clear proof of Martian life in meteorite ALH84001
Found in Martian meteorite ALH84001 are various fossils, including
fossilized remains of mammalian red blood cell, blood vessel,
Haversian canal, osteons, collagen fibril, and chromatin fibers as
shown in the following figures:
Fig. 1: shows mammalian red blood cell and branching blood vessel
http://www.wretch.cc/album/show.php?i=l ... 4796&p=186
Photo source:
http://www.lpi.usra.edu/lpi/meteorites/ ... ities.html
Credit: Dr. Allan Treiman
Fig. 2: shows a Haversian canal found in a carbonate globule of
meteorite ALH84001
http://www.wretch.cc/album/show.php?i=l ... 4797&p=187
Photo source:
http://brainmind.com/Mars.html
Credit: NASA
The following figures have been published previously in
http://wretchfossil.blogspot.com/
Fig. 3: shows a broken,fossilized collagen fibril
http://www.wretch.cc/album/show.php?i=l ... 7114&p=117
Fig. 4: shows several osteons
http://www.wretch.cc/album/show.php?i=l ... 5625&p=130
Fig. 5: shows several chromatin fibers
http://www.wretch.cc/album/show.php?i=l ... 8460&p=126
Found in Martian meteorite ALH84001 are various fossils, including
fossilized remains of mammalian red blood cell, blood vessel,
Haversian canal, osteons, collagen fibril, and chromatin fibers as
shown in the following figures:
Fig. 1: shows mammalian red blood cell and branching blood vessel
http://www.wretch.cc/album/show.php?i=l ... 4796&p=186
Photo source:
http://www.lpi.usra.edu/lpi/meteorites/ ... ities.html
Credit: Dr. Allan Treiman
Fig. 2: shows a Haversian canal found in a carbonate globule of
meteorite ALH84001
http://www.wretch.cc/album/show.php?i=l ... 4797&p=187
Photo source:
http://brainmind.com/Mars.html
Credit: NASA
The following figures have been published previously in
http://wretchfossil.blogspot.com/
Fig. 3: shows a broken,fossilized collagen fibril
http://www.wretch.cc/album/show.php?i=l ... 7114&p=117
Fig. 4: shows several osteons
http://www.wretch.cc/album/show.php?i=l ... 5625&p=130
Fig. 5: shows several chromatin fibers
http://www.wretch.cc/album/show.php?i=l ... 8460&p=126
Fri Jan 28, 2011 7:46 pm » by Bpeirce2
Jesus help you all! Gawking at rocks, microscopic speculations, vertical caves,...please, I will forward HD image of La Victoria crater,...there are dozens of consistently sized,positioned, colored human figures with large round heads and even some look to be wearing life support packs....Come on! Let's get past this smoke and start examining the loaded, cocked, warm, smoking gun, shall we?
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