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Sun of Goddard Space Flight Center (GSFC) from 2001
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The Carina Nebula: Star Birt
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| Title |
The Carina Nebula: Star Birth in the Extreme |
| General Information |
What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. In celebration of the 17th anniversary of the launch and deployment of NASA's Hubble Space Telescope, a team of astronomers is releasing one of the largest panoramic images ever taken with Hubble's cameras. READ: Junior version of this article Amazing Space Learn about this story in the Star Witness, a science newspaper available on our sister site, Amazing Space. [ http://amazing-space.stsci.edu/news/archive/2007/02/ ] It is a 50-light-year-wide view of the central region of the Carina Nebula where a maelstrom of star birth —, and death —, is taking place. This image is a mosaic of the Carina Nebula assembled from 48 frames taken with Hubble's Advanced Camera for Surveys. The Hubble images were taken in the light of neutral hydrogen during March and July 2005. Color information was added with data taken in December 2001 and March 2003 at the Cerro Tololo Inter-American Observatory in Chile. Red corresponds to sulfur, green to hydrogen, and blue to oxygen emission. |
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The 'Big Picture' View of th
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| Title |
The 'Big Picture' View of the Plasmapause and Ionospheric Electron Content - April 2001 |
| Abstract |
This visualization presents a wide-angle overview of the plasmapause-Earth system. Electron content data is mapped to the sphere of the Earth. As the space storm progresses, the structure of the plasmapause becomes distorted but is still constrained by the structure of the Earth's dipolar magnetic field. |
| Completed |
2005-11-18 |
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The 'Big Picture' View of th
…
| Title |
The 'Big Picture' View of the Plasmapause and Ionospheric Electron Content - April 2001 |
| Abstract |
This visualization presents a wide-angle overview of the plasmapause-Earth system. Electron content data is mapped to the sphere of the Earth. As the space storm progresses, the structure of the plasmapause becomes distorted but is still constrained by the structure of the Earth's dipolar magnetic field. |
| Completed |
2005-11-18 |
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The 'Big Picture' View of th
…
| Title |
The 'Big Picture' View of the Plasmapause and Ionospheric Electron Content - April 2001 |
| Abstract |
This visualization presents a wide-angle overview of the plasmapause-Earth system. Electron content data is mapped to the sphere of the Earth. As the space storm progresses, the structure of the plasmapause becomes distorted but is still constrained by the structure of the Earth's dipolar magnetic field. |
| Completed |
2005-11-18 |
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The 'Big Picture' View of th
…
| Title |
The 'Big Picture' View of the Plasmapause and Ionospheric Electron Content - April 2001 |
| Abstract |
This visualization presents a wide-angle overview of the plasmapause-Earth system. Electron content data is mapped to the sphere of the Earth. As the space storm progresses, the structure of the plasmapause becomes distorted but is still constrained by the structure of the Earth's dipolar magnetic field. |
| Completed |
2005-11-18 |
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Time-varying Plasmapause and
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| Title |
Time-varying Plasmapause and Electron data - April 2001 |
| Abstract |
This is another view of the plasmapause and electron content data for the April 11, 2001 time frame (similar to ID 3312). This point of view is shifted slightly to the sunlit side of the Earth to present a better view of the plume formation. |
| Completed |
2005-11-18 |
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Time-varying Plasmapause and
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| Title |
Time-varying Plasmapause and Electron data - April 2001 |
| Abstract |
This is another view of the plasmapause and electron content data for the April 11, 2001 time frame (similar to ID 3312). This point of view is shifted slightly to the sunlit side of the Earth to present a better view of the plume formation. |
| Completed |
2005-11-18 |
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SOHO/MDI Views the Sun - 200
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| Title |
SOHO/MDI Views the Sun - 2001 |
| Abstract |
This version projects the solar image on a flat plane. |
| Completed |
2001-09-28 |
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SOHO/MDI Views the Sun - 200
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| Title |
SOHO/MDI Views the Sun - 2001 |
| Abstract |
This version projects the solar image on a flat plane. |
| Completed |
2001-09-28 |
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Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
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Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
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Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
|
Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
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Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
|
Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
|
Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause (displayed here as a green surface enclosing the Earth) can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. |
| Completed |
2005-11-18 |
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Rotating Tour of Solar Coron
…
| Title |
Rotating Tour of Solar Coronal Loops |
| Abstract |
A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. |
| Completed |
2005-10-20 |
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Rotating Tour of Solar Coron
…
| Title |
Rotating Tour of Solar Coronal Loops |
| Abstract |
A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. |
| Completed |
2005-10-20 |
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Rotating Tour of Solar Coron
…
| Title |
Rotating Tour of Solar Coronal Loops |
| Abstract |
A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. |
| Completed |
2005-10-20 |
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Rotating Tour of Solar Coron
…
| Title |
Rotating Tour of Solar Coronal Loops |
| Abstract |
A slow rotating tour of a data-based coronal loop model. This version is designed for continuous loop play. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. |
| Completed |
2005-10-20 |
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Ionosphere Total Electron Co
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| Title |
Ionosphere Total Electron Content - April 2001 |
| Abstract |
A view of the ionospheric Total Electron Content (TEC) measured over North America during a storm in April 2001. Red is high electron counts, blue is low, grey where there is no data. From the pre-storm state, we see relatively low electron counts . As the storm intensity increases, so do the number of electrons. The increase will generate more interference for communications systems, GPS, etc. |
| Completed |
2005-11-18 |
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Ionosphere Total Electron Co
…
| Title |
Ionosphere Total Electron Content - April 2001 |
| Abstract |
A view of the ionospheric Total Electron Content (TEC) measured over North America during a storm in April 2001. Red is high electron counts, blue is low, grey where there is no data. From the pre-storm state, we see relatively low electron counts . As the storm intensity increases, so do the number of electrons. The increase will generate more interference for communications systems, GPS, etc. |
| Completed |
2005-11-18 |
|
Ionosphere Total Electron Co
…
| Title |
Ionosphere Total Electron Content - April 2001 |
| Abstract |
A view of the ionospheric Total Electron Content (TEC) measured over North America during a storm in April 2001. Red is high electron counts, blue is low, grey where there is no data. From the pre-storm state, we see relatively low electron counts . As the storm intensity increases, so do the number of electrons. The increase will generate more interference for communications systems, GPS, etc. |
| Completed |
2005-11-18 |
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Tour of the Plasmapause - Ap
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| Title |
Tour of the Plasmapause - April 2001 |
| Abstract |
The near-Earth space environment is filled with plasma formed when the sun's ultraviolet rays electrify the upper parts of the Earth's atmosphere. This region is called the plasmasphere and its outer boundary is called the plasmapause. Here we view the plasmasphere in a static state as the observer takes a slow polar-orbiting tour of the region. |
| Completed |
2005-11-18 |
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Tour of the Plasmapause - Ap
…
| Title |
Tour of the Plasmapause - April 2001 |
| Abstract |
The near-Earth space environment is filled with plasma formed when the sun's ultraviolet rays electrify the upper parts of the Earth's atmosphere. This region is called the plasmasphere and its outer boundary is called the plasmapause. Here we view the plasmasphere in a static state as the observer takes a slow polar-orbiting tour of the region. |
| Completed |
2005-11-18 |
|
Tour of the Plasmapause - Ap
…
| Title |
Tour of the Plasmapause - April 2001 |
| Abstract |
The near-Earth space environment is filled with plasma formed when the sun's ultraviolet rays electrify the upper parts of the Earth's atmosphere. This region is called the plasmasphere and its outer boundary is called the plasmapause. Here we view the plasmasphere in a static state as the observer takes a slow polar-orbiting tour of the region. |
| Completed |
2005-11-18 |
|
Zoom-in to plasmapause-induc
…
| Title |
Zoom-in to plasmapause-induced TEC enhancement - April 2001 |
| Abstract |
Space weather events which disturb the plasmapause can propagate down to the Earth's ionosphere. There they enhance the ionosphere electron content which can disrupt radio signals from satellites. This is a re-timed version of ID 3311. This version is designed to play synchronously with ID 3310, ID 3312, and ID 3314. |
| Completed |
2005-11-18 |
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The Solar 'Constant' - Facul
…
| Title |
The Solar 'Constant' - Faculae vs. Sunspots |
| Abstract |
Three views of the Sun showing different levels of solar activity. The color table has been altered to enhance the appearance of the faculae (white regions) which are hotter than sunspots (red-black regions) and whose greater total area contribute to increasing the solar flux reaching the Earth. |
| Completed |
2002-11-30 |
|
Grand Tour of the Coronal Lo
…
| Title |
Grand Tour of the Coronal Loops Model |
| Abstract |
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 Angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2006-03-16 |
|
Grand Tour of the Coronal Lo
…
| Title |
Grand Tour of the Coronal Loops Model |
| Abstract |
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 Angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2006-03-16 |
|
Grand Tour of the Coronal Lo
…
| Title |
Grand Tour of the Coronal Loops Model |
| Abstract |
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 Angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2006-03-16 |
|
Grand Tour of the Coronal Lo
…
| Title |
Grand Tour of the Coronal Loops Model |
| Abstract |
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 Angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2006-03-16 |
|
Grand Tour of the Coronal Lo
…
| Title |
Grand Tour of the Coronal Loops Model |
| Abstract |
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 Angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2006-03-16 |
|
Grand Tour of the Coronal Lo
…
| Title |
Grand Tour of the Coronal Loops Model |
| Abstract |
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 Angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2006-03-16 |
|
SOHO/MDI Views the Sun - 200
…
| Title |
SOHO/MDI Views the Sun - 2001 |
| Abstract |
This version projects the solar image on a sphere for improved perspective. |
| Completed |
2001-08-31 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Flight through the Coronal L
…
| Title |
Flight through the Coronal Loops |
| Abstract |
Here we illustrate the potential benefits of the 3-D views of the Sun which STEREO will provide. Starting with a simple 2-D EIT ultraviolet image from SOHO, we transition to a 3-D model and move through the coronal loops which are constructed along solar magnetic fields. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 Angstroms, the filter wavelength of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 Angstrom imagery using the EIT 'standard color table'. |
| Completed |
2005-10-20 |
|
Global, Seasonal Surface Alb
…
| Title |
Global, Seasonal Surface Albedos |
| Description |
Global models of the Earth system need accurate measurements of how much solar energy is reflected and absorbed by surfaces because this energy drives processes such as plant photosynthesis, snow melt, and longwave reradiation. These images from the Multi-angle Imaging SpectroRadiometer (MISR) provide global, seasonal summaries of a quantity called the Directional Hemispherical Reflectance (DHR), also sometimes referred to as the "black-sky" albedo. The amount of sunlight reflected from a surface, relative to the incident amount, is called the albedo. Bright surfaces have albedo near unity, and dark surfaces have albedo near zero. The DHR refers to the amount of spectral radiation reflected into all upward directions through an imaginary hemisphere situated above each surface point. The "directional" part of the name describes how, in the absence of an intervening atmosphere, light from the Sun would illuminate the surface from a single direction (that is, there is no diffuse skylight, hence the name "black-sky" albedo). To generate this product accurately, it is necessary to compensate for the effects of the atmosphere, and MISR's multi-angle retrieval techniques are used to screen clouds and account for the light scattered by airborne particulates (aerosols). The four image panels show DHR as it was retrieved over land surfaces in MISR's red, green, blue spectral bands (left), and near-infrared, red, blue spectral bands (right), for the seasonal periods December 2001 through February 2002 (top), and June 2002 through August 2002 (bottom). A one-year movie is also provided. Since relatively little sunlight reaches the polar regions during winter, the images were cropped to include only the area which is illuminated in both hemispheres during winter and summer. Noteworthy features include seasonal vegetation and the advance and retreat of the snow line. Regions where DHR could not be derived, either due to an inability to retrieve the necessary atmospheric characteristics or due to the presence of clouds, are shown in black. Further global summaries of the DHR (and other surface and vegetation products) from MISR are now available at the NASA Langley Atmospheric Sciences Data Center. [ http://eosweb.larc.nasa.gov/ ] The Multi-angle Imaging SpectroRadiometer observes the daylit Earth continuously from pole to pole, and every 9 days views the entire globe between 82 degrees north and 82 degrees south latitude. Image courtesy NASA/GSFC/LaRC/JPL, MISR Team. [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www-misr.jpl.nasa.gov/ ] Text by Clare Averill (Acro Service Corporation/JPL) and David J. Diner (JPL). |
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Dewatering Effects from the
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| Title |
Dewatering Effects from the Gujarat Earthquake |
| Description |
MISR Browse Image Viewer [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://eosweb.larc.nasa.gov/MISRBR/ ] provides access to low-resolution true-color versions of these images. This data product was generated from a portion of the imagery acquired during Terra orbits 5736 and 5969. The full-size images cover an area of 215 kilometers x 156 kilometers, and utilize data from blocks 71 to 72 within World Reference System-2 path 151. Image courtesy NASA/GSFC/LaRC/JPL, MISR Team. [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www-misr.jpl.nasa.gov/ ] Text by Clare Averill (Acro Service Corporation/JPL) and David J. Diner (JPL)., browse image of orbit 5969 (380 KB JPEG) On January 26, 2001, when India's Republic Day is normally celebrated, a devastating earthquake hit the state of Gujarat. About 20,000 people died and millions were injured throughout the region. The earthquake had a magnitude of 7.7 on the Richter scale. After the earthquake, local residents reported a mixture of water and sediments fountaining from the Earth. These effects, referred to as dewatering, can result from intense ground shaking by strong earthquakes in regions with shallow water tables. Scientists initially observed dewatering in parts of the Rann of Kutch (a large salt pan in northern Gujarat), and in areas close to the earthquake epicenter. Recent research utilizes the unique capabilities of the Multi-angle Imaging SpectroRadiometer (MISR) instrument to observe earthquake-related dewatering over a broader area (related story: NASA Satellite Helps Scientists See Effects of Earthquakes in Remote Areas [ http://earthobservatory.nasa.gov/Newsroom/NasaNews/2003/2003020511146.html ]). This research is published in the February 4, 2003, issue of EOS Transactions of the American Geophysical Union. These two false-color MISR images were acquired before and after the event, on January 15 and 31, respectively. The earthquake epicenter was located about 80 kilometers east of the city of Bhuj, situated in the lower part of the images. The later image depicts numerous areas where groundwater flowed up to the surface, including within the Rann of Kutch, as well as near the Indo-Pakistani border. These regions of earthquake-associated surface water are apparent up to 200 kilometers from the earthquake's epicenter. Water was observed in many remote areas, especially near the Indo-Pakistani border, which were not easily accessible to survey teams on the ground. Changes in reflection at different view angles and in the near-infrared spectral region assist with the identification of surface water, which appears here in shades of blue and purple. In these visualizations, data from the red band of MISR's most obliquely backward and forward-viewing cameras are displayed as red and blue, respectively, and data from the near-infrared band of MISR's vertically-downward viewing (nadir) camera are displayed as green. Water bodies tend to be more absorbing in the near-infrared, and to be brighter in the view acquired by the more sun-facing (in this case, the 70-degree forward) camera. This combination enhances the ability to distinguish wet surfaces. True color and multi-angle visualizations [ http://earthobservatory.nasa.gov/Newsroom/NewImages/images.php3?img_id=4810 ] of these data were also released in April 2001. The Multi-angle Imaging SpectroRadiometer observes the daylit Earth continuously and every 9 days views the entire globe between 82 degrees north and 82 degrees south latitude. The |
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Dewatering Effects from the
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| Title |
Dewatering Effects from the Gujarat Earthquake |
| Description |
MISR Browse Image Viewer [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://eosweb.larc.nasa.gov/MISRBR/ ] provides access to low-resolution true-color versions of these images. This data product was generated from a portion of the imagery acquired during Terra orbits 5736 and 5969. The full-size images cover an area of 215 kilometers x 156 kilometers, and utilize data from blocks 71 to 72 within World Reference System-2 path 151. Image courtesy NASA/GSFC/LaRC/JPL, MISR Team. [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www-misr.jpl.nasa.gov/ ] Text by Clare Averill (Acro Service Corporation/JPL) and David J. Diner (JPL)., browse image of orbit 5969 (380 KB JPEG) On January 26, 2001, when India's Republic Day is normally celebrated, a devastating earthquake hit the state of Gujarat. About 20,000 people died and millions were injured throughout the region. The earthquake had a magnitude of 7.7 on the Richter scale. After the earthquake, local residents reported a mixture of water and sediments fountaining from the Earth. These effects, referred to as dewatering, can result from intense ground shaking by strong earthquakes in regions with shallow water tables. Scientists initially observed dewatering in parts of the Rann of Kutch (a large salt pan in northern Gujarat), and in areas close to the earthquake epicenter. Recent research utilizes the unique capabilities of the Multi-angle Imaging SpectroRadiometer (MISR) instrument to observe earthquake-related dewatering over a broader area (related story: NASA Satellite Helps Scientists See Effects of Earthquakes in Remote Areas [ http://earthobservatory.nasa.gov/Newsroom/NasaNews/2003/2003020511146.html ]). This research is published in the February 4, 2003, issue of EOS Transactions of the American Geophysical Union. These two false-color MISR images were acquired before and after the event, on January 15 and 31, respectively. The earthquake epicenter was located about 80 kilometers east of the city of Bhuj, situated in the lower part of the images. The later image depicts numerous areas where groundwater flowed up to the surface, including within the Rann of Kutch, as well as near the Indo-Pakistani border. These regions of earthquake-associated surface water are apparent up to 200 kilometers from the earthquake's epicenter. Water was observed in many remote areas, especially near the Indo-Pakistani border, which were not easily accessible to survey teams on the ground. Changes in reflection at different view angles and in the near-infrared spectral region assist with the identification of surface water, which appears here in shades of blue and purple. In these visualizations, data from the red band of MISR's most obliquely backward and forward-viewing cameras are displayed as red and blue, respectively, and data from the near-infrared band of MISR's vertically-downward viewing (nadir) camera are displayed as green. Water bodies tend to be more absorbing in the near-infrared, and to be brighter in the view acquired by the more sun-facing (in this case, the 70-degree forward) camera. This combination enhances the ability to distinguish wet surfaces. True color and multi-angle visualizations [ http://earthobservatory.nasa.gov/Newsroom/NewImages/images.php3?img_id=4810 ] of these data were also released in April 2001. The Multi-angle Imaging SpectroRadiometer observes the daylit Earth continuously and every 9 days views the entire globe between 82 degrees north and 82 degrees south latitude. The |
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Liquefaction Effects from th
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| Title |
Liquefaction Effects from the Bhuj Earthquake |
| Description |
These Multi-angle Imaging Spectroradiometer (MISR) images show the Kachchh region in the Gujarat province of western India. On January 26, 2001, a magnitude 7.7 earthquake devastated this area, killing 20,000 people and destroying buildings, dams, and port facilities. The two upper MISR images are pre- and post-earthquake scenes acquired on January 15 and January 31, 2001, respectively. They are "true-color" images made by combining the red, green and blue bands from the nadir (vertically down-looking) camera. The two lower views are "false-color" images made by combining the red bands from three different cameras. Blue is assigned to the camera pointing 70 degrees forward (more sun-facing), green to the nadir camera, and red to the camera pointing 70 degrees aftward. Each of these images is about 275 kilometers wide by 218 kilometers high. The earthquake epicenter was just below the southern tip of the large, white area on the right-hand side of the images, and about 70 kilometers northeast of the city of Bhuj. The earthquake may have occurred on the Kachchh Mainland Fault, which extends from the region of the epicenter westward along the curved boundary between the darker brown region to the south and the lighter brown area north of it. The compressive stresses responsible for the earthquake are related to the collision of India with Asia and the resulting rise of the Himalayas to the northeast. That part of the Kachchh region which lies north of the Kachchh Mainland Fault includes the Banni Plains and the Rann of Kachchh. It is a low, flat basin characterized by salt pans and mud flats. The salt forms in the Rann of Kachchh as mineral-laden waters evaporate. The salt flats can be seen in the nadir images as highly reflective, white and gray areas. During the earthquake, strong shaking produced liquefaction in the fine silts and sands below the water table in the Rann of Kachchh. This caused the mineral grains to settle and expel their interstitial water to the surface. Field investigations have found abundant evidence of mud volcanos, sand boils, and fissures from which salty ground water erupted over an area exceeding 10,000 square kilometers. Evidence of the expelled water can also be seen on the MISR images. Notice the delicate, dendritic pattern of stream channels throughout many of the salt-flats on the post-earthquake image, especially due north of the epicenter. These carried water brought to the surface by liquefaction during the earthquake. Areas where shallow surface water is present are much easier to see on the false-color multi-angle composite images. Wet areas are exhibiting a combination of enhanced forward-scattered light due to the reflection by the water, and enhanced backward scattering due to surface roughness or the presence of sediments. This combination results in blue to purple hues. The region of sand dunes in the upper right and the Indus River valley and delta in the upper left are inside Pakistan. Near the top, of the images, there is an east-west trending linear feature separating the Thar desert of Pakistan from the Rann of Kachchh. This is the Nagar Parkar Fault. On both pre-earthquake images, this feature is evident only from the contrasting brown colors on either side of it. On the post-earthquake images, a narrow ribbon defines the boundary between the two geologic provinces. However, only in the multi-angle composite do we see evidence that this ribbon may be a water-filled channel. Because this area is politically sensitive and fairly inaccessible, no field teams have been able to verify liquefaction effects or the presence of water there. Image courtesy NASA/GSFC/LaRC/JPL, MISR Team [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www-misr.jpl.nasa.gov/ ] |
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Los Angeles Faults
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Los Angeles Faults |
| Description |
Los Angeles, Calif., is one of the world's largest metropolitan areas with a population of about 15 million people. The urban areas mostly cover the coastal plains and lie within the inland valleys. The intervening and adjacent mountains are generally too rugged for much urban development. This is in large part because the mountains are "young," meaning they are still building (and eroding) in this seismically active (earthquake prone) region. Earthquake faults commonly lie between the mountains and the lowlands. The San Andreas fault, the largest fault in California, likewise divides the very rugged San Gabriel Mountains from the low-relief Mojave Desert, thus forming a straight topographic boundary between the top center and lower right corner of the image. We present this perspective image from NASA's Shuttle Radar Topography Mission (SRTM) with a graphic overlay that maps faults that have been active in Late Quaternary times (white lines). The fault database was provided by the U.S. Geological Survey. The Landsat image used here was acquired on May 4, 2001, about seven weeks before the summer solstice, so natural terrain shading is not particularly strong. It is also not especially apparent given a view direction (northwest) nearly parallel to the sun illumination (shadows generally fall on the backsides of mountains). Consequently, topographic shading derived from the SRTM elevation model was added to the Landsat image, with a false sun illumination from the left (southwest). This synthetic shading enhances the appearance of the topography. Size: View width 134 kilometers (83 miles), view distance 150 kilometers (93 miles) Location: 34.3 degrees North latitude, 118.4 degrees West longitude Orientation: View west-northwest, 1.8 X vertical exaggeration Image Data: Landsat Bands 3, 2+4, 1 as red, green, blue, respectively Original Data Resolution: SRTM 1 arcsecond (30 meters or 98 feet), Landsat 30 meters (98 feet) Graphic Data: Earthquake faults active in Late Quaternary times Date Acquired: February 2000 (SRTM), May 4, 2001 (Landsat). Image Courtesy SRTM Team [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www.jpl.nasa.gov/srtm/ ] NASA/JPL/NIMA and Landsat 7 Science Team [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://landsat7.usgs.gov/ ] NASA GSFC/USGS |
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Fires in Southwestern Austra
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| Title |
Fires in Southwestern Australia |
| Description |
In the southwestern corner of Western Australia, several large fires were burning on December 21, 2001, when NASA?s Aqua satellite passed overhead. Over the weekend of December 18, firefighters contained several lightning-triggered fires burning along the southern coast, but these large fires to the north continued to rage. The image above is made from observations from the Moderate Resolution Imaging Spectroradiometer (MODIS) on Aqua. Vegetation appears bright green, burned areas appear reddish-brown, the ocean appears blue-black, and seasonal, salty lakes appear turquoise. The top image in the pair shows the wide-area view, while the bottom image shows an area of detail around Lakes Johnston and Hope at MODIS? maximum spatial resolution of 250 meters per pixel. Red has been used to outline pixels in which MODIS detected active fire. Dark smoke spreads southeast from the fires. The close-up also reveals an unusual sight for this kind of image: a very bright, red-orange "glow" inside the fire-detection pixels. The reddish color of the burned areas scattered across the top image in the pair comes from shortwave infrared energy reflected from the burned surface. The brightness of the red depends on the type of vegetation, how much ash and soot remain, and how recently the area burned. A red as intense as what appears inside the fire-detection pixels in the bottom image is very rare, however. The brightness suggests that MODIS was seeing more than just the shortwave infrared energy from the sun reflected back from a burned surface, but was also seeing shortwave infrared energy being emitted by intense flaming. Image courtesy the MODIS Rapid Response Team, NASA-Goddard Space Flight Center |
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Fires in Southwestern Austra
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| Title |
Fires in Southwestern Australia |
| Description |
In the southwestern corner of Western Australia, several large fires were burning on December 21, 2001, when NASA?s Aqua satellite passed overhead. Over the weekend of December 18, firefighters contained several lightning-triggered fires burning along the southern coast, but these large fires to the north continued to rage. The image above is made from observations from the Moderate Resolution Imaging Spectroradiometer (MODIS) on Aqua. Vegetation appears bright green, burned areas appear reddish-brown, the ocean appears blue-black, and seasonal, salty lakes appear turquoise. The top image in the pair shows the wide-area view, while the bottom image shows an area of detail around Lakes Johnston and Hope at MODIS? maximum spatial resolution of 250 meters per pixel. Red has been used to outline pixels in which MODIS detected active fire. Dark smoke spreads southeast from the fires. The close-up also reveals an unusual sight for this kind of image: a very bright, red-orange "glow" inside the fire-detection pixels. The reddish color of the burned areas scattered across the top image in the pair comes from shortwave infrared energy reflected from the burned surface. The brightness of the red depends on the type of vegetation, how much ash and soot remain, and how recently the area burned. A red as intense as what appears inside the fire-detection pixels in the bottom image is very rare, however. The brightness suggests that MODIS was seeing more than just the shortwave infrared energy from the sun reflected back from a burned surface, but was also seeing shortwave infrared energy being emitted by intense flaming. Image courtesy the MODIS Rapid Response Team, NASA-Goddard Space Flight Center |
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