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Sun of Goddard Space Flight Center (GSFC) from 2001 and December, 2001
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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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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 |
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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 |
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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 |
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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 |
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