{"dp_type": "Dataset", "free_text": "Keogram"}
[{"awards": "0840398 Mende, Stephen", "bounds_geometry": ["POLYGON((-180 -75,-144 -75,-108 -75,-72 -75,-36 -75,0 -75,36 -75,72 -75,108 -75,144 -75,180 -75,180 -76.5,180 -78,180 -79.5,180 -81,180 -82.5,180 -84,180 -85.5,180 -87,180 -88.5,180 -90,144 -90,108 -90,72 -90,36 -90,0 -90,-36 -90,-72 -90,-108 -90,-144 -90,-180 -90,-180 -88.5,-180 -87,-180 -85.5,-180 -84,-180 -82.5,-180 -81,-180 -79.5,-180 -78,-180 -76.5,-180 -75))"], "date_created": "Fri, 01 Jan 2010 00:00:00 GMT", "description": "This award is funded under the American Recovery and Reinvestment Act of 2009 (Public Law 111-5). The PENGUIn team will continue investigating in depth a multi-scale electrodynamic system that comprises space environment of Planet Earth (geospace). Several science topics important to the space physics and aeronomy are outlines in this proposal that can be broadly categorized as the following objectives: (a) to study reconnection and waves in the southern cusp region; (b) to investigate unraveling global geomagnetic substorm signatures; (c) to understand the dayside wave-particle interactions; and (d) to observe and investigate various polar cap phenomena and neutral atmosphere dynamics. Cutting-edge science on these critical topics will be accomplished by acquiring multi-instrument data from a distributed network of autonomous observatories in Antarctica, built and deployed with the matured technological achievements. In the last several years, advances in power supply systems and Iridium data transmission for the Automatic Geophysical Observatories (AGOs) have proven effective for providing real-time geophysical data reliably. Five AGOs that span from the auroral zone to deep in the polar cap will be maintained providing a wealth of data for science analyses. Additional instrumentation as GPS-based receivers measuring total electron content in the ionosphere will be deployed at AGOs. These scientific investigations will be enriched by complementary measurements from manned stations in the Antarctic, from magnetically conjugate regions in the Arctic, and from a fleet of magnetospheric and ionospheric spacecraft. Continued reliance on students provides a broader impact to this proposed research and firmly grounds this effort in its educational mission.", "east": 180.0, "geometry": ["POINT(0 -89.999)"], "keywords": "Antarctica; Atmosphere; Keogram; Potential Field", "locations": "Antarctica", "north": -75.0, "nsf_funding_programs": null, "persons": "Frey, Harald; Mende, Stephen", "project_titles": "Collaborative Research: PENGUIn - A High-Latitude Window to Geospace Dynamics", "projects": [{"proj_uid": "p0000685", "repository": "USAP-DC", "title": "Collaborative Research: PENGUIn - A High-Latitude Window to Geospace Dynamics"}], "repo": "USAP-DC", "repositories": "USAP-DC", "science_programs": null, "south": -90.0, "title": "PENGUIn - A High-Latitude Window to Geospace Dynamics", "uid": "600109", "west": -180.0}, {"awards": "0636899 Mende, Stephen", "bounds_geometry": null, "date_created": "Tue, 01 Jan 2008 00:00:00 GMT", "description": "Auroral protons are not energized by electric fields directly above the auroral atmosphere and therefore they are a much better diagnostic of processes deep in the magnetosphere. It has been shown from measurements from space by the IMAGE spacecraft that the dayside hydrogen emission is directly related to dayside reconnection processes. A four channel all-sky images had been operating at South Pole during 2004-2007 to observe auroral features in specific wavelengths channels that allowed a quantitative investigation of proton aurora. This was accomplished by measuring the Hydrogen Balmer beta line at 486.1 nm and by monitoring another wavelength band for subtracting non proton produced background emissions. South Pole allows these measurements because of the 24 hour darkness and favorable conditions even on the dayside. To increase the scientific return it was also attempted to measure the Doppler shift of the hydrogen emissions because that provides diagnostics regarding the energy of the protons. Thus the proton camera measured 3 wavelength bands simultaneously in the vicinity of the Balmer beta line to provide the line intensity near zero Doppler shift, at a substantial Doppler shift and a third channel for background. \n\nThe 4-channel all-sky camera at South Pole was modified in 2008 in order to observe several types of auroras, and to distinguish the cusp reconnection aurora from the normal plasma sheet precipitation. The camera simultaneously operates in four wavelength regions that allow a distinction between auroras that are created by higher energy electrons (greater than 1 keV) and those created by low energy (less than 500 eV) precipitation. The cusp is the location where plasma enters the magnetosphere through the process of magnetic reconnection. This reconnection occurs where the Interplanetary Magnetic Field (IMF) and the terrestrial magnetic field are oriented in opposite directions. \n\nThe data are represented as keograms (geomagnetic north-south slices through the time series of images) for the four different wavelengths. The top of the keogram points to the magnetic south pole. The time series allows a very quick assessment about the presence of aurora, motion, intensity, and brightness differences in the four simultaneously registered channels.", "east": null, "geometry": null, "keywords": "Antarctica; Atmosphere; Aurora; Cosmos; Photo/video; Photo/Video", "locations": "Antarctica", "north": null, "nsf_funding_programs": null, "persons": "Frey, Harald; Mende, Stephen", "project_titles": "Antarctic Auroral Imaging", "projects": [{"proj_uid": "p0000361", "repository": "USAP-DC", "title": "Antarctic Auroral Imaging"}], "repo": "USAP-DC", "repositories": "USAP-DC", "science_programs": null, "south": null, "title": "Antarctic Auroral Imaging", "uid": "600070", "west": null}]
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| Dataset Title/Abstract/Map | NSF Award(s) | Date Created | PIs / Scientists | Project Links | Abstract | Bounds Geometry | Geometry | Selected | Visible |
|---|---|---|---|---|---|---|---|---|---|
|
PENGUIn - A High-Latitude Window to Geospace Dynamics
|
0840398 |
2010-01-01 | Frey, Harald; Mende, Stephen |
Collaborative Research: PENGUIn - A High-Latitude Window to Geospace Dynamics |
This award is funded under the American Recovery and Reinvestment Act of 2009 (Public Law 111-5). The PENGUIn team will continue investigating in depth a multi-scale electrodynamic system that comprises space environment of Planet Earth (geospace). Several science topics important to the space physics and aeronomy are outlines in this proposal that can be broadly categorized as the following objectives: (a) to study reconnection and waves in the southern cusp region; (b) to investigate unraveling global geomagnetic substorm signatures; (c) to understand the dayside wave-particle interactions; and (d) to observe and investigate various polar cap phenomena and neutral atmosphere dynamics. Cutting-edge science on these critical topics will be accomplished by acquiring multi-instrument data from a distributed network of autonomous observatories in Antarctica, built and deployed with the matured technological achievements. In the last several years, advances in power supply systems and Iridium data transmission for the Automatic Geophysical Observatories (AGOs) have proven effective for providing real-time geophysical data reliably. Five AGOs that span from the auroral zone to deep in the polar cap will be maintained providing a wealth of data for science analyses. Additional instrumentation as GPS-based receivers measuring total electron content in the ionosphere will be deployed at AGOs. These scientific investigations will be enriched by complementary measurements from manned stations in the Antarctic, from magnetically conjugate regions in the Arctic, and from a fleet of magnetospheric and ionospheric spacecraft. Continued reliance on students provides a broader impact to this proposed research and firmly grounds this effort in its educational mission. | ["POLYGON((-180 -75,-144 -75,-108 -75,-72 -75,-36 -75,0 -75,36 -75,72 -75,108 -75,144 -75,180 -75,180 -76.5,180 -78,180 -79.5,180 -81,180 -82.5,180 -84,180 -85.5,180 -87,180 -88.5,180 -90,144 -90,108 -90,72 -90,36 -90,0 -90,-36 -90,-72 -90,-108 -90,-144 -90,-180 -90,-180 -88.5,-180 -87,-180 -85.5,-180 -84,-180 -82.5,-180 -81,-180 -79.5,-180 -78,-180 -76.5,-180 -75))"] | ["POINT(0 -89.999)"] | false | false |
|
Antarctic Auroral Imaging
|
0636899 |
2008-01-01 | Frey, Harald; Mende, Stephen |
Antarctic Auroral Imaging |
Auroral protons are not energized by electric fields directly above the auroral atmosphere and therefore they are a much better diagnostic of processes deep in the magnetosphere. It has been shown from measurements from space by the IMAGE spacecraft that the dayside hydrogen emission is directly related to dayside reconnection processes. A four channel all-sky images had been operating at South Pole during 2004-2007 to observe auroral features in specific wavelengths channels that allowed a quantitative investigation of proton aurora. This was accomplished by measuring the Hydrogen Balmer beta line at 486.1 nm and by monitoring another wavelength band for subtracting non proton produced background emissions. South Pole allows these measurements because of the 24 hour darkness and favorable conditions even on the dayside. To increase the scientific return it was also attempted to measure the Doppler shift of the hydrogen emissions because that provides diagnostics regarding the energy of the protons. Thus the proton camera measured 3 wavelength bands simultaneously in the vicinity of the Balmer beta line to provide the line intensity near zero Doppler shift, at a substantial Doppler shift and a third channel for background. The 4-channel all-sky camera at South Pole was modified in 2008 in order to observe several types of auroras, and to distinguish the cusp reconnection aurora from the normal plasma sheet precipitation. The camera simultaneously operates in four wavelength regions that allow a distinction between auroras that are created by higher energy electrons (greater than 1 keV) and those created by low energy (less than 500 eV) precipitation. The cusp is the location where plasma enters the magnetosphere through the process of magnetic reconnection. This reconnection occurs where the Interplanetary Magnetic Field (IMF) and the terrestrial magnetic field are oriented in opposite directions. The data are represented as keograms (geomagnetic north-south slices through the time series of images) for the four different wavelengths. The top of the keogram points to the magnetic south pole. The time series allows a very quick assessment about the presence of aurora, motion, intensity, and brightness differences in the four simultaneously registered channels. | [] | [] | false | false |
