The Experts below are selected from a list of 27399 Experts worldwide ranked by ideXlab platform
William E. Mcclintock - One of the best experts on this subject based on the ideXlab platform.
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Improving Solar wind modeling at Mercury: Incorporating transient Solar Phenomena into the WSA‐ENLIL model with the Cone extension
Journal of Geophysical Research: Space Physics, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. Mcclintock, Dusan OdstrcilAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
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improving Solar wind modeling at mercury incorporating transient Solar Phenomena into the wsa enlil model with the cone extension
Journal of Geophysical Research, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. McclintockAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
Daniel J. Gershman - One of the best experts on this subject based on the ideXlab platform.
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Improving Solar wind modeling at Mercury: Incorporating transient Solar Phenomena into the WSA‐ENLIL model with the Cone extension
Journal of Geophysical Research: Space Physics, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. Mcclintock, Dusan OdstrcilAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
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improving Solar wind modeling at mercury incorporating transient Solar Phenomena into the wsa enlil model with the cone extension
Journal of Geophysical Research, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. McclintockAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
Catherine L. Johnson - One of the best experts on this subject based on the ideXlab platform.
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Improving Solar wind modeling at Mercury: Incorporating transient Solar Phenomena into the WSA‐ENLIL model with the Cone extension
Journal of Geophysical Research: Space Physics, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. Mcclintock, Dusan OdstrcilAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
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improving Solar wind modeling at mercury incorporating transient Solar Phenomena into the wsa enlil model with the cone extension
Journal of Geophysical Research, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. McclintockAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
R. M. Dewey - One of the best experts on this subject based on the ideXlab platform.
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Improving Solar wind modeling at Mercury: Incorporating transient Solar Phenomena into the WSA‐ENLIL model with the Cone extension
Journal of Geophysical Research: Space Physics, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. Mcclintock, Dusan OdstrcilAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
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improving Solar wind modeling at mercury incorporating transient Solar Phenomena into the wsa enlil model with the cone extension
Journal of Geophysical Research, 2015Co-Authors: R. M. Dewey, Daniel N. Baker, Brian J. Anderson, Mehdi Benna, Catherine L. Johnson, Haje Korth, Daniel J. Gershman, William E. McclintockAbstract:Coronal mass ejections (CMEs) and other transient Solar Phenomena play important roles in magnetospheric and exospheric dynamics. Although a planet may interact only occasionally with the interplanetary consequences of these events, such transient Phenomena can result in departures from the background Solar wind that often involve more than an order of magnitude greater ram pressure and interplanetary electric field applied to the planetary magnetosphere. For Mercury, an order of magnitude greater ram pressure combined with high Alfven speeds and reconnection rates can push the magnetopause essentially to the planet's surface, exposing the surface directly to the Solar wind flow. In order to understand how the Solar wind interacts with Mercury's magnetosphere and exosphere, previous studies have used the Wang-Sheeley-Arge (WSA)-ENLIL Solar wind modeling tool to calculate basic and composite Solar wind parameters at Mercury's orbital location. This model forecasts only the background Solar wind, however, and does not include major transient events. The Cone extension permits the inclusion of CMEs and related Solar wind perturbations and thus enables characterization of the effects of strong Solar wind disturbances on the Mercury system. The Cone extension is predicated on the assumption of constant angular and radial velocities of CMEs to integrate these Phenomena into the WSA-ENLIL coupled model. Comparisons of the model results with observations by the MESSENGER spacecraft indicate that the WSA-ENLIL+Cone model more accurately forecasts total Solar wind conditions at Mercury and has greater predictive power for magnetospheric and exospheric processes than the WSA-ENLIL model alone.
Blanca Mendoza - One of the best experts on this subject based on the ideXlab platform.
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Assessing the relationship between Solar activity and some large scale climatic Phenomena
Advances in Space Research, 2008Co-Authors: Victor Velasco, Blanca MendozaAbstract:Abstract The nature of the climatic response to Solar variability is assessed over a long-time scale. The wavelet analysis applied to paleoclimatic proxy data of large scale atmospheric Phenomena (North Atlantic Oscillation, Atlantic Multidecadal Oscillation, Pacific Decadal Oscillation and Southern Oscillation Index) has revealed coherence between the climatic oscillations and the Solar Phenomena (the cosmogenic isotope 10 Be and the Total Solar Irradiance) preferentially with periods of Schwabe, Hale and Yoshimura–Gleissberg cycles that may reflect a modulation of Solar activity.
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An Analysis of Polar Coronal Hole Evolution: Relations to Other Solar Phenomena and Heliospheric Consequences
Solar Physics, 2001Co-Authors: Dolores Maravilla, Alejandro Lara, José F. Valdés Galicia, Blanca MendozaAbstract:We use observations of the green corona low-brightness regions to construct a time series of a polar coronal hole area from 1939 to 1996, covering 5 Solar cycles. We then perform a power-spectral analysis of the monthly data time series. Several persistent significant periodicities appear in the spectra, which are related with those found in Solar magnetic flux emergence, geomagnetic storm sudden commencements and cosmic-ray flux at Earth. Of particular importance are the peak at around 1.6–1.8 yr recently found in cosmic-ray intensity fluctuations, and the peak at around 1 yr, also identified in coronal hole magnetic flux variations. Additional interesting features are the peaks close to 5 yr, 3 yr and the possible peak at around 30 yr, that were also found in other Solar and interplanetary Phenomena. Our results stress the physical connection between the Solar magnetic flux emergence and the interplanetary medium dynamics, in particular the importance of coronal hole evolution in the structuring of the heliosphere.
