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| science:imofmonth [2025/06/03 15:46] – [Images of the month] etienne | science:imofmonth [2025/06/03 15:47] (current) – etienne |
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| <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:mercury:mercury_mangano2013.jpg"> <img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:mercury:mercury_mangano2013.jpg" alt="Hourly dynamics of Sodium emission on Mercury" style="width: 70%; height: auto;"></a></html> \\ | <html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:mercury:mercury_mangano2013.jpg"> <img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:mercury:mercury_mangano2013.jpg" alt="Hourly dynamics of Sodium emission on Mercury" style="width: 70%; height: auto;"></a></html> \\ |
| **May was Mercury Month a theMis! : ** This past month of May took place the usual annual observation campaign of Mercury, led by researchers from the Italian National Institute of Astrophysics (INAF/IAPS in Rome) in collaboration with scientist from the French Laboratoire Atmosphères, Observations Spatiales (LATMOS/CNRS-UVSQ-SU-CNES in Paris). \\ | **May was Mercury Month a theMis! : ** In May 2025 took place the usual annual observation campaign of Mercury, led by researchers from the Italian National Institute of Astrophysics (INAF/IAPS in Rome) in collaboration with scientist from the French Laboratoire Atmosphères, Observations Spatiales (LATMOS/CNRS-UVSQ-SU-CNES in Paris). \\ |
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| In a sequence of scans of the exosphere of Mercury obtained some years ago, THEMIS could follow the hourly evolution of the reconstructed distribution of the Sodium emission. The figure displays the intensity emission (in kiloRayleigh) after preliminary reduction, including bias and sky background subtraction, as well as spectral and flux calibrations. Solid white line highlights the disk of the planet, the cross indicating the center of the disk. Mercury disk is 6.0'' wide. The Sun is located on the left. The images show the two peaks of higher intensity at high hermian latitude in the direction of the Sun. These peaks of sodium emission are roughly co-spatial with the positions of the magnetic footprints. Their evolution is due to the link of such emission with the Mercury magnetosphere and the interaction with the varying solar wind particles penetrating the magnetosphere and flowing to the surface. | In a sequence of scans of the exosphere of Mercury obtained some years ago, THEMIS could follow the hourly evolution of the reconstructed distribution of the Sodium emission. The figure displays the intensity emission (in kiloRayleigh) after preliminary reduction, including bias and sky background subtraction, as well as spectral and flux calibrations. Solid white line highlights the disk of the planet, the cross indicating the center of the disk. Mercury disk is 6.0'' wide. The Sun is located on the left. The images show the two peaks of higher intensity at high hermian latitude in the direction of the Sun. These peaks of sodium emission are roughly co-spatial with the positions of the magnetic footprints. Their evolution is due to the link of such emission with the Mercury magnetosphere and the interaction with the varying solar wind particles penetrating the magnetosphere and flowing to the surface. |
