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--- science:imofmonth [2025/06/03 15:46] – [Images of the month] etienne
+++ science:imofmonth [2025/07/03 09:53] (current) – etienne
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 ===== Images of the month =====
-== THEMIS image of the month: May 2025 ==
+=== June 2025 ===
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+<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:protu:solarfilament_meteospace_2025june05.jpg"> <img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:protu:solarfilament_meteospace_2025june05.jpg" alt="Solar filament observations on June 5th 2025." style="width: 70%; height: auto;"></a></html> \\
+In June, during an observation campaign lead by researchers from the Paris Observatory (France) and the University of Wroclaw (Poland), THEMIS observed solar filaments. Solar filaments are large magnetised structure of the solar corona confining cold chromospheric-like plasma. Thanks to its specific magnetic structure, solar filaments plasma, of a temperature of about 10 000°K, "hangs" thermally isolated from the million °K solar corona. As this dense and cool plasma absorbs the light emitted from the lower solar layer, the filament appears dark relatively to the background.\\
+The THEMIS observations, presented in the left panel, results from two reconstructed images obtained from two adjacent scans over the solar filament with the THEMIS spectrograph slit. The two scans, which have a 90" range with a 0.5" spatial step, are then stitched together to obtain a larger field of view of about 110"x90". Only the reconstructed image in the core of Hα line is displayed here, but THEMIS data allow to sample the full range of the Hα line with a spectral resolution of 4mÅ.THEMIS high-resolution observations are very complementary to the observations of the [[https://www.oca.eu/fr/lag-physol-projects?option=com_content&view=category&layout=blog&id=295&Itemid=908 | Meteospace/3SOLEIL]] solar surveillance service of OCA/CNRS-INSU, which provide full-Sun high cadence (every 10s) Hα observations, presented on the right panel. \\
+Thanks to its high-resolution, as illustrated in the left panel, THEMIS permits to analyse the filamentary structure of the solar filament and understand its magnetic field thanks to THEMIS polarised measurements. In particular, the magnetic properties of the "barbs" of the filament, the features which extend away from the "spine" (the filament axis), remains ill understood and an active topic of research.
+\\
+</columns>
+=== May 2025 ===
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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> \\
-**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). \\
 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.
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 === April 2025 ===
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-<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:ar:activeregionbestof_6x2.jpg"> <img src="https://www.themis.iac.es/lib/exe/fetch.php?media=results:gallery:ar:activeregionbestof_6x2.jpg" alt="2022-2025 THEMIS sunspot best-of" style="width: 100%; height: auto;"></a></html>
+<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:ar:activeregionbestof_6x2.jpg"> <img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:ar:activeregionbestof_6x2.jpg" alt="2022-2025 THEMIS sunspot best-of" style="width: 100%; height: auto;"></a></html>
 \\
 A selection of THEMIS sunspot observations obtained between 2022 and 2025 with the [[technical:description#broadband_imaging_bbi_filter_camera | BroadBand Imaging Camera]]. Observations are performed using [[technical:tao|Themis Adaptive Optics]] and images are processed with a Knox-Thompson image-reconstruction method. </columns>