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This shows you the differences between two versions of the page.

--- themis [2025/06/26 11:41] – etienne
+++ themis [2025/09/08 16:58] (current) – etienne
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+<color red >   ** New :** </color>
+[[science:resources | Downloadable posters highlighting recent high-resolution observations of solar active regions by THEMIS]]\\
 Click for information on: \  \  **[[admin:location| How to reach THEMIS locations]]** \ ; \ **[[admin:contacts| How to contact the THEMIS team]]**
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-<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=dsc7357.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=dsc7357.jpg" style="width:90%; height:auto;"></a></html>
+/*WINTER PIC*/
+/*<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:dsc7357.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=dsc7357.jpg" style="width:90%; height:auto;"></a></html>*/
+/* SPRING PIC */
+<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=themis_spring25.jpg"><img src="https://www.themis.iac.es/lib/exe/fetch.php?media=themis_spring25.jpg" style="width:90%; height:auto;"></a></html>
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 === Observing with THEMIS  ===
 **[[observation| Information for research scientists wishing to observe with THEMIS]]** \\
-**[[observation:2025campaign#2025 campaign schedule | Schedule of 2025 observing campaign]** \\
+**[[observation:2025campaign#2025 campaign schedule | Schedule of 2025 observing campaign]]** \\
 [[observation:weather | Weather at THEMIS location and weather forecast]] \\
 [[observation:data| THEMIS data products & data access]]
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-== THEMIS image of the month: May 2025 ==
+== THEMIS image of the month: August 2025 ==
+=== August 2025 ===
+<columns 100% l 60>
+<html> <a href="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:protu:limbprominenceobservation_20250506_withandwithoutao.jpg
+"> <img src="https://www.themis.iac.es/lib/exe/fetch.php?media=science:gallery:protu:limbprominenceobservation_20250506_withandwithoutao.jpg
+" alt="Prominence Halpha observations at limb: Adaptive Optics comparison" style="width: 100%; height: auto;"></a></html> \\
+<newcolumn 40%>
+During the 2025 observation campaign of Brigitte Schmieder and Arek Berlicki, THEMIS targeted a small prominence. Prominence are emitting structures that can be observed at the solar limb, beyond the outer edge of the Sun's disk. Prominences and filaments are two aspects of an unique physical feature: a domain of cold chromosphere like plasma, magnetically confined in the much hotter solar corona. While this structure appears as dark when seen in contrast with the disk, and is then called a filament, it appears bright in contrast to the plane of sky. As a magnetised structure filament/prominence can erupt, releasing plasma and material toward the solar system. Understanding how the magnetic structure them is fundamental to comprehend their stability or lack off.
+THEMIS is mainly a [[technical:mtr2 | scanning spectrograph instrument]], i.e. a very thin slit scans the region of interest, in order to obtain high resolution spectrograms. THEMIS images are thus reconstructed. While scanning, THEMIS is thus very sensitive to the effect of turbulence and the reconstructed image have necessarily a lower resolution that direct imaging. On the other hand, THEMIS can deliver simultaneous images at different wavelength.
+\\
+</columns>
-<columns 80% l >
+While adaptive optics can generally be used to significantly improve on disc observations, such as with our own [[technical:tao|Themis AO]], AOs fail when trying to observe over the limb because no structure there can be tracked by the AO. Recently our colleagues of the U.S. National Science Foundation National Solar Observatory and New Jersey Institute of Technology, observed [[https://nso.edu/press-release/new-adaptive-optics-shows-stunning-details-of-our-stars-atmosphere/ | beautiful prominence dynamics]] with the Goode Solar Telescope thanks to their [[https://www.nature.com/articles/s41550-025-02564-0 |new coronal adaptive optics]] in a direct imaging approach.
-<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: 100%; 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). \\
+At THEMIS, during our 2025 campaign we tried a different approach. While we were scanning a prominence at the limb, we use TAO on an offset region which is close to the limb while still on the disc. TAO is a simple AO which isoplanatic region (region where most of the AO correction is done) is limited. Since the isoplanatic region and the region of scientific interest are far away, the AO correction may be limited at the prominence. We were however very please to see that TAO still provide significant improvements. As can be seen in this image of the month, the turbulence induced motions (in the direction of the slit) which are present when TAO is off, are strongly reduced when TAO is switched on. The limb appears much smoother and the prominence better resolved.
-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.
-Adapted from [[https://doi.org/10.1016/j.pss.2013.03.002]| Mangano et al. 2013]]. \\
- </columns>