MASFIPRO · The three-dimensional Magnetic Structure of solar Filaments and Prominences
7РП — „Хора“ (Действия „Мария Кюри“)
- Период
- 2014-01-01 → 2015-12-31
- Финансиране от ЕС
- 173 371 €
- Участници
- 1
- Схема
- MC-IIF
Линиите свързват координатора с партньорите.
Накратко на български
Слънчевите филаменти и проминаенции са огромни плазмени структури, чието триизмерно магнитно поле се анализира чрез специални телескопи. Това помага за разбирането на механизмите при изхвърлянето на слънчева маса, което е важно за прогнозирането на космическото време.
Кратко обяснение, генерирано от езиков модел по текста на CORDIS. Оригиналът е по-долу.
Резултати накратко
The three-dimensional Magnetic Structure of solar Filaments and Prominences
The determination of the vector magnetic field in solar filaments and prominences (filaments seen against the background sky of the solar limb) is of paramount importance for Solar and Stellar Physics. Solar filaments are one of the most prominent plasma structures that can be seen in our Sun extending from the solar surface and into the hot solar Corona. These structures are embedded in a large magnetic skeleton that provides the means of their support in the solar chromosphere and low corona. Therefore, their magnetic characterization provides an effective way for understanding the magnetic coupling between the Photosphere, Chromosphere, and Corona. More importantly, this characterization is important for Space-Weather forecasting dice these magnetic structures may eventually destabilize and give rise to the ejection of solar filaments that, when the involved energetics are large enough, become Coronal Mass Ejections (CMEs). The main objectives of this project were to observe solar filaments simultaneously in the Photosphere and in the Chromosphere, to characterize in quantitative detail their magnetic structure, to follow their evolution, and to investigate possible mechanisms behind filament eruptions and generation of CMEs. During the project, observations of different solar structures in the 1083 nm spectral region have been taken with the GREGOR and VTT (Vacuum Tower Telescope) german telescopes installed at the Izaña Observatory in Tenerife (Spain). The observations have been analyzed with the HAZEL (HAnle and ZEeman Light) inversion code that, from the interpretation of the intensity and polarization signals of the He I 1083 nm triplet spectral line, provide the wanted vector magnetic field information. In particular, during the project it has been possible to: 1- Obtain, for the first time, the variation of the vector magnetic field with height in the so-called solar spicules. This result has a strong impact in the current understanding and modeling of solar spicules and will help understand the physics behind their formation mechanism. 2- Observe a solar filament before it was ejected from the solar surface. The analysis of the spectropolarimetric data and of the Large Amplitude Oscillations the filament exhibits, will help understanding the eruption of this particular solar filament. 3- Obtain data of a quiescent prominence with very high spatial resolution. The data revealed the presence of small-scale structures in intensity and polarization. 4-Detect, for the very first time, a direct spectropolarimetric signature of reconnection jets in the solar atmosphere.
Текст от CORDIS, на английски · Данни: CORDIS, © Европейски съюз
Цел на проекта
Solar filaments are prominent cold and dense structures of plasma suspended in the hot corona. They are called prominences when observed above the solar limb. Despite they were probably the first solar features to be observed, the magnetic structure of solar filaments is still largely unknown, being their determination a fundamental problem for Solar Physics. The reason is the lack of chromospheric observables able to provide binding information for the magnetic field. Therefore, though there are two main proposed models, namely sheared-arcade and twisted flux-rope models, due to the lack of observational constraints it is unclear what is the filament most probable magnetic configuration. High-spatial resolution observations have revealed that filaments are also highly structured at very small scales. Remarkably, most solar filaments erupt, giving rise to coronal mass ejection. Thus, the understanding of solar filaments is also important for space-weather forecasting. To infer their magnetic structure it is crucial to observe the formation and evolution of solar filaments in the Photosphere and in the Chromosphere, in polarized light, and at the highest spatial resolution. We propose to observe solar filaments with the Tenerife Infrared Polarimeter (TIP-II) installed at the GREGOR ground-based 1.5-meter telescope in synchrony with the Hinode space-based observatory. I will use TIP-II to observe the 1083.0 nm spectral region containing a photospheric line and the chromospheric He I 1083.0 nm triplet. This line is sensitive to atomic level polarization and to the joint action of the Hanle and Zeeman effects. Thus, it is ideal for determining a wide range of field strengths in prominences. The data will be analyzed using state-of-the art inversion algorithms. Finally, Hinode will provide a wealth of binding information for the determination of the magnetic structure of solar filaments and also for identify possible trigger mechanism of filament eruption.
Оригинален текст от CORDIS (на английски).
Участници
- INSTITUTO DE ASTROFISICA DE CANARIAS · SAN CRISTOBAL DE LA LAGUNAКоординаторИспания
Връзки
Данни: CORDIS, © Европейски съюз