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5 results on '"prominences -Sun"'

1. Observations of a prominence eruption and loop contraction

Author

Pascal Démoulin, Brigitte Schmieder, Ramesh Chandra, Pooja Devi, Reetika Joshi, Bhuwan Joshi, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, magnetic fields -Sun, Flux, Astrophysics, 01 natural sciences, law.invention, CORONAL MASS EJECTION, prominences, INITIATION, law, MAGNETIC RECONNECTION, prominences -Sun, Coronal mass ejection, RHESSI, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Sun, FLARE, flares, Magnetic flux, IMPLOSION, Astrophysics - Solar and Stellar Astrophysics, magnetic fields [Sun], Physical Sciences, Physics::Space Physics, Flare, filaments [Sun], FOS: Physical sciences, Context (language use), Astronomy & Astrophysics, ACCELERATION, Computer Science::Digital Libraries, Lateral loop, 0103 physical sciences, filaments, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Science & Technology, Astronomy and Astrophysics, Physics::History of Physics, Vortex, MODEL, flares [Sun], 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], FLUX ROPES, Rope
Abstract

Context. Prominence eruptions provide key observations to understand the launch of coronal mass ejections as their cold plasma traces a part of the unstable magnetic configuration. Aims. We select a well observed case to derive observational constraints for eruption models. Methods. We analyze the prominence eruption and loop expansion and contraction observed on 02 March 2015 associated with a GOES M3.7 class flare (SOL2015-03-02T15:27) using the data from Atmospheric Imaging Assembly (AIA) and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). We study the prominence eruption and the evolution of loops using the time-distance techniques. Results. The source region is a decaying bipolar active region where magnetic flux cancellation is present for several days before the eruption. AIA observations locate the erupting prominence within a flux rope viewed along its local axis direction. We identify and quantify the motion of loops in contraction and expansion located on the side of the erupting flux rope. Finally, RHESSI hard X-ray observations identify the loop top and two foot-point sources. Conclusions. Both AIA and RHESSI observations support the standard model of eruptive flares. The contraction occurs 19 minutes after the start of the prominence eruption indicating that this contraction is not associated with the eruption driver. Rather, this prominence eruption is compatible with an unstable flux rope where the contraction and expansion of the lateral loop is the consequence of a side vortex developing after the flux rope is launched., Comment: 16 pages, 9 figures, 1 table, and appendix

Published
2021

2. Modelling and observations: Comparison of the magnetic field properties in a prominence

Author

Yang Su, Brigitte Schmieder, A. López Ariste, Duncan H. Mackay, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), European Research Council, Science & Technology Facilities Council, University of St Andrews. Applied Mathematics, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Field (physics), Flux, Context (language use), Field strength, Astrophysics, magnetic fields, 01 natural sciences, Solar prominence, 0103 physical sciences, prominences -Sun, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, filaments, QC, QB, 0105 earth and related environmental sciences, Line (formation), Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Sun, Astronomy and Astrophysics, 3rd-DAS, Computational physics, Magnetic field, QC Physics, magnetic fields [Sun], Space and Planetary Science, filaments, prominences [Sun], Rope
Abstract

Context. Direct magnetic field measurements in solar prominences occur infrequently and are difficult to make and interpret. As a consequence, alternative methods are needed to derive the main properties of the magnetic field that supports the prominence mass. This is important for our understanding of solar prominences, but also for understanding how eruptive prominences may affect space weather. Aims. We present the first direct comparison of the magnetic field strength derived from spectro-polarimetric observations of a solar prominence, with corresponding results from a theoretical flux rope model constructed from on-disc normal component magnetograms. Methods. We first used spectro-polarimetric observations of a prominence obtained with the magnetograph THEMIS operating in the Canary Islands to derive the magnetic field of the observed prominence by inverting the Stokes parameters measured in the He D3 line. Next, we constructed two data-constrained non-linear force-free field (NLFFF) models of the same prominence. In one model we assumed a strongly twisted flux rope solution, and in the other a weakly twisted flux rope solution. Results. The physical extent of the prominence at the limb (height and length) is best reproduced with the strongly twisted flux rope solution. The line-of-sight average of the magnetic field for the strongly twisted solution results in a magnetic field that has a magnitude of within a factor of 1−2 of the observed magnetic field strength. For the peak field strength along the line of sight, an agreement to within 20% of the observations is obtained for the strongly twisted solution. The weakly twisted solution produces significantly lower magnetic field strengths and gives a poor agreement with the observations. Conclusions. The results of this first comparison are promising. We found that the flux rope insertion method of producing a NLFFF is able to deduce the overall properties of the magnetic field in an observed prominence.

Published
2020

3. Filaments and the magnetic configuration. I. Observation of the solar case

Author

N. Meunier, X. Delfosse, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
activity -Sun, Solar surface, macromolecular substances, Astrophysics, 01 natural sciences, Solar prominence, Protein filament, prominences -Sun, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, activitystars, filaments, 010303 astronomy & astrophysics, Physics, Pixel, 010308 nuclear & particles physics, chromospheres, Sun, chromosphere -Sun, Astronomy and Astrophysics, Observable, Magnetic field gradient, Large sample, Stars, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, magnetic topology -stars, Physics::Space Physics
Abstract

International audience; Context. The emission of Ca and Hα is correlated for the Sun, but this does not seem to be true for other stars. We previously demonstrated that this lack of correlation could be due to the presence of filaments. Aims. We aim to establish a link between the activity level, the magnetic configuration, and the number of filaments, and therefore with observables of other stars that the Sun. Methods. We studied the relationship between the filaments and the magnetic configuration using a large scale approach on MDI/SOHO magnetograms and a large sample of filaments. We validated the reconstruction of synthetic time series of filament surface coverage representative of the magnetic configuration, and then apply it to observations over a full solar cycle. Results. We derived quantitative criteria that relates the presence of filaments to the properties at polarity inversion lines, hereafter PIL, magnetic field gradient, and unipolar areas on the solar surface (size and distance to these areas). We also observed that the number of PIL pixels is anti-correlated with the activity level, and the increase in filament surface coverage is due to the modification of the PIL pixel properties. We reconstructed synthetic time series of filaments that are in good agreement with observations. Conclusions. This work validates our method, which will later be applied to solar and stellar simulations.

Published
2011

4. Oscillations in a solar filament: first observation of long periods in the HeI 584.33 Å line, modelling and diagnostic

Author

J. Solomon, Karine Bocchialini, G. Pouget, Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics, 01 natural sciences, magnetohydrodynamics (MHD), Solar prominence, Protein filament, symbols.namesake, 0103 physical sciences, prominences -Sun, waves, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), Physics, Spectrometer, oscillations -Sun, UV radiation -Sun, Sun, Astronomy and Astrophysics, Magnetic field, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Temporal resolution, symbols, Magnetohydrodynamics, Doppler effect, filaments -Sun
Abstract

International audience; Three long observations of filaments were carried out in the 584.33 Å HeI line during MEDOC campaigns in November 2003 and November 2004, by the Coronal Diagnostic Spectrometer onboard SOHO. Their duration was 15−16 h and the temporal resolution was 20 s, allowing measurements of the entire range of periodicities theoretically expected in a filament (particularly both the short periods, less than 10 min, and the long ones, more than 40 min). Fourier analysis of the Doppler velocities in the filament allows us to detect oscillations over a wide range, and particularly very slow velocity oscillations (5−6 h) that were not detected previously. We test an earlier interpretation of these velocity oscillations in the prominence model of Joarder & Roberts (1993, A&A, 277, 225), who treat the prominence as a slab. We used a systematic method to identify the six fundamental modes predicted by the model among the numerous frequencies detected. Identification of these modes-and especially the slowest one, the slow kink mode-provides a complete diagnostic of the filament in terms of the Alfvén speed, temperature, and angle between the magnetic field and the main axis of the filament.

Published
2006

5. Full-Stokes spectropolarimetry of solar prominences

Author

V. Bommier, M. Semel, A. López Ariste, Frédéric Paletou, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Télescope héliographique pour l'étude du magnétisme et des instabilites solaires (THEMIS), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
010504 meteorology & atmospheric sciences, Astrophysics, 01 natural sciences, Solar prominence, Preliminary analysis, symbols.namesake, prominences -Sun, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, Zeeman effect, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Sun, Astronomy, Astronomy and Astrophysics, Polarization (waves), Magnetic field, magnetic fields -polarization, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; We report on first spectropolarimetric observations of solar prominences made at THEMIS. Hereafter we shall emphasis on the preliminary analysis of He i D3 full-Stokes observations. Our measurements clearly show manifestations of both the Hanle and Zeeman effects. More generally, we demonstrate the very favourable performances of the THEMIS multi-line spectropolarimetric mode for further new investigations of the magnetic field in solar prominences.

Published
2001

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