B. Schmieder

Observatoire de Paris

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Papers

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i-10 index

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Document Type

Co-Authors

G. Aulanier

Observatoire de Paris

138

P. Démoulin

Observatoire de Paris

104

P. Mein

Observatoire de Paris

P. Heinzel

Czech Academy of Sciences, Astronomical Institute

Ramesh Chandra

Kumaun University

L. van Driel‐Gesztelyi

Laboratoire d’études spatiales et d’instrumentation en astrophysique

N. Mein

Laboratoire d’études spatiales et d’instrumentation en astrophysique

Jean-Marie Malherbe

Observatoire de Paris

C. H. Mandrini

Institute of Astronomy and Space Physics

Stefaan Poedts

KU Leuven

Cooperative Institutions

Centre National de la Recherche Scientifique

218

Goddard Space Flight Center

116

Instituto de Astrofísica de Canarias

115

Université Paris Cité

Sorbonne Université

Max Planck Institute for Solar System Research

Observatoire de Paris

Laboratoire d’études spatiales et d’instrumentation en astrophysique

Max Planck Society

Heliophysics

Author Statistics

Papers

Citation

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Research Field

Dynamics and evolution of the post-flare loops of June 1992

Advances in Space Research (1997)

J. E. Wiik L. Van Driel-Gesztely B. Schmieder P. Heinzel

Flare

Solar flare

10.1016/s0273-1177(97)00907-1

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Citations (1)

The role of magnetic bald patches in surges and arch filament systems

Astronomy and Astrophysics (2002)

C. H. Mandrini P. Démoulin B. Schmieder Yuanyong Deng P. Rudawy

The short-lived active region (AR) NOAA 7968 was thoroughly observed all along its disk transit (June 3 to 10, 1996) from space and from the ground. During the early stage of its evolution, flux emerged in between the two main polarities and arch filament systems (AFS) were observed to be linked to this emergence. New bipoles and a related surge were observed on June 9. We have modeled the magnetic configuration of AR 7968 using a magnetohydrostatic approach and we have analyzed its topology on June 6 and June 9 in detail. We have found that some of the AFS and the surge were associated with field lines having dips tangent to the photosphere (the so called "bald patches", BPs). Two interacting BP separatrices, defining a separator, have been identified in the configuration where these very different events occurred. The observed evolution of the AFS and the surge is consistent with the expected results of magnetic reconnection occuring in this magnetic topology, which is specific to 3D configurations. Previously BPs have been found to be related to filament feet, small flares and transition region brightenings. Our results are evidence of the importance of BPs in a much wider range of phenomena, and show that current layers can be formed and efficiently dissipated in the chromosphere.

Chromosphere

10.1051/0004-6361:20020745

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Citations (53)

The magnetic nature of wide EUV filament channels and their role in the mass loading of CMEs

Astronomy and Astrophysics (2002)

G. Aulanier B. Schmieder

Previous works have shown that dark and wide EUV filament channels observed at Å are due to absorption of EUV lines in cool plasma condensations that are not observed in . We extend this interpretation and we address the issue of the possible injection of their mass into CMEs, through the magneto-hydrostatic modeling in 3D of one filament observed both in and in EUV. The model parameters are fixed so as to match the observations only. Further comparison of the model with the EUV observations reveal the magnetic nature of the absorbing plasma condensations. They are formed in magnetic dips, as for the filament itself. Opacity ratios and the hydrostatic condition imply that the dips must be filled by cool material up to 1700 km, which increases the filament mass by 50% as compared to estimations. Far from the filament, the absorbing condensations are located below 4 Mm in altitude above the photosphere, on the edge of weak photospheric parasitic polarities, within the lower parts of long field lines overlaying the filament. By physical analogy with filament feet, we redefined these extended regions as EUV feet. The broadening of the EUV filament channel is dominated by EUV feet, while the larger filling of dips plays a non-negligible but minor role. Further implications from this work are discussed, on the visibility and the geometry of the condensations, on the existence of EUV filament channels in the absence of filaments, on the loading of cool material into filament feet through bald patch reconnection and on the complex geometry of the upper prominence-corona transition region. The magnetic topology implies that during the filament eruption, the mass of its wide EUV feet will not contribute to the CME, whereas the extra mass provided by the large filling of dips in the filament flux tube will be loaded into the CME.

Extreme Ultraviolet Lithography

Solar prominence

Photosphere

Extreme ultraviolet

Opacity

10.1051/0004-6361:20020179

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Citations (86)

Chromospheric Recurrent Jets in a Sunspot Group and Their Intergranular Origin

The Astrophysical Journal (2022)

Jie Zhao Jiangtao Su Xu Yang Hui Li B. Schmieder

Abstract We report on high-resolution observations of recurrent fan-like jets by the Goode Solar Telescope in multiple wavelengths inside a sunspot group. The dynamics behavior of the jets is derived from the H α line profiles. Quantitative values for one well-identified event have been obtained, showing a maximum projected velocity of 42 km s −1 and a Doppler shift of the order of 20 km s −1 . The footpoints/roots of the jets have a lifted center on the H α line profile compared to the quiet Sun, suggesting a long-lasting heating at these locations. The magnetic field between the small sunspots in the group shows a very high resolution pattern with parasitic polarities along the intergranular lanes accompanied by high-velocity converging flows (4 km s −1 ) in the photosphere. Magnetic cancellations between the opposite polarities are observed in the vicinity of the footpoints of the jets. Along the intergranular lanes horizontal magnetic field around 1000 G is generated impulsively. Overall, all the kinetic features at the different layers through the photosphere and chromosphere favor a convection-driven reconnection scenario for the recurrent fan-like jets and evidence a site of reconnection between the photosphere and chromosphere corresponding to the intergranular lanes.

Chromosphere

Sunspot

Photosphere

Solar telescope

Line (geometry)

10.3847/1538-4357/ac6e3b

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Citations (4)

Magnetic Field Structures in a Facular Region Observed by THEMIS and Hinode

Solar Physics (2010)

Yang Guo B. Schmieder V. Bommier Sanjay Gosain

Flux tube

Line (geometry)

Photosphere

Solar atmosphere

10.1007/s11207-010-9519-2

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Citations (4)

International Heliophysical Year in Europe

HAL (Le Centre pour la Communication Scientifique Directe) (2005)

Carine Briand Jean‐Louis Bougeret J. A. Bonet Navaro A. Breen M. Candidi

Source

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Citations (0)

Preface: Magnetic flux ropes in solar environments

Advances in Space Research (2022)

C. H. Mandrini B. Schmieder

10.1016/j.asr.2022.06.074

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Citations (0)

Electric Current Evolution at the Footpoints of Solar Eruptions

The Astrophysical Journal (2020)

K. Barczyński G. Aulanier Miho Janvier B. Schmieder S. Masson

Electric currents play a critical role in the triggering of solar flares and their evolution. The aim of the present paper is to test whether the surface electric current has a surface or subsurface fixed source as predicts the circuit approach of flare physics, or is the response of the surface magnetic field to the evolution of the coronal magnetic field as the MHD approach proposes. Out of all 19 X-class flares as observed by SDO from 2011 to 2016 near the disk center, we analyzed the only 9 eruptive flares for which clear ribbon-hooks were identifiable. Flare ribbons with hooks are considered to be the footprints of eruptive flux ropes in MHD flare models. For the first time, fine measurements of time-evolution of electric currents inside the hooks in the observations as well as in the OHM 3D MHD simulation are performed. Our analysis shows a decrease of the electric current in the area surrounded by the ribbon hooks during and after the eruption. We interpret the decrease of the electric currents as due to the expansion of the flux rope in the corona during the eruption. Our analysis brings a new contribution to the standard flare model in 3D.

Flare

Solar flare

Electric current

Corona (planetary geology)

10.3847/1538-4357/ab893d

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Citations (2)

L'atmosphère du Soleil

HAL (Le Centre pour la Communication Scientifique Directe) (2011)

B. Schmieder G. Aulanier

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