Delayed, Line-dependent Reorganization of Pore Oscillations Following a Compact C8.2 Flare Observed by S unrise iii /SUSI
Year: 2026
Type: article
Abstract: Magnetic oscillations permeating the solar atmosphere can be altered by flares. This could be due to changes in the atmospheric magnetic waveguide, the thermodynamic stratification, or both. To investigate this, we examine oscillations in a magnetic pore crossed in part by the ribbon of a C8.2 flare, using observations from the S unrise Ultraviolet Spectropolarimeter and Imager (SUSI) aboard S unrise iii . We track the core intensities of eight spectral lines between 327–329 nm and show that oscillatory power in the 4.2–7.0 mHz range, measured around 30 minutes after the flare peak, exceeds the preevent value in all eight lines by factors of 1.60–8.71. Conversely, in the 7.0–11.5 mHz band, the postevent intensity power is lower—approximately 0.13–0.41 of the original power in seven of the observed lines. Line-center velocity measurements support the lower-frequency enhancement. This delayed, line-dependent shift toward the lower-frequency band is consistent with flare-induced changes in wave transmission, reflection, or resonant response, although thermodynamic and magnetic effects cannot yet be separated.
Authors: Shahin Jafarzadeh, David B. Jess, Marco Stangalini, Lyndsay Fletcher, Ryan O. Milligan, Paulo J. A. Simões, Peter H. Keys, Sami K. Solanki, H. N. Smitha, Andreas Lagg, Achim Gandorfer, Alex Feller, Francisco A. Iglesias, Tino L. Riethmüller, Bianca Grauf, Johannes Hoelken, Jose Carlos del Toro Iniesta, Yukio Katsukawa, Pietro Bernasconi, Thomas Berkefeld, Alberto Álvarez-Herrero, Masahito Kubo, David Orozco Suárez, Michael Carpenter, Alexander Bell, Valentín Martínez Pillet, Francisco Javier Bailén, Julian Blanco Rodríguez, Juan Sebastián Castellanos Durán, Edvarda Harnes, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Takuma Matsumoto, Takayoshi Oba, Azaymi L. Siu-Tapia, Hanna Strecker, Dušan Vukadinović
Institutions: Queen's University Belfast, Max Planck Institute for Solar System Research, California State University, Northridge, Agenzia Spaziale Italiana, University of Oslo, Scottish Universities Physics Alliance, Universidade Presbiteriana Mackenzie, University of Mendoza, Instituto de Astrofísica de Andalucía, The Graduate University for Advanced Studies, SOKENDAI, National Astronomical Observatory of Japan, The University of Tokyo, Johns Hopkins University Applied Physics Laboratory, Institut für Sonnenphysik, Instituto Nacional de Técnica Aeroespacial, Instituto de Astrofísica de Canarias, Universitat de València, National Institute for Fusion Science, Nagoya University, Kanazawa University
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: gold
Estimated APC paid: $2,400
Funders: National Aeronautics and Space Administration, Max-Planck-Förderstiftung, Leverhulme Trust, Royal Society, European Commission, Conselho Nacional de Desenvolvimento Científico e Tecnológico, Universitetet i Oslo, Norges Forskningsråd, Instituto de Astrofísica de Andalucía, Science and Technology Facilities Council, Japan Society for the Promotion of Science, Japan Aerospace Exploration Agency, Agencia Estatal de Investigación
Awards: G1171257612, G2028935194, G2124616825, Queen's University Belfast Consolidated Grant in Solar Physics and Solar System Studies 2020 - 2023, SUMMARY SUNRISE IS A BALLOON-BORNE SOLAR OBSERVATORY DEDICATED TO THE INVESTIGATION OF THE PHYSICS GOVERNING THE EVOLUTION OF THE MAGNETIC FIELD AND THE CONVECTIVE PLASMA FLOWS IN THE LOWER SOLAR ATMOSPHERE. THESE PROCESSES ARE CRUCIAL FOR OUR UNDERSTANDING OF THE MAGNETIC ACTIVITY OF THE SUN AND OF THE OUTWARD TRANSPORT OF ENERGY TO HEAT ITS OUTER ATMOSPHERE AND TO FUEL THE ERUPTIONS AND CORONAL MASS EJECTIONS I.E. PHENOMENA THAT DRIVE SPACE WEATHER. THE SUNRISE OBSERVATORY IS DESIGNED FOR OPERATION IN THE STRATOSPHERE (AT HEIGHTS AROUND 36 KM) TO AVOID THE IMAGE DEGRADATION DUE TO TURBULENCE IN THE EARTH S LOWER ATMOSPHERE AND TO GAIN ACCESS TO THE UV WAVELENGTHS DOWN TO 200NM. A 1-M-DIAMETER TELESCOPE (THE LARGEST SOLAR TELESCOPE FLOWN TO-DATE) FEEDS AN UV IMAGER AND AN IMAGING FILTER MAGNETOGRAPH. SUNRISE WAS FLOWN TWICE IN JUNE 2009 AND JUNE 2013 DURING PERIODS OF VERY LOW AND HIGH SOLAR ACTIVITY RESPECTIVELY AND THE OBSERVATIONS RESULTED IN OVER 60 PEERREVIEWED PUBLICATIONS SO FAR. THE 3RD FLIGHT PROPOSED HERE WILL INCLUDE SUBSTANTIAL IMPROVEMENTS IN THE SUNRISE INSTRUMENTATION A NEW HIGHLY STABLE GONDOLA AND A SET OF STRONG SCIENCE OBJECTIVES TO ADDRESS ALL THREE OF NASA S HELIOPHYSICS SCIENCE GOALS IN THE 2014 SCIENCE PLAN. OBJECTIVES THE FIRST TWO SCIENCE FLIGHTS OF SUNRISE HAVE BEEN HIGHLY SUCCESSFUL. HOWEVER THESE RESULTS HAVE BEEN MAINLY RESTRICTED TO THE SOLAR PHOTOSPHERE AND BEG THE QUESTION OF WHAT INFLUENCE THE DYNAMICAL AND MAGNETIC PHENOMENA STUDIED IN THE EARLIER SUNRISE FLIGHTS HAVE ON THE HIGHER ATMOSPHERE IN PARTICULAR THE CHROMOSPHERE. THIS WILL CHANGE WITH THE THIRD SUNRISE FLIGHT WHICH WILL CARRY INSTRUMENTS TO SAMPLE THE CHROMOSPHERE IN A MULTITUDE OF SPECTRAL LINES OVER A BROAD WAVELENGTH RANGE (300 860 NM). THE INVESTIGATION WILL FOCUS ON THE FOLLOWING SCIENCE OBJECTIVES: WHAT IS THE STRUCTURE OF THE CHROMOSPHERIC MAGNETIC FIELD IN DIFFERENT TYPES OF SOLAR REGIONS? HOW WELL IS THIS MAGNETIC STRUCTURE REPRODUCED BY FORCE-FREE EXTRAPOLATIONS FROM THE PHOTOSPHERE? WHICH IS MORE IMPORTANT FOR HEATING THE SUN'S UPPER ATMOSPHERE FIELD LINE BRAIDING OR (MAGNETOHYDRODYNAMIC) WAVE FLUX? HOW IS MAGNETIC FLUX REMOVED FROM THE SURFACE OF THE SUN? HOW IMPORTANT IS MAGNETIC RECONNECTION IN THIS RESPECT? METHODOLOGY FOR ITS THIRD FLIGHT SUNRISE WILL CARRY TWO NEW INSTRUMENTS AND A MAJOR UPGRADE OF ONE OF ITS CURRENT INSTRUMENTS. THE NEW INSTRUMENTS ARE A NOVEL UV SPECTROPOLARIMETER (TO BE BUILT BY MPS) TO EXPLORE AND EXPLOIT THE EXCITING BUT DUE TO ITS POOR ACCESSIBILITY FROM THE GROUND VERY POORLY STUDIED SPECTRAL RANGE BETWEEN 300 AND 420 NM AND A VISIBLE-INFRARED SPECTROPOLARIMETER TO BE BUILT JOINTLY BY NAOJ AND ISAS IN JAPAN MPS AND IAA IN SPAIN. THE IMAGING MAGNETOGRAPH IMAX WILL BE UPGRADED TO GREATLY INCREASE ITS SPEED AND TO ALLOW IT TO ACCESS MULTIPLE SPECTRAL LINES (COMPARED WITH A SINGLE ONE SO FAR). THE BALLOON WILL BE LAUNCHED FROM ESRANGE SPACE CENTER IN KIRUNA SWEDEN WITH EXPECTED FLIGHT DURATION OF 7 DAYS AROUND THE SUMMER SOLSTICE IN 2020. THE MISSION IS A COLLABORATION BETWEEN APL (USA) MPS (GERMANY) NAOJ (JAPAN) AND IAA (SPAIN). THIS PROPOSAL WILL FUND THE USA CONTRIBUTION TO THE SUNRISE COLLABORATION. THIS CONTRIBUTION INCLUDES: BUILDING AND FLYING THE STABLE OBSERVING PLATFORM (THE GONDOLA AND ALL ITS SUBSYSTEMS) PROVIDE COORDINATION FOR A JOINT OBSERVING CAMPAIGN WITH THE 4-M APERTURE DKIST GROUND BASED SOLAR TELESCOPE AND THE USA PARTICIPATION IN SCIENCE OBJECTIVES DEFINITIONS AND OBSERVATIONS PLANNING AS WELL AS POST FLIGHT DATA ANALYSIS INTERPRETATION AND RESULTS PUBLICATIONS., G3160769488, Consolidated Grant in Solar Physics, G3696727022, G3789114225, G3874399491, G3975875632, G4212819517, G4613259628, G463062595, Integrating High Resolution Solar Physics, G5455020569, G5625221556, G5748749482, G5881647929, G5894067328, G6319620625, Queen's University Belfast Consolidated Grant in Solar Physics and Solar System Studies 2023 - 2026, G7518687652, G8524849061, G856857239, G8605206908, G8920101981
OpenAlex ID: W7222008717