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Hardi Peter (MPS), Sami Solanki (MPS)02/06/2026, 09:00Science Meeting
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02/06/2026, 09:05Science Meeting
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02/06/2026, 09:20Science Meeting
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02/06/2026, 09:35Science Meeting
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Johannes Hoelken (MPS)02/06/2026, 09:50Science Meeting
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Jose Carlos del Toro Iniesta (Instituto de Astrofísica de Andalucía (IAA-CSIC))02/06/2026, 10:05
Studies of image formation in astronomical instruments are often conducted under the assumption that light polarization has no significant influence. When diffraction effects are considered, they are typically treated using scalar point spread functions. This contribution aims to address the general problem by highlighting the potential impact of polarization and assessing it for a specific...
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Francisco Javier Bailen (IAA-CSIC)02/06/2026, 10:20Science Meeting
Solar magnetographs are often equipped with Fabry–Pérot etalons to sample spectral lines that are sensitive to the magnetic field. Typically, two etalons with different optical thicknesses and reflectivities are used to reduce unwanted light from secondary orders while improving the spectral resolution. However, using two etalons in spaceborne or balloon-borne applications is usually...
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Dr Shahin Jafarzadeh (Queen's University Belfast, UK)02/06/2026, 11:00
The seeing-free, multi-line, high-cadence observations delivered by Sunrise III provide a uniquely powerful new framework for studying waves and oscillations in the lower solar atmosphere. In this talk, I will present first results from our early-science investigations of active-region targets in the 327–329 nm near-UV window observed by SUSI, including line-dependent frequency structuring in...
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Takuma Matsumoto (Nagoya University)02/06/2026, 11:15Science Meeting
We report high-spatial-resolution spectropolarimetric observations of a solar filament and its surrounding region, obtained with the Sunrise Chromospheric Infrared spectro-Polarimeter (SCIP) onboard the SUNRISE III balloon-borne observatory on 15 July 2024.
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The target, a filament located near the disk center adjacent to an active region, was monitored for over two hours.
SCIP recorded full... -
Yusuke Kawabata (National Astronomical Observatory of Japan)02/06/2026, 11:30Science Meeting
Ellerman bombs (EBs) are transient brightenings in the wings of chromospheric lines, recognized as signatures of magnetic reconnection in the lower solar atmosphere. However, the three-dimensional (3D) magnetic topology of EBs has remained elusive due to the lack of seamless height coverage in spectropolarimetric observations.
We present initial results from SUNRISE III/SCIP observations...
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David Arroyo Caballero (IAA-CSIC)02/06/2026, 11:45Science Meeting
The weak-field approximation (WFA) is extensively used to infer solar magnetic fields due to its simplicity and low computational cost, often being applied beyond its formal range of validity. In this work, we reassess its limitations using Generalized Response Functions (GRFs), which quantify the sensitivity of WFA-derived magnetic fields to atmospheric parameters. We derive analytical...
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Masahito Kubo (National Astronomical Observatory of Japan)02/06/2026, 12:00Science Meeting
Sunrise III/SCIP acquired a unique, high-precision spectropolarimetric dataset for a quiet Sun region near the disk center on 2024 July 11 with the full field of view of 58" x 58". With an integration time of 10 s per slit position, the scan was completed in 107 minutes without interruption, achieving a polarimetric precision of 0.03-0.04% (1$\sigma$). The multi-wavelength SCIP observations,...
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Patrick Ondratschek (MPS)02/06/2026, 12:15Science Meeting
The SCIP instrument on board Sunrise III observed the solar chromosphere at high spectral and spatial resolution through the Ca II 854.2 nm line. Kubo et al. (2026) present quiet Sun observations that reveal fine-structured network magnetic fields at chromospheric heights. By using the recently developed chromospheric extension of the MURaM code in combination with radiative transfer...
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Momchil Molnar (GNOI)02/06/2026, 14:00
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Shihao Rao (MPS)02/06/2026, 14:15Science Meeting
We describe transient brightenings in a very quiet Sun region detected with SUNRISE III/SUSI spectroscopic observations covering the Ca II K at 3933.663 Angstrom. The Ca II K line is one of the strongest lines in the solar spectrum and serves as a key diagnostic of the solar atmosphere. On its wings there are plenty of absorption lines that originate from various atmospheric heights. At some...
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Ivan Milic (KIS)02/06/2026, 14:30Science Meeting
Sunrise III identified extended Ca II K emission above the limb. In a recently submitted letter, we described this emission and performed a simple radiative transfer modeling to compare emission properties with 1D and 3D models of the solar atmosphere. Here, we present more detailed modeling, including the 3D scattering in the upper chromosphere, as well as the discussion on the intensity of...
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Ana Belen Grinon-Marin (Institute for Solar Physics / Stockholm University)02/06/2026, 14:45Science Meeting
In this talk we aim at deepening our understanding of pores with particular focus on their characterization at middle atmospheric layers (upper photosphere / lower chromosphere). Pores are small and dark magnetic features observed in the photosphere that are composed of only an umbral core, i.e. they do not have penumbral structure, and have short lifetimes compared to larger sunspots. The...
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Sergio Javier González Manrique (Instituto de Astrofisica de Canarias)02/06/2026, 15:00Science Meeting
Emerging flux regions (EFRs) are highly dynamic environments where magnetic fields rise through the solar atmosphere, often giving rise to arch filament systems (AFSs) and filamentary structures. We present high-resolution, multi-line observations of an EFR obtained during the Sunrise III mission, combining spectropolarimetric measurements from TuMag and SCIP with EUV observations from SDO....
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Juan Sebastian Castellanos Duran (MPS)02/06/2026, 15:15Science Meeting
Sunrise III/SUSI conducted observations at the 409 nm spectral window, capturing an exceptional scan from near the disk up to 7 Mm above it. Ground-based acquisition of such data is hindered by foreshortening, low contrast, and variable atmospheric conditions. Over one hundred spectral transitions were detected, including Hydrogen (H$\delta$), Sr II, rare-earth elements such as La, Dy, and Hf,...
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Santiago Vargas-Domínguez (Universidad Nacional de Colombia - Observatorio Astronómico Nacional)02/06/2026, 16:00
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Andreas Lagg (MPS)02/06/2026, 16:15Science Meeting
In this presentation I summarize my early-science paper, where we report on the direct measurement of the height dependence of $p$-mode phase shifts in the lower solar atmosphere.
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The line-core positions of 19 spectral lines in a 2 nm-wide window around the Ca II H line (396.8 nm) were used to determine the vertical oscillations at their respective formation heights. We find that the phases... -
Pietro Bernasconi (JHU/APL)02/06/2026, 16:30Science Meeting
We present our first result on the reconstruction of vector magnetic fields in the emerging flux region labeled 02_EMEF from vector polarimetric data acquired by TuMag/Sunrise III on July 10, 2024 from 19:14 to 21:47 UT. The full dataset is composed of a time series of 97 sets of vector polarimetric spectral images taken across the Fe I 5250.2 A (a photospheric line) and Mg I b2 5172.7 A (a...
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Manolis Georgoulis (Johns Hopkins APL)02/06/2026, 16:45Science Meeting
Following an effort (see abstract by P. Bernasconi et al.) to infer the magnetic field components of TuMag sample 02_EMEF (emerging flux region) in the absence of a full inversion process, we present a preliminary magnetic field analysis of this dataset. We possess 97 sets of Fe I and Mg I Stokes profiles at Levels 1.0 and 1.1, with a mean cadence of 82.8 sec, taken roughly between 19:14 and...
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Dusan Vukadinovic (Institute of Physics, University of Graz)02/06/2026, 17:00Science Meeting
To fully exploit the rich SCIP observations, it is important to update the atomic data of observed lines. In this contribution, I will discuss the procedure to identify lines with poorly constrained parameters, such as the transition probability, and how these are inferred from observations, self-consistently with the physical parameters. For this purpose I use SCIP observations of an emerging...
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Daniel Ramos (GNOI)02/06/2026, 17:15Science Meeting
We present an analysis of magnetic bright points (BPs) using high-resolution images from the SUSI instrument. We built a neural network to detect automatic BPs in thousands of reconstructed SJ images, and from this, a morphological analysis is performed to characterise properties such as area, length, and proper motion velocities.
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Nitin Yadav (Indian Institute of Technology Delhi)03/06/2026, 09:00
Vortex motions in the solar atmosphere play a crucial role in energy transport and plasma heating. Current observational methods for detecting vortices rely primarily on intensity morphology, which is limited in sensitivity and often fails to capture the full vortex population. In this Letter, we propose linear polarization (LP) as a novel diagnostic for identifying vortices in...
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Suzana de Souza e Almeida Silva (University of Sheffield)03/06/2026, 09:15Science Meeting
We analyse high-resolution data from the TuMag instrument aboard the Sunrise III balloon mission. Vortices are identified using a velocity-independent approach that detects their signatures directly in intensity patterns, combining morphological identification of vortex structures with Spectral Proper Orthogonal Decomposition to extract coherent dynamical patterns imprinted by vortices in Mg...
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Christoph Kuckein (Instituto de Astrofisica de Canarias (IAC))03/06/2026, 09:30Science Meeting
We analyze spectropolarimetric observations acquired with the SCIP instrument in the near-infrared spectral window CH1 around 850 nm. This wavelength range contains a total of 12 spectral lines sampling different layers of the solar atmosphere. In this work, we focus on a subset of seven Fe and Ca lines, spanning photospheric, upper-photospheric, and chromospheric heights, including the Ca II...
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Shujun CAI (National Astronomical Observatory of Japan)03/06/2026, 09:45Science Meeting
We investigate small-scale magnetic features in the quiet solar photosphere through high-resolution multi-wavelength spectropolarimetric observations taken by the Sunrise Chromospheric Infrared spectro-Polarimeter on board the Sunrise-III stratospheric balloon-borne solar observatory. The instrument allows for high signal-to-noise observations of multiple spectral lines.
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Our analysis focuses... -
Ryohtaroh Ishikawa (National Institute for Fusion Science)03/06/2026, 10:00Science Meeting
SUNRISE III observed an M5.3-class flare on July 13th. The 3-hour observation began at 11:44 UT, one hour before the GOES X-ray flux peaked at 12:40 UT. SCIP obtained full Stokes profiles in the 770 nm and 850 nm range, covering the photospheric Fe I 849 nm, the upper photospheric K I 766 nm and 770 nm, and the chromospheric Ca II 849 nm and 854 nm lines. The FOV of SCIP covered a part of the...
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Lakshmi Pradeep Chitta (MPS)03/06/2026, 10:15Science Meeting
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Jan Jurcak (Astronomical Institute of the CAS)03/06/2026, 11:00
The solar photosphere is shaped by the interplay between convection and magnetic fields, producing a rich variety of structures in active regions. While granulation represents the fundamental convective pattern of the quiet Sun, magnetic field in active regions gives rise to distinct magneto-convective regimes, each defined by a different balance between plasma motions and magnetic forces....
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Ayumi Asai (Astronomical Observatory, Kyoto University)03/06/2026, 11:15Science Meeting
We report imaging spectroscopic observations of an M1.4 solar flare obtained during a coordinated observation between SUNRISE-III/SCIP and Domeless Solar Telescope (DST) at Hida Observatory, Kyoto University.
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The flare that occurred on 2024 July 13 in NOAA Active Region 13738 exhibited a compact flare kernel located within a sunspot umbra.
SCIP performed rapid slit-scan observations over a... -
Takayoshi Oba (Advanced Research Center for Space Science and Technology (ARC-SAT), Institute of Science and Engineering, Kanazawa University)03/06/2026, 11:30Science Meeting
Acoustic waves propagate into the chromosphere and upper atmosphere, contributing significantly to energy transport and dynamics. Their upward propagation, however, is restricted to frequencies above the acoustic cutoff frequency, which depends on atmospheric conditions. In particular, the magnetic field configuration plays a key role, as the cutoff frequency is reduced in regions where the...
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Johannes Hoelken (MPS)03/06/2026, 11:45Science Meeting
High-resolution broad-band observations of the Sun reveal a multitude of small-scale structures, everywhere in the photosphere. The increase in resolution usually comes with the cost of increased noise and decreased polarimetric signal.
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In this contribution we present an approach inspired by stellar astrophysics, in particular the study of stellar magnetism. We use least-squares deconvolution... -
Azaymi L. Siu-Tapia (Instituto de Astrofísica de Andalucía (IAA-CSIC))03/06/2026, 12:00Science Meeting
We analyze high-resolution spectropolarimetric observations from TuMag/SUNRISE III in the Fe I 5250.2 Å and Mg I b2 5173 Å lines to investigate how sunspot properties change from the photosphere to the low chromosphere, a transition layer characterized by key changes in the thermal, dynamic, and magnetic structure of the solar atmosphere.
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We perform a comparative analysis using both spectral... -
Haocheng Yu (NAOJ)03/06/2026, 12:15Science Meeting
We report the detection of high-order hydrogen Paschen emission lines (Pa~15, Pa~16, and Pa~17) in the quiet-Sun chromosphere off the solar limb using the Chromospheric Infrared SpectroPolarimeter (SCIP) on board the SUNRISE balloon telescope. These lines reveal thread-like structures resembling spicules and exhibit systematically smaller Doppler velocities than Ca II 854.2 nm, indicating that...
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ryan campbell (Queen's University Belfast)03/06/2026, 14:00Science Meeting
We present an analysis of high-resolution multi-line spectropolarimetric observations of quiet-Sun network elements obtained with the Sunrise III Chromospheric Infrared SpectroPolarimeter (SCIP). Using simultaneous photospheric Fe I and chromospheric Ca II diagnostics, we examine the magnetic structure of a network element across optical depth. We find a coherent transverse magnetic structure...
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Carlos Quintero Noda (Institute of Astrophysics of the Canary Islands / La Laguna University)03/06/2026, 14:15Science Meeting
Deciphering the physical properties of flares is crucial for understanding the nature of one of the most energetic events on the Sun. We make use of high spatial and spectral resolution observations of a flare-producing active region, focusing on a complex light bridge, to analyse the physical properties of a C-class flare. The observations show Stokes profiles with different line Doppler...
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Edvarda Harnes (MPS)03/06/2026, 14:30Science Meeting
The Sunrise Ultraviolet Spectropolarimeter and Imager (SUSI) instrument captured high spectral and spatial resolution observations of the strong Fe I line at 407.17 nm. We observe that within a sunspot penumbra, this line displays multi-lobed Stokes V profiles unlike other lines in the same spectrum. These multi-lobed profiles were predicted in earlier computations and are found to result from...
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Iñigo Juanikorena Berasategi (GNOI)03/06/2026, 14:45Science Meeting
We investigate the height dependence of the line-of-sight (LOS) magnetic field in an active-region (AR) plage from the upper photosphere to the upper chromosphere using co-spatial ultraviolet (UV) and infrared (IR) spectropolarimetric observations. We analyze the Stokes I and V profiles acquired during the Sunrise III stratospheric balloon flight with the SUSI and SCIP instruments. The Ca II K...
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Yoshihiro Naito (NAOJ/SOKENDAI)03/06/2026, 15:00Science Meeting
Understanding the magnetic field structure of spicules is essential for developing formation models of spicules, which are important for understanding mass transport to the corona and the coronal heating.
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We report the spatial distribution of spicule magnetic fields along the line-of-sight ($B_{\rm{LOS}}$) from spectropolarimetric observations of the solar limb with SUNRISE-III/SCIP under... -
Kunal Hardeep Singh (MPS)03/06/2026, 15:15Science Meeting
Small-scale impulsive energy events, often attributed to magnetic reconnection, are prime candidates for heating the solar corona to millions of degrees. However, the direct detection of the effect of such events in the corona remains challenging due to fast energy dissipation in the corona. These events, though faint in the corona, can drive significant chromospheric dynamics, leaving...
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Florian Kröll (GNOI)03/06/2026, 16:00Science Meeting
Faculae are a major source of spectral and radial velocity (RV) variability in the Sun and in Sun-like stars, yet their disk-integrated spectroscopic imprint remains insufficiently constrained. We investigate how faculae modify spectral line morphology and line-of-sight velocity signatures from disk centre to the limb using a physically consistent forward model based on 3D radiative...
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Dr Sowmya Krishnamurthy (University of Graz)03/06/2026, 16:15Science Meeting
Convective velocity fields in the solar photosphere are strongly modified by magnetic structures such as faculae, leading to measurable changes in spectral line shapes and shifts. These effects become increasingly complex away from the disk center. Accurately capturing this center-to-limb variation is essential for interpreting spatially resolved solar observations and for modeling unresolved...
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Vigeesh Gangadharan (Institut für Sonnenphysik (KIS))03/06/2026, 16:30Science Meeting
Plasma flows in the near-surface region are thought to play an important role in replenishing the quiet Sun magnetic field. The interaction of magnetic fields with the complex flow structure causes these fields to reorganize at sub-granular scales. Horizontally aligned vortex flows near the edge of solar granules can grab magnetic fields from the interior and bring them to the visible surface....
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Sandeep Dubey (Udaipur Solar Observatory, PRL, India)03/06/2026, 16:45Science Meeting
The solar chromosphere is one of the most intriguing yet poorly understood regions of the solar atmosphere, and its heating remains a central problem in solar physics. Plage regions, characterized by the strong, predominantly vertical magnetic fields, show enhanced chromospheric emission, indicating localized energy deposition. The dominant
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mechanisms that heat the chromosphere include waves,... -
Sami Solanki (MPS)03/06/2026, 17:00Science Meeting
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