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Sunrise III: Overview of Observatory and Instruments

T0 review · 2 major / 4 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read Sunrise III's 2024 flight shows a balloon-borne 1-meter telescope can hold a stable, diffraction-limited image while three full-Stokes instruments observe the Sun from 309 to 855 nm.

desk verdict A solid observatory overview: the hardware and flight claims are well supported, and the polarimetric calibration caveat is real but honestly deferred. read the letter →

arxiv 2502.06483 v2 pith:VJBLMYDW submitted 2025-02-10 astro-ph.IM astro-ph.SR

Andreas Korpi-Lagg , Achim Gandorfer , Sami K. Solanki , Jose Carlos del Toro Iniesta , Yukio Katsukawa , Pietro Bernasconi , Thomas Berkefeld , Alex Feller
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Tino L. Riethmüller Alberto Álvarez-Herrero Masahito Kubo Valentín Martínez Pillet H. N. Smitha David Orozco Suárez Bianca Grauf Michael Carpenter Alexander Bell María-Teresa Álvarez-Alonso Daniel Álvarez García Beatriz Aparicio del Moral Daniel Ayoub Francisco Javier Bailén Eduardo Bailón Martínez Maria Balaguer Jiménez Peter Barthol Montserrat Bayon Laguna Luis R. Bellot Rubio Melani Bergmann Julian Blanco Rodríguez Jan Bochmann Juan Manuel Borrero Antonio Campos-Jara Juan Sebastián Castellanos Durán María Cebollero Aitor Conde Rodríguez Werner Deutsch Harry Eaton Ana Belen Fernández-Medina German Fernandez-Rico Agustin Ferreres Andrés García Ramón María García Alarcia Pilar García Parejo Daniel Garranzo-García José Luis Gasent Blesa Karin Gerber Dietmar Germerott David Gilabert Palmer Laurent Gizon Miguel Angel Gómez Sánchez-Tirado David Gonzalez Alejandro Gonzalo Melchor Sam Goodyear Hirohisa Hara Edvarda Harnes Klaus Heerlein Frank Heidecke Jan Heinrichs David Hernández Expósito Johann Hirzberger Johannes Hoelken Sangwon Hyun Francisco A. Iglesias Ryohtaroh T. Ishikawa Minwoo Jeon Yusuke Kawabata Martin Kolleck Hugo Laguna Julian Lomas Antonio C. López Jiménez Paula Manzano Takuma Matsumoto David Mayo Turrado Thimo Meierdierks Stefan Meining Markus Monecke José Miguel Morales-Fernández Antonio Jesús Moreno Mantas Alejandro Moreno Vacas Marc Ferenc Müller Reinhard Müller Yoshihiro Naito Eiji Nakai Armonía Núñez Peral Takayoshi Oba Geoffrey Palo Isabel Pérez-Grande Javier Piqueras Carreño Tobias Preis Damien Przybylski Carlos Quintero Noda Sandeep Ramanath Jose Luis Ramos Más Nour Raouafi María-Jesús Rivas-Martínez Pedro Rodríguez Martínez Manuel Rodríguez Valido Basilio Ruiz Cobo Antonio Sánchez Rodríguez Antonio Sánchez Gómez Esteban Sanchis Kilders Kamal Sant Pablo Santamarina Guerrero Erich Schulze Toshifumi Shimizu Manuel Silva-López Azaymi L. Siu-Tapia Thomas Sonner Jan Staub Hanna Strecker Angel Tobaruela Ignacio Torralbo Alexandra Tritschler Toshihiro Tsuzuki Fumihiro Uraguchi Reiner Volkmer Angelos Vourlidas Dušan Vukadinović Stephan Werner Andreas Zerr
This is my paper · ORCID
classification astro-ph.IMastro-ph.SR
keywords SunriseIIIstratosphericballoonobservatorysolarspectropolarimetrynear-ultravioletspectrumchromosphericmagneticfieldsfullStokespolarimetryhighangularresolutionimagestabilization
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Sunrise III is a balloon-borne observatory built around a 1-meter Gregory telescope and three new instruments that measure the full polarization state of sunlight across 309–855 nm. The paper's central claim is that the system worked as designed: during a 6.5-day stratospheric flight in July 2024 it executed every high-priority predefined observing program, held images stable to better than 0.005 arcseconds rms, and recorded more than 200 TB. The payoff, if the data reduce to the stated polarimetric sensitivity of better than $10^{-3}$ of the continuum, is a seeing-free multi-wavelength view of solar magnetism that reaches from the photosphere into the chromosphere, including the near-UV window that ground-based telescopes cannot access cleanly. This would directly address long-standing questions about how small-scale magnetic fields, waves, and flows heat the upper solar atmosphere.

What carries the argument

The load-bearing architecture is ISLiD, the Image Stabilization and Light Distribution unit: a 1:1 Offner relay made of two concentric spherical mirrors with radii in a 2:1 ratio, a configuration that is intrinsically free of spherical aberration, astigmatism, and coma. The relay sits at the telescope focus, splits the beam among SUSI, TuMag, SCIP, and the CWS with anti-parallel beam-splitter pairs that cancel astigmatism and chromatic shift, and carries a fast tip/tilt mirror on its secondary. The Correlating Wavefront Sensor (CWS) closes the loop: a 7 kHz correlation tracker drives the tip/tilt mirror for milli-arcsecond image motion correction, while a six-subaperture Shack-Hartmann sensor controls focus and coma through the secondary mirror. The new three-axis gondola provides the coarse pointing, with a roll reaction wheel damping pendulum motion above 0.5 Hz. Together they are what turns a 1-meter balloon telescope into a multi-hour, diffraction-limited polarimetric platform.

What would settle it

Using SUSI's recorded spectra of the magnetically insensitive Fe I 406.538 nm line, one can search for residual Stokes Q, U, or V signals above $10^{-3}$ of the continuum that correlate with telescope elevation, time, or target position; if such signals survive the calibration, the ground-plus-solar correction has not captured the main mirror's contribution and the field vectors are biased.

Watch

Extended reading notes

Core claim

The paper presents Sunrise III not as a single instrument but as an integrated observatory: one telescope, three complementary full-Stokes spectropolarimeters, and a stabilization chain that delivers space-like observing conditions from a balloon. Its claim is that the 2024 flight demonstrated this architecture. SUSI covered 309–417 nm, a spectral region with a much higher density of lines than the visible and more than 150 lines formed above 600 km; TuMag mapped $46\times46$ Mm$^2$ fields of view in the visible Fe I 525 nm and Mg I 517 nm lines; and SCIP observed the Ca II infrared triplet and K lines at 765–855 nm, where telluric blends are weak or absent. With the three instruments aligned to about 0.1 arcseconds and scanning together for hours, the dataset couples photospheric and chromospheric diagnostics in time and space. The authors report that all high-priority predefined programs were executed, that the correlation tracker held a four-hour-plus record lock, and that the flight accumulated more than 200 TB of raw data for public release after reduction.

Load-bearing premise

All three instruments' polarimetric claims rest on the assumption that the telescope's polarization response is fully known: for SUSI and SCIP the ground calibration was done without the main mirror M1, and the residual crosstalk is corrected only through in-flight solar signals of known polarization, so if M1's contribution is not captured the magnetic field vectors would be biased.

Editorial extensions

If this is right

  • The SUSI near-UV data set gives solar physics its first high-resolution full-Stokes look at 309–417 nm, where more than 150 lines form in the chromosphere and many-line Hanle and Zeeman diagnostics can be combined.
  • Co-aligned SUSI and SCIP slit scans inside TuMag's full field of view produce simultaneous photosphere-to-chromosphere stratifications of the magnetic field vector for the same small-scale features.
  • Hour-long, and in one record case longer than four hours, continuous lock times support studies of magnetic flux emergence, cancellation, and local helioseismology at constant spatial resolution.
  • If the $10^{-3}$ polarimetric sensitivity is confirmed in reduction, the publicly released dataset becomes a benchmark for quiet-Sun and chromospheric magnetism that ground-based observatories can compare against.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A corollary the paper does not spell out: if the near-UV many-line polarimetry reaches its stated accuracy, it is a much stronger Hanle-effect probe of weak turbulent fields than Zeeman-only measurements, so the data could help settle whether a small-scale dynamo maintains quiet-Sun magnetism.
  • The ISLiD/Offner-relay plus correlation-tracker design is a portable pattern; the same 1:1 relay with an integrated fast steering mirror could give diffraction-limited polarimetry on future balloon or small-satellite solar telescopes without adaptive optics.
  • A direct test of the telescope-polarization correction strategy would be to invert vector magnetic fields from overlapping photospheric lines in SUSI and SCIP data on the same target; if the recovered fields disagree beyond the stated uncertainties, the M1 correction would need revision.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 4 minor

Summary. This paper is a system-level overview of the Sunrise III balloon-borne solar observatory and its 2024 flight. It describes the 1-m Gregory telescope, the new APL gondola and pointing control system, the ISLiD light-distribution unit with the CWS image stabilization and autofocus, the three new full-Stokes instruments (SUSI, SCIP, TuMag), the electronics, communications, thermal design, testing campaign, flight operations, and data policy. The paper reports a successful 6.5-day flight in July 2024 with over 200 TB of data, and it presents two headline performance claims: a polarimetric sensitivity better than 10^-3 of the continuum for all three instruments and an image stability better than 0.005 arcsec rms. The authors repeatedly state that detailed post-flight performance assessment is deferred until the data-reduction phase is complete.

Significance. If the stated performance is confirmed, Sunrise III will provide a unique dataset: simultaneous full-Stokes spectropolarimetry from the near-UV (309 nm) to the near-IR (855 nm) at high spatial resolution and with multi-hour stability, including the first high-resolution spectropolarimetric coverage of the poorly explored 309-417 nm range. The paper is valuable as the mission-level reference for this observatory and for its calibration and operations philosophy. Its strengths are the breadth of ground testing (mechanism tests, optical tests, thermal-vacuum tests, hang tests), the detailed reporting of flight anomalies (power interruptions, pointing loss, RAMON battery failure, the 2022 launch failure), and the clearly stated open-data concept. The main weakness is that some of the headline performance numbers in the Abstract, Table 3, and Summary are worded as achieved results, while the evidence presented in the body is preliminary or based on ground calibrations that exclude a key optical element; this gap should be closed by explicit qualification in the final version.

major comments (2)
  1. [Section 5.3] The polarimetric sensitivity claim of better than 10^-3 of the continuum for SUSI and SCIP is presented as achieved ('SCIP reaches a polarimetric sensitivity of 3e-4', Table 3 row 'Pol. sensitivity', and Section 7 'reach a polarimetric sensitivity of better than 10^-3'), but the end-to-end calibration path described in Section 5.3 excludes the main mirror M1, states that 'no independent telescope calibration is foreseen', and relies on in-flight solar signals of 'known polarization properties' to correct residual crosstalk. The chosen zero-polarization targets (spectral continuum, average quiet Sun, Fe I 406.538 nm) are not guaranteed to be zero at the 10^-3 level, especially near the limb or in the presence of scattering polarization, and the time/elevation dependence of M1's Mueller matrix is not constrained by the F1/F2 calibrations. Since the full-Stokes capability at 10^-3 is the core scientific specification of SUSI and SCIP, I recommend that the paper explicitly label this number as a pre-flight requirement or ground-calibration result pending end-to-end validation, or provide an error-budget estimate that includes M1.
  2. [Section 6.1] The pointing-stability reporting is internally inconsistent and should be clarified. Table 1 lists the gondola pointing specification as '<3 arcsec rms', but Section 6.1 states that the measured rms pointing stability was 'on average better than 3 arcsec, exceeding the specifications by a factor of 5'; a value of 3 arcsec does not exceed a 3-arcsec specification by a factor of 5. In addition, the Abstract presents 'an image stability with a root-mean-square value smaller than 0.005 arcsec' as an accomplished fact, whereas Section 6.1 reports only a preliminary assessment with 'milli-arcsecond rms accuracy' and no quantitative number for the 0.005 arcsec value. Please distinguish clearly between specified, ground-tested, and in-flight-verified values, and either report the measured CWS residual or mark 0.005 arcsec as a requirement with preliminary confirmation.
minor comments (4)
  1. [Section 4.3.2] The text '0db correction bandwidth' should read '0 dB correction bandwidth' for consistency with standard notation.
  2. [Section 4.1.1] The value '190◦s–2' should be typeset as 190 deg s^-2 or 190° s^-2 with proper unit formatting.
  3. [Section 2.2.1] The phrase 'Sunrise iii had an unsuccessful flight on 10 July 2022' is slightly misleading; the 2022 event was an unsuccessful launch attempt of the same observatory. Consider rephrasing to 'an unsuccessful launch attempt' for clarity.
  4. [Section 6.2] In the sentence 'Simultaneous spectra over long time periods in the near-IR and near-UV with sub-arcsecond alignment accuracy (0.1") over hours become possible', the verb should be singular: 'becomes possible'.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: the Sunrise III overview makes descriptive hardware and performance claims supported by direct ground tests, flight telemetry, and companion instrument papers; the polarimetric-calibration caveat is an unvalidated assumption, not a self-referential derivation.

full rationale

The paper is an instrument-overview and mission-report, not a derivation with fitted parameters. No performance number is obtained by defining its own input. The headline claims (CWS image stability <0.005 arcsec rms, >200 TB recorded, successful execution of predefined observing programs, 6.5-day flight) are supported by direct ground tests, in-flight telemetry, and flight operations logs quoted in the text. The polarimetric sensitivity of <10^-3 is presented as a design requirement and is backed by laboratory calibration measurements (e.g., SCIP 3x10^-4 after 10 s, cited to Kawabata et al. 2022, and SUSI standalone tests, cited to Iglesias et al. 2025). These are companion-authored calibrations but they are externally falsifiable laboratory measurements, not circular self-support. The paper explicitly notes that SUSI/SCIP F1/F2 calibrations exclude the main mirror M1 and that no independent telescope calibration is foreseen, relying instead on in-flight solar signals of assumed known polarization. This is a real validation risk for the polarimetric accuracy claim, but it is not circularity: the solar-signal correction is a planned calibration procedure, not a derivation of the claimed sensitivity from the claimed sensitivity, and the paper itself defers full performance assessment to the data-reduction phase (Section 6.3). Self-citations to companion instrument papers are for detailed component descriptions and do not carry the load of any inference made here. No equation equates an input to an output, no fitted parameter is renamed as a prediction, and no uniqueness theorem is imported from the authors' prior work. The paper is therefore self-contained against external benchmarks and its descriptive claims are independently evidenced.

Assumptions & free parameters 0 free parameters · 3 assumptions · 0 invented entities

No numeric fits or new physical entities appear; the central content is descriptive engineering. The listed axioms are background assumptions used for motivation and design rationale, not fitted quantities.

assumptions (3)
  • domain assumption The RH/FALC-based formation heights of roughly 60,000 spectral lines in the SUSI range (Figure 5) correctly indicate the atmospheric layers each line probes.
    Invoked in Section 3.1.6 to argue for the scientific potential of the near-UV; it supports mission motivation rather than the hardware claims.
  • standard math The Offner relay used in ISLiD is free of spherical aberration, astigmatism, and coma by design.
    Section 4.3.1 relies on this standard optical property to justify the light-distribution design; it is not independently verified in this paper.
  • domain assumption Flight sensor telemetry (pointing, temperatures, power, data rates) accurately represents the observatory state.
    Sections 4.5.5 and 6.1 use housekeeping values to support performance statements; calibration of those sensors is not shown in this overview.

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Cite this review

Pith. "Pith review of Sunrise III: Overview of Observatory and Instruments." pith.science (2026). https://pith.science/paper/VJBLMYDW

@misc{pith2026250206483,
  author       = {Pith},
  title        = {Pith review of: Sunrise III: Overview of Observatory and Instruments},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VJBLMYDW}},
  note         = {Machine review of arXiv:2502.06483}
}
abstract

In July 2024, Sunrise completed its third successful science flight. The Sunrise III observatory had been upgraded significantly after the two previous successful flights in 2009 and 2013. Three completely new instruments focus on the small-scale physical processes and their complex interaction from the deepest observable layers in the photosphere up to chromospheric heights. Previously poorly explored spectral regions and lines are exploited to paint a three-dimensional picture of the solar atmosphere with unprecedented completeness and level of detail. The full polarimetric information is captured by all three instruments to reveal the interaction between the magnetic fields and the hydrodynamic processes. Two slit-based spectropolarimeters, the Sunrise UV Spectropolarimeter and Imager (SUSI) and the Sunrise Chromospheric Infrared spectro-Polarimeter (SCIP), focus on the near-ultraviolet and the near-infrared regions respectively, and the imaging spectropolarimeter Tunable Magnetograph (TuMag) simultaneously obtains maps of the full field-of-view of $46 \times 46$ Mm$^2$ in the photosphere and the chromosphere in the visible. The instruments are operated in an orchestrated mode, benefiting from a new Image Stabilization and Light Distribution unit (ISLiD), with the Correlating Wavefront Sensor (CWS) providing the autofocus control and an image stability with a root-mean-square value smaller than 0.005''. A new gondola was constructed to significantly improve the telescope pointing stability, required to achieve uninterrupted observations over many hours. Sunrise III was launched successfully on July 10, 2024, from the Esrange Space Center near Kiruna (Sweden). It reached the landing site between the Mackenzie River and the Great Bear Lake in Canada after a flight duration of 6.5 days. In this paper, we give an overview of the Sunrise III observatory and its instruments.

Figures

Figures reproduced from arXiv: 2502.06483 by the authors.

Figure 1
Figure 1. Sunrise iii a few minutes before the launch on 10 July 2024 on the balloon pad of Esrange space center. The balloon is already fully inflated, the red and white parachute is attached to the flight train, that stretches over the launch vehicle to the observatory. Image courtesy: SSC / Mattias Forsberg. (see [PITH_FULL_IMAGE:figures/full_fig_p009_1.png] view at source ↗
Figure 2
Figure 2. Top: Trajectories of the three successful Sunrise flights: Sunrise i (green), Sunrise ii (blue), and Sunrise iii (orange). Bottom: Sun elevation angle (blue) and flight altitude obtained from the gondola GPS receiver (orange) for Sunrise iii. Background map: Google Earth (data attribution: Google Landsat / Copernicus Data SIO, NOAA, U.S. Navy, GEBCO IBCAO U.S. Geological Survey INEGI). solar features down to a size … view at source ↗
Figure 3
Figure 3. Vertical cut showing the temperature stratification in a MURaM-ChE simulation. The heights for optical depth unity for the continuum at 500 nm and for selected spectral lines observed by the Sunrise iii instruments are indicated by the colored solid lines. der Voort, Rutten, and Vissers 2016; Kawabata et al. 2024). Finally, magnetic vortex flows with twisted magnetic fields, so-called solar tornadoes, have been iden… view at source ↗
Figures from the paper (23 more)
Figure 4
Figure 4. Figure 4: Simulated SCIP observation in the Ca ii 849.8 nm line showing the temporal evolution of a chro￾mospheric jet (adopted from Matsumoto et al. 2023, [PITH_FULL_IMAGE:figures/full_fig_p016_4.png]
Figure 5
Figure 5. Figure 5: Formation height of ≈ 60,000 spectral lines in the SUSI spectral range from 309 to 417 nm. The highest forming lines (above 600 km) of a few selected species are indicated by colored symbols. The shaded regions indicate the six most requested SUSI spectral windows, wit…
Figure 6
Figure 6. Figure 6: Timeline ‘SP_2’ defining the operation of the three science instruments, the ICS, the PCS, and the CWS to study the fine structure of a penumbral filament. (mode ‘SP3’) is followed by a 3-hour long observation (‘SP8’) with the spectrograph slits placed along a penumbra…
Figure 7
Figure 7. Figure 7: Image rotation speed (left panel), telescope elevation angle (middle) and slit orientation angle with respect to the solar North-South direction (right) for the first 48 hours of the 2024 flight as produced by SPPT (see Section 3.3). The horizontal bars at the bottom i…
Figure 8
Figure 8. Figure 8: Snapshot from the SPPT observation planning page. The most recent solar images (here SDO/HMI) are used to define the pointing of Sunrise. The tool presents the FoVs of the individual instruments (green TuMag, red SCIP, blue SUSI, black CWS, right panel), taking into ac…
Figure 9
Figure 9. Figure 9: Design drawing of the Sunrise iii observatory. The telescope is located in the middle of the gondola and is oriented horizontally in the plotted configuration. The gray-purple box on top of the telescope is the Post Focus Instrumentation (PFI) platform housing the scie…
Figure 10
Figure 10. Figure 10: Schematic illustrating the four major building blocks of the Sunrise iii instruments and infrastructures. The coloring indicates the responsible institute or team. design of the Sunrise iii observatory is shown in [PITH_FULL_IMAGE:figures/full_fig_p023_10.png]
Figure 11
Figure 11. Figure 11 [PITH_FULL_IMAGE:figures/full_fig_p025_11.png]
Figure 12
Figure 12. Figure 12: Sunrise iii telescope during alignment in the ISO-8 cleanroom at MPS. The 1-m primary mirror is on the left and can be recognized by the brownish honeycomb structure, the central frame houses the aperture door (open in this image) and the spider to the right holds the…
Figure 13
Figure 13. Figure 13: CAD model of the Sunrise iii PFI (left) and the flight-version of the PFI under the clean tent in the MPS clean room (right). and provides a stable platform for both, the scientific instruments, the image stabilizer and the light distribution optics. It also contains …
Figure 14
Figure 14. Figure 14: The ISLiD system during assembly, before the left-hand side stiffening wall is mounted. The optical paths within the ISLiD system including the SCIP scan unit are illustrated by thin colored lines (white means panchromatic, green symbolises the wavelength band sent to…
Figure 15
Figure 15. Figure 15: Central part of the ISLiD system, showing the Offner-M2 (tip/tilt) mirror on its piezo stage, and the beam splitter arrangement. White arrows mark the panchromatic beam from the telescope. The colored arrows indicate the wavelength bands sent towards the exit foci. Bl…
Figure 16
Figure 16. Figure 16: SCIP scan unit during assembly. The red arrows symbolize the light path from ISLiD towards the SCIP interface focus. The Offner relay uses the SMM as its secondary mirror. A set of three folding mirrors (only two are visible here) acts as path length compensator and i…
Figure 17
Figure 17. Figure 17: Optics Unit of the CWS. The light enters the CWS at the entrance focus on the right. z-direction (see [PITH_FULL_IMAGE:figures/full_fig_p033_17.png]
Figure 18
Figure 18. Figure 18: Layout of SUSI. Panel (a), top: basic optical layout; the components of the main functional units are labeled in different colors: scan unit (sky blue), spectrograph (black), polarization modulator (red) and slit-jaw unit (green); underlined labels denote a moving com…
Figure 19
Figure 19. Figure 19: Opto-mechanical design of the TuMag instrument (left), and flight instrument before closing the housing, including the electronic unit in its white housing (right). (Solar Physics Group Cameras, SPGCams, Orozco Suárez et al. 2023), a composite￾material optical bench (…
Figure 20
Figure 20. Figure 20: Opto-mechanical layout of SCIP (left) and pre-flight laboratory setup (right) showing opto-me￾chanical elements mounted on an optical bench made of a carbon fiber-reinforced polymers (CFRP) sandwich panel with low thermal expansion. width and the spatial pixel samplin…
Figure 21
Figure 21. Figure 21: ICS shortly before the final closing in October 2021. The mainboard of the ICU is at the bottom of the housing, left and right are the two DSS stacks containing the SSD disks. Identified hot spots on the electronic boards are connected via heat pipes to copper blocks.…
Figure 22
Figure 22. Figure 22: Sunrise iii network setup illustrating the data connections within the Sunrise iii observatory and to the TM/TC links to the ground stations. Colored boxes indicate the scientific instruments, gray boxes the central units provided by MPS and APL, and white boxes show …
Figure 23
Figure 23. Figure 23: Sunrise iii shortly before the launch on 10 July 2024, hanging on the launch vehicle Hercules. The locations of the piggy back payloads IRIS-2 and RAMON are marked with the yellow and the red circles, respectively. Image courtesy: SSC / Mattias Forsberg. to the target…
Figure 24
Figure 24. Figure 24: IRIS-2 images recorded during the 2024 flight. IRIS-2 is attached to the top of the gondola’s left roll-cage (see yellow circle in [PITH_FULL_IMAGE:figures/full_fig_p047_24.png]
Figure 25
Figure 25. Figure 25: E-rack –x temperature measurements during the 2022 flight of Sunrise iii (solid and dashed black lines) compared to operational (red and blue) and non-operational (green and yellow) case analyses. the PFI to act as a wind shield to avoid freezing of the instruments du…
Figure 26
Figure 26. Figure 26: Sunrise iii ground segment, data flow and communication concept for the 2024 flight. had to present, amongst others, a science status review, a deployment and integration schedule, requirements for integration and operation, and to prove that the current status of the…

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  1. The magnetic sensitivity of the Ca II resonance and subordinate lines in the solar atmosphere

    astro-ph.SR 2025-10 accept novelty 6.0 of 10

    The Ca II H and K lines respond to magnetic fields from sub-gauss to tens of gauss, the infrared triplet mainly to milligauss fields, and the weak-field approximation overestimates the line-of-sight field in the outer...

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