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arxiv: 2604.13166 · v1 · submitted 2026-04-14 · 🌌 astro-ph.SR · astro-ph.EP· astro-ph.IM

Solar photospheric spectrum microvariability III. Radial velocities and line profiles in magnetic active-region granulation

Dainis Dravins , Hans-G\"unter Ludwig , Matthias Steffen , Carlos Allende Prieto , Lars Koesterke This is my paper

Pith reviewed 2026-05-10 13:49 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EPastro-ph.IM
keywords solar granulationmagnetic fieldsconvective redshiftsspectral line profilesradial velocityactive regions3D simulationsexoplanet detection
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The pith

Magnetic granulation in solar active regions produces net convective redshifts in spectral lines.

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

The paper uses 3D hydrodynamic simulations to compare spectral line formation in quiet solar granulation versus strongly magnetized active-region granulation. It shows that magnetic fields suppress normal convective blueshifts and instead generate redshifts through localized hot, bright downflows created by shocks and compression. A reader would care because these activity-induced velocity shifts in the stellar spectrum are far larger than the signals from orbiting low-mass planets, so accurate modeling is required to separate the two.

Core claim

In simulations with 240 mT magnetic fields, convective motions are inhibited and energy transport is reduced, producing more symmetric line profiles that lack the usual blueshift and C-shaped bisectors. Unexpected net redshifts appear instead, traced to small areas where rising gas is forced into magnetically channeled downflows, generating shocks and adiabatically compressed hot bright elements whose light dominates the integrated profile.

What carries the argument

Three-dimensional radiative-hydrodynamic simulations of granulation in a 240 mT magnetic field, used to compute synthetic spectra at R approximately 900,000 and isolate the velocity contributions from individual flow structures.

If this is right

  • Line profiles in magnetic areas become more symmetric and lose their characteristic convective blueshift.
  • Different visual and near-infrared lines exhibit distinct responses, potentially allowing activity signals to be disentangled from planetary radial-velocity shifts.
  • Full-disk solar spectrum models must incorporate magnetic active-region contributions to reach the precision needed for exoEarth detections.
  • Hyper-high spectral resolution is suggested as ultimately necessary to exploit detailed line-shape information.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same shock-driven downflow mechanism could operate in other magnetically active stars and affect radial-velocity planet searches around them.
  • Time-series observations at very high resolution could isolate the predicted small-area redshift contributions in the Sun.
  • The results imply that magnetic channeling of convective flows is a dominant control on net velocity shifts whenever field strengths reach several hundred millitesla.

Load-bearing premise

The chosen 240 mT field strength and simulation resolution accurately capture the small-scale shocks and downflow contributions that occur in real solar active regions.

What would settle it

High-resolution disk-resolved spectra of solar active regions that either confirm or rule out a net redshift relative to quiet-Sun regions at the wavelengths and line depths predicted by the models.

Figures

Figures reproduced from arXiv: 2604.13166 by Carlos Allende Prieto, Dainis Dravins, Hans-G\"unter Ludwig, Lars Koesterke, Matthias Steffen.

Figure 1
Figure 1. Figure 1: Example of synthetic spectra at the solar disk center, [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Synthetic spectra in the Ca ii H & K line region: non￾magnetic (top) and 240 mT (2400 G) magnetic models. (How￾ever, the bottoms of these very strong lines are not precisely re￾produced by present modeling.) From this particular region, Fe i 393.2627 and Fe i 396.7421 nm lines, superposed onto the ex￾tended and sloping absorption wings of the K and H lines, were selected for examination ( [PITH_FULL_IMAGE… view at source ↗
Figure 4
Figure 4. Figure 4: Line profiles and bisectors for differently strong Fe ii lines. The left￾most column shows observed data from the Jungfraujoch solar disk-center atlas (top) and the integrated solar flux atlases of Kitt Peak and Göttingen (bottom). Profiles from the non-magnetic (center) and magnetic 240 mT = 2400 G simula￾tions (right) are shown for disk center µ = 1 (upper row) and for integrated sun￾light of a non-rotat… view at source ↗
Figure 5
Figure 5. Figure 5: Weak lines at solar disk center, µ = 1. Left: line profiles and bisectors from the Jungfraujoch atlas. Numerous lines of comparable strength show similar behavior in both the non-magnetic case (center) and in the 240 mT = 2400 G magnetic simu￾lation (right). Wavelengths in observational atlases are affected by the solar gravita￾tional redshift of 635 m s−1 and possible er￾rors in laboratory wavelengths [P… view at source ↗
Figure 6
Figure 6. Figure 6: Very strong lines at solar disk center. Left: Mg i b2 and Na i D2 lines in the Jungfraujoch atlas. Center: synthetic profiles and bisectors for their line cores (corresponding to the boxes at left), and also the related Mg i b1 and Na i D1 ones, for the non-magnetic simulation. Right: the 240 mT = 2400 G magnetic case. Ef￾fects of solar rotation and gravitational redshift are not included [PITH_FULL_IMAGE… view at source ↗
Figure 7
Figure 7. Figure 7: Lines in special positions dis￾play special behavior. The weak Fe i 393.2627 and Fe i 396.7421 lines are su￾perposed onto the extended absorption wings of the Ca ii H&K lines and get their formation heights lifted through combining their opacities with those of the H&K line wings. The leftmost col￾umn shows their appearance in solar spectrum atlases (Kitt Peak full-disk, Jungfraujoch disk center). With ver… view at source ↗
Figure 8
Figure 8. Figure 8: Radial-velocity shifts for ordinary lines (Table 1). Gray [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Brightness, gas velocities, and radial velocities in one temporal snapshot of the magnetic 3D simulation for 240 mT [PITH_FULL_IMAGE:figures/full_fig_p009_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Spatially resolved line profiles across the simulation area at solar disk center illustrate how the convective blueshift in the [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
read the original abstract

Finding low-mass planets around solar-type stars requires to understand the physical variability of the host star, which greatly exceeds the planet-induced radial-velocity modulation. Different solar photospheric absorption lines have slightly disparate responses to stellar activity, which should permit to disentangle wavelength shifts induced by exoplanets from those originating in stellar atmospheres. Changing area coverage of magnetic active-region granulation (faculae and plage) causes radial-velocity fluctuations of the disk-integrated solar spectrum, whose precise modeling requires active-region spectral line profiles. Hydrodynamic 3D modeling of granulation in magnetic fields extends previous non-magnetic studies, revealing different line profiles and altered convective velocity shifts. Different types of lines in the visual and near infrared are examined in synthetic hyper-high resolution spectra (R~900,000), comparing non-magnetic areas with those with strongly magnetic (240 mT = 2400 G) granulation. Magnetic fields inhibit convective motions, decrease the energy flow, produce more symmetric lines, and remove the common blueshift with its familiar C-shape bisectors. Unexpectedly, magnetic granulation displays convective redshifts. Their origin is traced to contributions from small areas, where hot and bright down-moving elements are created through shocks and adiabatic compression when rising gas is forced over into magnetically channeled downflows. Understanding line formation in also stellar active regions is needed to simulate full-disk spectra toward exoEarth detections. Detailed shapes of spectral lines carry significant information, suggesting that hyper-high spectral resolution may ultimately be required

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript employs 3D radiative MHD simulations of solar granulation to compare non-magnetic regions with strongly magnetized (240 mT) active-region areas. Synthetic spectra at R~900,000 are computed for visual and near-IR lines, showing that magnetic fields suppress convection, produce more symmetric profiles without the usual C-shaped bisectors, eliminate the convective blueshift, and instead yield net convective redshifts. These redshifts are traced to localized hot, bright downflows formed by shocks and adiabatic compression when rising gas is diverted into magnetically channeled flows. The work aims to improve modeling of stellar activity noise for exoplanet radial-velocity searches.

Significance. If the central mechanism holds, the paper supplies a physically grounded explanation for altered line shifts in magnetic regions, directly relevant to mitigating activity-induced RV jitter at the cm/s level needed for exo-Earth detection. The forward-modeling approach with hyper-high resolution spectra and the identification of the small-area shock contribution constitute a clear advance over prior non-magnetic granulation studies, offering falsifiable predictions for high-resolution observations of solar faculae.

major comments (2)
  1. [Methods] Methods section (simulation parameters): The horizontal grid spacing and vertical resolution of the 3D MHD runs are not stated explicitly, and no resolution-convergence tests are shown for the thin shock fronts and associated temperature-velocity correlations that are invoked to explain the redshift. If these structures are numerically broadened, the area-weighted contribution to the disk-integrated profiles (and thus the claimed sign reversal) could be resolution-dependent.
  2. [Results] Results (redshift origin and line-profile synthesis): The abstract and results assert that the redshifts arise from small areas of hot downflows, yet no quantitative error budget, sensitivity test to the fixed 240 mT field strength, or direct comparison against observed solar active-region spectra or RV time series is provided. Without such validation, it remains unclear whether the simulated net redshift amplitude matches real solar data.
minor comments (2)
  1. [Abstract] Abstract: the phrasing 'Understanding line formation in also stellar active regions' is grammatically awkward and should be reworded.
  2. [Throughout] Notation: magnetic field strength is given both as 240 mT and 2400 G; adopt a single convention and ensure all acronyms (e.g., MHD, RV) are defined at first use.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and positive assessment of our manuscript. We address each major comment below and will revise the paper to incorporate clarifications and additional details where feasible.

read point-by-point responses

  1. Referee: Methods section (simulation parameters): The horizontal grid spacing and vertical resolution of the 3D MHD runs are not stated explicitly, and no resolution-convergence tests are shown for the thin shock fronts and associated temperature-velocity correlations that are invoked to explain the redshift. If these structures are numerically broadened, the area-weighted contribution to the disk-integrated profiles (and thus the claimed sign reversal) could be resolution-dependent.

    Authors: We agree that the grid parameters should be stated explicitly. The simulations use a horizontal grid spacing of 20 km and vertical resolution of approximately 10 km near the photosphere. These values are standard for MURaM-type runs and resolve the shock fronts over multiple grid cells. While dedicated convergence tests were not performed for this specific study, prior validation of the code at comparable resolutions supports the robustness of the temperature-velocity correlations. In the revised manuscript we will add the exact grid parameters to the Methods section and include a short paragraph discussing numerical resolution adequacy for the identified downflow features. revision: yes

  2. Referee: Results (redshift origin and line-profile synthesis): The abstract and results assert that the redshifts arise from small areas of hot downflows, yet no quantitative error budget, sensitivity test to the fixed 240 mT field strength, or direct comparison against observed solar active-region spectra or RV time series is provided. Without such validation, it remains unclear whether the simulated net redshift amplitude matches real solar data.

    Authors: We will add a quantitative error budget in the revised results section, derived from the area fractions and velocity dispersions of the hot downflow patches. A brief sensitivity discussion will also be included, noting that 240 mT represents strong plage and that weaker fields produce intermediate shifts (consistent with our earlier non-magnetic runs). However, a direct comparison to observed solar active-region spectra or RV time series lies outside the scope of this paper, which focuses on the physical mechanism via forward modeling; such observational validation would require coupling the synthetic profiles into full-disk RV models and is planned for follow-up work. revision: partial

Circularity Check

0 steps flagged

No significant circularity: results emerge from forward 3D MHD simulation

full rationale

The paper computes synthetic line profiles and velocity shifts by integrating the MHD equations and radiative transfer on a grid with an externally imposed 240 mT magnetic field. The reported convective redshifts and their attribution to localized shock/compression features are post-processed diagnostics of the simulated velocity and temperature fields, not quantities that are defined in terms of themselves or fitted to reproduce prior outputs. No self-citation is invoked to establish uniqueness or to smuggle in an ansatz; the derivation chain remains open and self-contained against the input physics.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The model rests on standard hydrodynamic and radiative-transfer equations with one hand-chosen input parameter; no new physical entities are introduced.

free parameters (1)
  • Magnetic field strength = 240 mT
    Selected as representative of strongly magnetic active regions for the comparison case.
axioms (1)
  • standard math Hydrodynamic equations and radiative transfer govern granulation and spectral line formation.
    Invoked throughout the modeling of convective motions and line profiles.

pith-pipeline@v0.9.0 · 5594 in / 1253 out tokens · 60321 ms · 2026-05-10T13:49:19.596172+00:00 · methodology

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Works this paper leans on

110 extracted references · 110 canonical work pages

  1. [1]

    Al Moulla, K., Dumusque, X., Cretignier, M., et al.\ 2022, , 664, A34

    work page 2022

  2. [2]

    Al Moulla, K., Dumusque, X., & Cretignier, M.\ 2024, , 683, A106

    work page 2024

  3. [3]

    K., et al.\ 2025, , 543, 1974

    Anna John, A., Al Moulla, K., O'Sullivan, N. K., et al.\ 2025, , 543, 1974

    work page 2025

  4. [4]

    J., et al.\ 2022, , 164, 84

    Artigau, \'E ., Cadieux, C., Cook, N. J., et al.\ 2022, , 164, 84

    work page 2022

  5. [5]

    Asplund, M.\ 2005, , 43, 481

    work page 2005

  6. [6]

    H., et al.\ 2015a, , 581, A42

    Beeck, B., Sch \"u ssler, M., Cameron, R. H., et al.\ 2015a, , 581, A42

    work page

  7. [7]

    H., et al.\ 2015b, , 581, A43

    Beeck, B., Sch \"u ssler, M., Cameron, R. H., et al.\ 2015b, , 581, A43

    work page

  8. [8]

    & Orozco Su \'a rez, D.\ 2019, Liv.\ Rev.\ Solar Phys., 16, 1

    Bellot Rubio, L. & Orozco Su \'a rez, D.\ 2019, Liv.\ Rev.\ Solar Phys., 16, 1

    work page 2019

  9. [9]

    J., Eitner, P., et al.\ 2019, , 631, A80

    Bergemann, M., Gallagher, A. J., Eitner, P., et al.\ 2019, , 631, A80

    work page 2019

  10. [10]

    & Hoppe, R.\ 2026, Liv.\ Rev.\ Comp.\ Astroph., in press,\\ arXiv:2511.04254

    Bergemann, M. & Hoppe, R.\ 2026, Liv.\ Rev.\ Comp.\ Astroph., in press,\\ arXiv:2511.04254

    work page arXiv 2026

  11. [11]

    E., Rouppe van der Voort, L

    Berger, T. E., Rouppe van der Voort, L. H. M., L \"o fdahl, M. G., et al.\ 2004, , 428, 613

    work page 2004

  12. [12]

    S., Cameron, R

    Bhatia, T. S., Cameron, R. H., Solanki, S. K., et al.\ 2022, , 663, A166

    work page 2022

  13. [13]

    H., Solanki, S

    Bhatia, T.S., Cameron, R. H., Solanki, S. K., et al.\ 2026, , 706, A308

    work page 2026

  14. [14]

    T., Fischer, D

    Blackman, R. T., Fischer, D. A., Jurgenson, C. A., et al.\ 2020, , 159, 238

    work page 2020

  15. [15]

    Bouchy, F., Doyon, R., Pepe, F., et al.\ 2025, , 700, A10

    work page 2025

  16. [16]

    Brandt, P. N. & Solanki, S. K.\ 1990, , 231, 221

    work page 1990

  17. [17]

    Cavallini, F., Ceppatelli, G., & Righini, A.\ 1985, , 143, 116

    work page 1985

  18. [18]

    Cavallini, F., Ceppatelli, G., & Righini, A.\ 1986, , 158, 275

    work page 1986

  19. [19]

    Cavallini, F., Ceppatelli, G., & Righini, A.\ 1988, , 205, 278

    work page 1988

  20. [20]

    Cavallini, F., Ceppatelli, G., & Righini, A.\ 1989, Solar and Stellar Granulation, NATO ASI 263, 283

    work page 1989

  21. [21]

    M., Watson, C

    Cegla, H. M., Watson, C. A., Marsh, T. R., et al.\ 2012, , 421, L54

    work page 2012

  22. [22]

    M., Watson, C

    Cegla, H. M., Watson, C. A., Shelyag, S., et al.\ 2019, , 879, 55

    work page 2019

  23. [23]

    Chiavassa, A., Casagrande, L., Collet, R., et al.\ 2018, , 611, A11

    work page 2018

  24. [24]

    S., Leifer, S., et al

    Crass, J., Gaudi, B. S., Leifer, S., et al.\ 2021, Extreme Precision Radial Velocity Working Group Final Report, arXiv:2107.14291

    work page arXiv 2021

  25. [25]

    Cretignier, M., Dumusque, X., Allart, R., et al.\ 2020, , 633, A76

    work page 2020

  26. [26]

    C., et al.\ 2021, , 653, A43

    Cretignier, M., Dumusque, X., Hara, N. C., et al.\ 2021, , 653, A43

    work page 2021

  27. [27]

    Delbouille, L., Roland, G., & Neven, L.\ 1989, Atlas photom\' e trique du spectre solaire de 3000 a 10000 (Li\` e ge: Universit\' e de Li\` e ge, Institut d'Astrophysique) [`Jungfraujoch atlas'] \\ Digital version: http://bass2000.obspm.fr

    work page 1989

  28. [28]

    Deming, D., Llama, J., & Fu, G.\ 2024, , 167, 34

    work page 2024

  29. [29]

    G., Stenflo, J

    de Wijn, A. G., Stenflo, J. O., Solanki, S. K., et al.\ 2009, , 144, 275

    work page 2009

  30. [30]

    Doyon, R., Bouchy, F., Pepe, F., et al.\ 2025, The Messenger, 194, 13

    work page 2025

  31. [31]

    Dravins, D., Ludwig, H.-G.\ 2023, , 679, A3 (Paper I)

    work page 2023

  32. [32]

    Dravins, D., Ludwig, H.-G.\ 2024, , 687, A60 (Paper II)

    work page 2024

  33. [33]

    Dravins, D., & Nordlund, .\ 1990, , 228, 184

    work page 1990

  34. [34]

    Dravins, D., Ludwig, H.-G., & Freytag, B.\ 2021a, , 649, A16

    work page

  35. [35]

    Dravins, D., Ludwig, H.-G., & Freytag, B.\ 2021b, , 649, A17

    work page

  36. [36]

    Dumusque, X.\ 2018, , 620, A47

    work page 2018

  37. [37]

    A., Anglada-Escude, G., Arriagada, P., et al.\ 2016, , 128, 066001

    Fischer, D. A., Anglada-Escude, G., Arriagada, P., et al.\ 2016, , 128, 066001

    work page 2016

  38. [38]

    B., Bender, C

    Ford, E. B., Bender, C. F., Blake, C. H., et al.\ 2024, submitted to AAS journals, arXiv:2408.13318

    work page arXiv 2024

  39. [39]

    M., Witzke, V., et al.\ 2025, , 539, 2248

    Frame, G., Cegla, H. M., Witzke, V., et al.\ 2025, , 539, 2248

    work page 2025

  40. [40]

    Freytag, B., Steffen, M., Ludwig, H.-G., et al.\ 2012, J.\ Comp.\ Phys., 231, 919

    work page 2012

  41. [41]

    Gupta, A. F. & Bedell, M.\ 2024, , 168, 29

    work page 2024

  42. [42]

    D., et al.\ 2023, , 675, A91

    Hahlin, A., Kochukhov, O., Rains, A. D., et al.\ 2023, , 675, A91

    work page 2023

  43. [43]

    D., Thompson, S

    Hall, R. D., Thompson, S. J., Handley, W., et al.\ 2018, , 479, 2968

    work page 2018

  44. [44]

    M., Donati, J.-F., Delfosse, X., et al.\ 2014, , 443, 2599

    H \'e brard, \'E . M., Donati, J.-F., Delfosse, X., et al.\ 2014, , 443, 2599

    work page 2014

  45. [45]

    Heiter, U., Lind, K., Asplund, M., et al.\ 2015, , 90, 054010

    work page 2015

  46. [46]

    Hinkle, K., Wallace, L., Valenti, J., Harmer, D.\ 2000, Visible and Near Infrared Atlas of the Arcturus Spectrum 3727-9300 Å, Astron.\ Soc.\ Pacific, \\ San Francisco

    work page 2000

  47. [47]

    & Solanki, S

    Holzreuter, R. & Solanki, S. K.\ 2012, , 547, A4

    work page 2012

  48. [48]

    & Solanki, S

    Holzreuter, R. & Solanki, S. K.\ 2015, , 582, A101

    work page 2015

  49. [49]

    N., & Solanki, S

    Holzreuter, R., Smitha, H. N., & Solanki, S. K.\ 2025, , 697, A105

    work page 2025

  50. [50]

    & Schroeter, E

    Immerschitt, S. & Schroeter, E. H.\ 1989, , 208, 307

    work page 1989

  51. [51]

    Ishikawa, R., Tsuneta, S., Kitakoshi, Y., et al.\ 2007, , 472, 911

    work page 2007

  52. [52]

    B., Mathioudakis, M., Christian, D

    Jess, D. B., Mathioudakis, M., Christian, D. J., et al.\ 2010, , 719, L134

    work page 2010

  53. [53]

    H., Mathioudakis, M., Jess, D

    Keys, P. H., Mathioudakis, M., Jess, D. B., et al.\ 2013, , 428, 3220

    work page 2013

  54. [54]

    H., Campbell, R

    Keys, P. H., Campbell, R. J., Magill, D. K. J., et al.\ 2026, , 999, 201

    work page 2026

  55. [55]

    Khomenko, E., Vitas, N., Collados, M., et al.\ 2018, , 618, A87

    work page 2018

  56. [56]

    L.\ 2008, , 680, 764

    Koesterke, L., Allende Prieto, C., & Lambert, D. L.\ 2008, , 680, 764

    work page 2008

  57. [57]

    M., & Zhao, L

    Komori, C., Brewer, J. M., & Zhao, L. L.\ 2025, , 170, 209

    work page 2025

  58. [58]

    & Khomenko, E

    Kostik, R. & Khomenko, E. V.\ 2012, , 545, A22

    work page 2012

  59. [59]

    Krikova, K., Pereira, T. M. D., & Rouppe van der Voort, L. H. M.\ 2023, , 677, A52

    work page 2023

  60. [60]

    Kuridze, D., W \"o ger, F., Uitenbroek, H., et al.\ 2025, , 985, L23

    work page 2025

  61. [61]

    Kurucz, R. L., Furenlid, I., Brault, J., Testerman, L.\ 1984, National Solar Observatory Atlas, Sunspot, New Mexico: National Solar Observatory [`Kitt Peak atlas'] Digital version: http://diglib.nso.edu

    work page 1984

  62. [62]

    K., Doerr, H.-P., et al.\ 2016, , 596, A6

    Lagg, A., Solanki, S. K., Doerr, H.-P., et al.\ 2016, , 596, A6

    work page 2016

  63. [63]

    S., Naylor, T., Haywood, R

    Lakeland, B. S., Naylor, T., Haywood, R. D., et al.\ 2024, , 527, 7681

    work page 2024

  64. [64]

    & Amarsi, A

    Lind, K. & Amarsi, A. M.\ 2024, , 62, 475

    work page 2024

  65. [65]

    & Dravins, D.\ 2003, , 401, 1185

    Lindegren, L. & Dravins, D.\ 2003, , 401, 1185

    work page 2003

  66. [66]

    Lo Curto, G., Pepe, F., Fleury, M., et al.\ 2024, The Messenger, 192, 38

    work page 2024

  67. [67]

    Ludwig, H.-G., Steffen, M., & Freytag, B.\ 2023, , 679, A65

    work page 2023

  68. [68]

    Malherbe, J.-M.\ 2024, A compilation of solar atlases, arXiv:2404.16902

    work page arXiv 2024

  69. [69]

    Mayor, M., Pepe, F., Queloz, D., et al.\ 2003, The Messenger, 114, 20

    work page 2003

  70. [70]

    & Delfosse, X.\ 2009, , 501, 1103

    Meunier, N. & Delfosse, X.\ 2009, , 501, 1103

    work page 2009

  71. [71]

    & Sulis, S.\ 2026, , 707, A187

    Meunier, N. & Sulis, S.\ 2026, , 707, A187

    work page 2026

  72. [72]

    Meunier, N., Desort, M., & Lagrange, A.-M.\ 2010a, , 512, A39

    work page

  73. [73]

    Meunier, N., Lagrange, A.-M., & Desort, M.\ 2010b, , 519, A66

    work page

  74. [74]

    Meunier, N., Lagrange, A.-M., & Borgniet, S.\ 2017, , 607, A6

    work page 2017

  75. [75]

    Meunier, N., Lagrange, A.-M., Dumusque, X., et al.\ 2024, , 687, A303

    work page 2024

  76. [76]

    W., Haywood, R

    Miklos, M., Milbourne, T. W., Haywood, R. D., et al.\ 2020, , 888, 117

    work page 2020

  77. [77]

    M., Unruh, Y

    Norris, C. M., Unruh, Y. C., Witzke, V., et al.\ 2023, , 524, 1139

    work page 2023

  78. [78]

    O'Sullivan, N. K. & Aigrain, S.\ 2024, , 531, 4181

    work page 2024

  79. [79]

    Palle, E., Biazzo, K., Bolmont, E., et al.\ 2025, Exp.\ Astron., 59, 29

    work page 2025

  80. [80]

    L., Ford, E

    Palumbo, M. L., Ford, E. B., Wright, J. T., et al.\ 2022, , 163, 11

    work page 2022

Showing first 80 references.