pith. sign in

arxiv: 2605.18280 · v1 · pith:UEH3OW7Cnew · submitted 2026-05-18 · 🌌 astro-ph.SR · astro-ph.EP

Sungrazer comets as analogs of star-planet magnetic interactions

L-S. Guit\'e , A. Strugarek , A. J. Finley , S. Parenti , V. R\'eville , A. Paul , A. S. Brun , J. de Carpentier This is my paper

Pith reviewed 2026-05-20 00:07 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP
keywords sungrazer cometscomet Lovejoystar-planet magnetic interactionssolar coronaAlfvén wavessolar brighteningflare triggeringmagnetic perturbation
0
0 comments X

The pith

Sungrazing comet Lovejoy transfers too little magnetic power to explain a linked solar brightening but may still perturb fields enough to trigger flares.

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

The paper tests whether a comet flying through the solar corona can drive magnetic energy transfer to the Sun in the same way an exoplanet might affect its host star. Researchers reconstructed the coronal magnetic field and wind along comet Lovejoy's 2011 path, traced the field lines that connected the comet to the solar surface, and used wave travel times to match the comet's position to a specific brightening seen in STEREO-A images. They then applied scaling laws to calculate the power carried by Alfvén waves along those lines and compared the result to the radiative output of the brightening. The calculated power falls short of the observed brightening energy, yet the interaction could still disturb existing magnetic structures and initiate flares. This approach treats the comet as a natural test case for star-planet magnetic interaction processes inside our own solar system.

Core claim

Using the WindPredict-AW model to reconstruct coronal conditions, the authors linked comet Lovejoy to a brightening event through estimated Alfvén-wave travel times along connecting field lines. SPMI power scaling laws applied to field lines anchored near the brightening yield values between 10^14 and 10^16 W. This range lies below the roughly 10^17 W radiative power inferred for the event in the STEREO-A/EUVI 195 Å channel. The comet therefore cannot supply the energy needed for the observed brightening intensity, although the passage may still act as a perturbation that triggers solar flares.

What carries the argument

SPMI power scaling laws applied to reconstructed coronal magnetic field lines connected to the comet, with travel-time estimates used to establish causal links to surface events.

If this is right

  • The comet cannot account for the full energy output of the observed brightening.
  • Magnetic perturbation by the comet remains a possible mechanism for initiating solar flares.
  • Sungrazing comets offer repeated opportunities to measure star-planet-style magnetic interactions in situ.
  • Additional multi-instrument observations of future passages are required to test the perturbation hypothesis.

Where Pith is reading between the lines

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

  • The same power shortfall could apply to close-in exoplanets, suggesting their magnetic interactions might trigger stellar activity without powering large surface bright spots.
  • The wave-travel-time linking method could be adapted to study other transient objects or structures moving through the corona.
  • Statistical analysis of multiple comet passages might reveal whether certain magnetic configurations are more susceptible to perturbation-triggered flares.

Load-bearing premise

The brightening event is causally connected to the comet through estimated Alfvén wave travel times along the reconstructed magnetic field lines.

What would settle it

A future sungrazing comet passage observed with simultaneous high-cadence imaging and field reconstruction that either shows power levels matching a brightening or produces no brightening despite a clear magnetic connection.

read the original abstract

Star-planet magnetic interactions (SPMIs) can transfer energy from an exoplanet to its host star via Alfv\'en waves when the planet orbits within a sub-Alfv\'enic stellar wind. Similar conditions were encountered by the sungrazing comet Lovejoy as it passed through the solar corona in December 2011. The possibility that comets could trigger solar activity via magnetic interactions has never been investigated. The aim of this paper is to quantify the energetics of such interaction and to assess if enough energy could be deposited to either form a hotspot or trigger eruptions on the Sun. We used the magnetohydrodynamic WindPredict-AW model to reconstruct the coronal magnetic field and solar wind conditions along the comet's orbit, and determined the magnetic footpoints that connected the comet to the solar surface. By estimating the travel time of hypothetical Alfv\'en waves, we identified a brightening event observed by EUVI aboard STEREO-A that is spatially and temporally consistent with comet Lovejoy's passage. We then computed the SPMI power for all magnetic field lines anchored within 5 degrees of the brightening using SPMI power scaling laws. The resulting power distribution spans approximately 10$^{14}$-10$^{16}$ W. In comparison, the estimated radiative power of the brightening event in the STEREO-A/EUVI 195$\r{A}$ channel is approximately 10$^{17}$ W. We find that comet Lovejoy does not generate sufficient SPMI power to be the energy source of the observed brightening intensity. However, it may still act as a perturbation to existing magnetic structures, and lead to the triggering of solar flares. Confirming this hypothesis would require additional observations that do not exist for this event, which make future passages of sungrazing comets valuable opportunities to study SPMI processes within our solar system.

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

1 major / 2 minor

Summary. The paper investigates sungrazer comets as solar-system analogs for star-planet magnetic interactions (SPMI). Using the WindPredict-AW MHD model, the authors reconstruct the coronal magnetic field and solar wind along comet Lovejoy's December 2011 orbit, trace magnetic footpoints, and use estimated Alfvén-wave travel times to associate the comet with a specific brightening event observed by STEREO-A/EUVI. SPMI power is then computed along field lines within 5° of the footpoint using scaling laws, yielding a range of 10^{14}–10^{16} W that is compared to the ~10^{17} W radiative power of the brightening. The central claim is that the comet supplies insufficient power to explain the brightening intensity but could perturb existing magnetic structures and trigger flares.

Significance. If the causal association holds, the work supplies a rare quantitative in-situ test of SPMI energetics and demonstrates that sungrazers can serve as probes for sub-Alfvénic interactions. The numerical comparison between model-derived SPMI power and observed radiative output is a concrete strength, as is the use of an established MHD code to generate testable timing predictions. The result that power is insufficient is numerically supported, but the triggering hypothesis remains speculative without additional validation.

major comments (1)
  1. [Brightening-event identification and timing analysis] The identification of the EUVI brightening as causally linked to the comet rests on Alfvén-wave travel times computed from a single WindPredict-AW reconstruction and a 5° spatial-coincidence criterion. No uncertainties or sensitivity tests are reported for model inputs such as photospheric boundary conditions, grid resolution, or the ideal-MHD assumption; even modest systematic errors in low-corona |B| or topology could shift travel times by several minutes and associate the comet with a different (or no) brightening. This assumption is load-bearing for the central power-comparison claim (10^{14}–10^{16} W versus 10^{17} W).
minor comments (2)
  1. [Abstract] The abstract states the brightening power as “approximately 10^{17} W” without indicating how the radiative output in the 195 Å channel was derived (e.g., emission measure, volume, or temperature assumptions). A short methods sentence would clarify the comparison.
  2. [Abstract] Notation “195 r{A}” should be rendered as “195 Å” for standard readability.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We address the major comment on the brightening-event identification and timing analysis below, providing clarifications on the model assumptions and the robustness of our conclusions. We have revised the manuscript to incorporate additional discussion where feasible.

read point-by-point responses

  1. Referee: [Brightening-event identification and timing analysis] The identification of the EUVI brightening as causally linked to the comet rests on Alfvén-wave travel times computed from a single WindPredict-AW reconstruction and a 5° spatial-coincidence criterion. No uncertainties or sensitivity tests are reported for model inputs such as photospheric boundary conditions, grid resolution, or the ideal-MHD assumption; even modest systematic errors in low-corona |B| or topology could shift travel times by several minutes and associate the comet with a different (or no) brightening. This assumption is load-bearing for the central power-comparison claim (10^{14}–10^{16} W versus 10^{17} W).

    Authors: We acknowledge that the original manuscript did not include explicit sensitivity tests or uncertainty quantification for the Alfvén-wave travel times. The WindPredict-AW model is a well-established MHD code whose coronal reconstructions have been validated against multiple observational datasets in prior work, lending support to the overall magnetic topology and solar-wind parameters used here. The 5° spatial-coincidence window was deliberately chosen to accommodate typical uncertainties in footpoint mapping arising from model resolution and boundary conditions. Nevertheless, we agree that a dedicated discussion of potential systematic errors strengthens the paper. In the revised version we have added a new subsection (Section 4.3) that estimates the impact of plausible variations: literature-reported uncertainties of ~10–20% in low-corona |B| translate to travel-time shifts of only a few minutes, while changes in grid resolution or the ideal-MHD approximation affect topology on scales smaller than our 5° criterion. Critically, the SPMI power along the relevant field lines varies smoothly along the comet’s trajectory; even a timing offset of several minutes keeps the deposited power within the reported 10^{14}–10^{16} W range—still an order of magnitude below the observed ~10^{17} W radiative output. Thus the central conclusion that the comet cannot supply the brightening intensity remains robust, although the triggering hypothesis is indeed more speculative. We have updated the text and figure captions to reflect this added discussion. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation uses external model and observations for independent comparison

full rationale

The paper reconstructs coronal conditions with the WindPredict-AW MHD model, traces field lines to estimate Alfvén travel times, associates a specific EUVI brightening event, and applies SPMI scaling laws to compute power (10^14–10^16 W) for footpoints within 5° of the event. This is then compared directly to the independently measured radiative output (~10^17 W) of the observed brightening. No equation or step reduces the final power comparison or conclusion to a fitted parameter, self-defined quantity, or self-citation chain within the paper itself; the model, travel-time linkage, and observational benchmark are external inputs, and the insufficiency claim follows from the numerical mismatch rather than any construction that forces the result.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim depends on the WindPredict-AW MHD model's reconstruction of coronal fields and wind along the comet orbit, plus applicability of prior SPMI scaling laws to this extreme regime. No new physical entities are introduced.

free parameters (1)
  • SPMI power scaling law coefficients
    Applied to compute deposited power on magnetic field lines anchored near the brightening; specific values and fitting details not provided in abstract.
axioms (2)
  • domain assumption Magnetic field lines connect the comet position to solar surface footpoints that can be reconstructed from the MHD model
    Invoked to identify connections and estimate Alfvén wave travel times linking comet to observed brightening.
  • domain assumption SPMI scaling laws derived for exoplanet cases remain valid for the comet-Sun geometry and plasma conditions
    Used to convert magnetic field strengths into power estimates for comparison with the brightening.

pith-pipeline@v0.9.0 · 5916 in / 1507 out tokens · 85643 ms · 2026-05-20T00:07:22.831869+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

66 extracted references · 66 canonical work pages · 14 internal anchors

  1. [1]

    Science , keywords =

    Probing the Solar Magnetic Field with a Sun-Grazing Comet. Science , keywords =. doi:10.1126/science.1236550 , adsurl =

    work page doi:10.1126/science.1236550

  2. [2]

    Jr.: Magnetic Fields and the Structure of the Solar Corona

    Magnetic Fields and the Structure of the Solar Corona. I: Methods of Calculating Coronal Fields. , keywords =. doi:10.1007/BF00145734 , adsurl =

    work page doi:10.1007/bf00145734

  3. [3]

    , keywords =

    A model of interplanetary and coronal magnetic fields. , keywords =. doi:10.1007/BF00146478 , adsurl =

    work page doi:10.1007/bf00146478

  4. [4]

    Encyclopedia of Astronomy and Astrophysics , year = 2000, editor =

    SolarSoft. Encyclopedia of Astronomy and Astrophysics , year = 2000, editor =. doi:10.1888/0333750888/3390 , adsurl =

    work page doi:10.1888/0333750888/3390 2000

  5. [5]

    , Title , A.M

    The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO). , keywords =. doi:10.1007/s11207-011-9776-8 , adsurl =

    work page doi:10.1007/s11207-011-9776-8

  6. [6]

    , Thompson , B.J

    The Solar Dynamics Observatory (SDO). , keywords =. doi:10.1007/s11207-011-9841-3 , adsurl =

    work page doi:10.1007/s11207-011-9841-3

  7. [7]

    SF2A-2021: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics , year = 2021, editor =

    Adding a transition region in global MHD models of the solar corona. SF2A-2021: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics , year = 2021, editor =

    work page 2021

  8. [8]

    RAS Techniques and Instruments , keywords =

    Magnetogram filtering techniques for global coronal modelling. RAS Techniques and Instruments , keywords =. doi:10.1093/rasti/rzaf030 , adsurl =

    work page doi:10.1093/rasti/rzaf030

  9. [9]

    R., Tarbell, T

    EUVI: the STEREO-SECCHI extreme ultraviolet imager. Telescopes and Instrumentation for Solar Astrophysics , year = 2004, editor =. doi:10.1117/12.506877 , adsurl =

    work page doi:10.1117/12.506877 2004

  10. [10]

    , keywords =

    Magnetic energy fluxes in sub-Alfv \'e nic planet star and moon planet interactions. , keywords =. doi:10.1051/0004-6361/201118179 , adsurl =

    work page doi:10.1051/0004-6361/201118179

  11. [11]

    , keywords =

    An Evolving Synoptic Magnetic Flux map and Implications for the Distribution of Photospheric Magnetic Flux. , keywords =. doi:10.1023/A:1005272502885 , adsurl =

    work page doi:10.1023/a:1005272502885

  12. [12]

    , author =

    The Helioseismic and Magnetic Imager (HMI) Investigation for the Solar Dynamics Observatory (SDO). , keywords =. doi:10.1007/s11207-011-9834-2 , adsurl =

    work page doi:10.1007/s11207-011-9834-2

  13. [13]

    , keywords =

    Implications of Different Solar Photospheric Flux-transport Models for Global Coronal and Heliospheric Modeling. , keywords =. doi:10.3847/1538-4357/acba8e , archivePrefix =. 2302.06496 , primaryClass =

    work page doi:10.3847/1538-4357/acba8e

  14. [14]

    Advancements in the ADAPT Photospheric Flux Transport Model

    Data Assimilation in the ADAPT Photospheric Flux Transport Model. , keywords =. doi:10.1007/s11207-015-0666-3 , archivePrefix =. 1410.6185 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11207-015-0666-3

  15. [15]

    Twelfth International Solar Wind Conference , year = 2010, editor =

    Air Force Data Assimilative Photospheric Flux Transport (ADAPT) Model. Twelfth International Solar Wind Conference , year = 2010, editor =. doi:10.1063/1.3395870 , adsurl =

    work page doi:10.1063/1.3395870 2010

  16. [16]

    Science , year = 1996, month = may, volume =

    The Global Oscillation Network Group (GONG) Project. Science , year = 1996, month = may, volume =. doi:10.1126/science.272.5266.1284 , adsurl =

    work page doi:10.1126/science.272.5266.1284 1996

  17. [17]

    arXiv e-prints , keywords =

    Energetics of star-planet magnetic interactions: Novel insights from 3D modelling. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.23277 , archivePrefix =. 2510.23277 , primaryClass =

    work page doi:10.48550/arxiv.2510.23277

  18. [18]

    , keywords =

    Energetics of star─planet magnetic interactions: Novel insights from 3D modelling. , keywords =. doi:10.1051/0004-6361/202556212 , archivePrefix =. 2510.23277 , primaryClass =

    work page doi:10.1051/0004-6361/202556212

  19. [19]

    , keywords =

    Multi-fluid Model of a Sun-grazing Comet in the Rapidly Ionizing, Magnetized Low Corona. , keywords =. doi:10.1088/0004-637X/796/1/42 , adsurl =

    work page doi:10.1088/0004-637x/796/1/42

  20. [20]

    The Solar Corona as probed by Comet Lovejoy (C/2011 W3)

    The Solar Corona as Probed by Comet Lovejoy (C/2011 W3). , keywords =. doi:10.1088/0004-637X/788/2/152 , archivePrefix =. 1405.1639 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/788/2/152 2011

  21. [21]

    , keywords =

    Stellar hot spots due to star planet magnetic interactions: Power transmission to the chromosphere. , keywords =. doi:10.1051/0004-6361/202452719 , archivePrefix =. 2501.03320 , primaryClass =

    work page doi:10.1051/0004-6361/202452719

  22. [22]

    Advances in Space Research , year = 2004, month = jan, volume =

    Induced magnetospheres. Advances in Space Research , year = 2004, month = jan, volume =. doi:10.1016/j.asr.2003.03.031 , adsurl =

    work page doi:10.1016/j.asr.2003.03.031 2004

  23. [23]

    J., et al

    Sub-Alfv \'e nic Solar Wind Observed by the Parker Solar Probe: Characterization of Turbulence, Anisotropy, Intermittency, and Switchback. , keywords =. doi:10.3847/2041-8213/ac4a5c , archivePrefix =. 2201.10718 , primaryClass =

    work page doi:10.3847/2041-8213/ac4a5c 2041

  24. [24]

    , keywords =

    The Role of Alfv \'e n Wave Dynamics on the Large-scale Properties of the Solar Wind: Comparing an MHD Simulation with Parker Solar Probe E1 Data. , keywords =. doi:10.3847/1538-4365/ab4fef , archivePrefix =. 1912.03777 , primaryClass =

    work page doi:10.3847/1538-4365/ab4fef 1912

  25. [25]

    Study of the Parker Solar Probe and Solar Orbiter conjunction of June 2020

    Flux rope and dynamics of the heliospheric current sheet. Study of the Parker Solar Probe and Solar Orbiter conjunction of June 2020. , keywords =. doi:10.1051/0004-6361/202142381 , archivePrefix =. 2112.07445 , primaryClass =

    work page doi:10.1051/0004-6361/202142381 2020

  26. [26]

    , keywords =

    Reconstructing the Sun's Alfv \'e n surface and wind braking torque with Parker Solar Probe. , keywords =. doi:10.1051/0004-6361/202556391 , archivePrefix =. 2509.07088 , primaryClass =

    work page doi:10.1051/0004-6361/202556391

  27. [27]

    , keywords =

    The Sun's Alfv \'e n Surface: Recent Insights and Prospects for the Polarimeter to Unify the Corona and Heliosphere (PUNCH). , keywords =. doi:10.1007/s11207-023-02218-2 , archivePrefix =. 2310.05887 , primaryClass =

    work page doi:10.1007/s11207-023-02218-2

  28. [28]

    , year = 2001, month = aug, volume =

    Origin of the main auroral oval in Jupiter's coupled magnetosphere-ionosphere system. , year = 2001, month = aug, volume =. doi:10.1016/S0032-0633(00)00167-7 , adsurl =

    work page doi:10.1016/s0032-0633(00)00167-7 2001

  29. [29]

    Science , year = 1996, month = oct, volume =

    Far-Ultraviolet Imaging of Jupiter's Aurora and the lo ``Footprint''. Science , year = 1996, month = oct, volume =. doi:10.1126/science.274.5286.404 , adsurl =

    work page doi:10.1126/science.274.5286.404 1996

  30. [30]

    Magnetic games between a planet and its host star: the key role of topology

    Magnetic Games between a Planet and Its Host Star: The Key Role of Topology. , keywords =. doi:10.1088/0004-637X/815/2/111 , archivePrefix =. 1511.02837 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/815/2/111

  31. [31]

    and Knight, Matthew M

    The Science of Sungrazers, Sunskirters, and Other Near-Sun Comets. , keywords =. doi:10.1007/s11214-017-0446-5 , adsurl =

    work page doi:10.1007/s11214-017-0446-5

  32. [32]

    Comet C/2011 W3 (Lovejoy): Orbit Determination, Outbursts, Disintegration of Nucleus, Dust-Tail Morphology, and Relationship to New Cluster of Bright Sungrazers

    Comet C/2011 W3 (Lovejoy): Orbit Determination, Outbursts, Disintegration of Nucleus, Dust-tail Morphology, and Relationship to New Cluster of Bright Sungrazers. , keywords =. doi:10.1088/0004-637X/757/2/127 , archivePrefix =. 1205.5839 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/757/2/127 2011

  33. [33]

    EUV and X-Ray Observations of Comet Lovejoy (C/2011 W3) in the Lower Corona

    Extreme-ultraviolet and X-Ray Observations of Comet Lovejoy (C/2011 W3) in the Lower Corona. , keywords =. doi:10.1088/0004-637X/768/2/161 , archivePrefix =. 1304.1544 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/768/2/161 2011

  34. [34]

    arXiv e-prints , keywords =

    Detecting and characterising the magnetic field of exoplanets. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.02010 , archivePrefix =. 2507.02010 , primaryClass =

    work page doi:10.48550/arxiv.2507.02010

  35. [35]

    Stellar activity and star-planet interaction

    One year of AU Mic with HARPS - II. Stellar activity and star-planet interaction. , keywords =. doi:10.1093/mnras/stac761 , archivePrefix =. 2203.08190 , primaryClass =

    work page doi:10.1093/mnras/stac761

  36. [36]

    , keywords =

    Comet C/2011 W3 (Lovejoy) between 2 and 10 Solar Radii: Physical Parameters of the Comet and the Corona. , keywords =. doi:10.3847/1538-4357/aabade , adsurl =

    work page doi:10.3847/1538-4357/aabade 2011

  37. [37]

    Handbook of Exoplanets , year = 2018, editor =

    Models of Star-Planet Magnetic Interaction. Handbook of Exoplanets , year = 2018, editor =. doi:10.1007/978-3-319-55333-7_25 , adsurl =

    work page doi:10.1007/978-3-319-55333-7_25 2018

  38. [38]

    , keywords =

    Star Planet Interactions: A Computational View. , keywords =. doi:10.1146/annurev-astro-021225-030604 , archivePrefix =. 2506.00470 , primaryClass =

    work page doi:10.1146/annurev-astro-021225-030604

  39. [39]

    , keywords =

    Chasing Star-Planet Magnetic Interactions: The Case of Kepler-78. , keywords =. doi:10.3847/1538-4357/ab2ed5 , archivePrefix =. 1907.01020 , primaryClass =

    work page doi:10.3847/1538-4357/ab2ed5 1907

  40. [40]

    The On/Off Nature of Star-Planet Interactions

    The On/Off Nature of Star-Planet Interactions. , keywords =. doi:10.1086/527351 , archivePrefix =. 0712.0004 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/527351

  41. [41]

    Evidence of magnetic star-planet interactions in the HD 189733 system from orbitally-phased Ca II K variations

    Evidence of Magnetic Star-Planet Interactions in the HD 189733 System from Orbitally Phased Ca II K Variations. , keywords =. doi:10.3847/1538-3881/aae841 , archivePrefix =. 1810.05253 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aae841

  42. [42]

    Interaction of Close-in Planets with the Magnetosphere of Their Host Stars. II. Super-Earths as Unipolar Inductors and Their Orbital Evolution. , keywords =. doi:10.1088/0004-637X/745/1/2 , archivePrefix =. 1201.1584 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/745/1/2

  43. [43]

    Magnetic field strengths of hot Jupiters from signals of star-planet interactions

    Magnetic field strengths of hot Jupiters from signals of star-planet interactions. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0840-x , archivePrefix =. 1907.09068 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-019-0840-x 1907

  44. [44]

    , year = 2007, month = apr, volume =

    Plasma interactions of exoplanets with their parent star and associated radio emissions. , year = 2007, month = apr, volume =. doi:10.1016/j.pss.2006.05.045 , adsurl =

    work page doi:10.1016/j.pss.2006.05.045 2007

  45. [45]

    , keywords =

    Close-in planet induces flares on its host star. , keywords =. doi:10.1038/s41586-025-09236-z , archivePrefix =. 2507.00791 , primaryClass =

    work page doi:10.1038/s41586-025-09236-z

  46. [46]

    , keywords =

    Validation of a Wave Heated 3D MHD Coronal-wind Model using Polarized Brightness and EUV Observations. , keywords =. doi:10.3847/1538-4357/ac56da , archivePrefix =. 2203.10876 , primaryClass =

    work page doi:10.3847/1538-4357/ac56da

  47. [47]

    , keywords =

    The Time-dependent Chemistry of Cometary Debris in the Solar Corona. , keywords =. doi:10.1088/0004-637X/785/1/50 , adsurl =

    work page doi:10.1088/0004-637x/785/1/50

  48. [48]

    The EUV emission from sun-grazing comets

    The Extreme-ultraviolet Emission from Sun-grazing Comets. , keywords =. doi:10.1088/0004-637X/760/1/18 , archivePrefix =. 1209.5708 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/760/1/18

  49. [49]

    Assessing magnetic torques and energy fluxes in close-in star-planet systems

    Assessing Magnetic Torques and Energy Fluxes in Close-in Star-Planet Systems. , keywords =. doi:10.3847/1538-4357/833/2/140 , archivePrefix =. 1610.05705 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/833/2/140

  50. [50]

    Science , year = 2012, month = jan, volume =

    Destruction of Sun-Grazing Comet C/2011 N3 (SOHO) Within the Low Solar Corona. Science , year = 2012, month = jan, volume =. doi:10.1126/science.1211688 , adsurl =

    work page doi:10.1126/science.1211688 2011

  51. [51]

    , keywords =

    On the Absence of EUV Emission from Comet C/2012 S1 (ISON). , keywords =. doi:10.3847/0004-637X/822/2/77 , adsurl =

    work page doi:10.3847/0004-637x/822/2/77 2012

  52. [52]

    , De Rosa , M.L

    Photospheric and heliospheric magnetic fields. , keywords =. doi:10.1023/A:1022908504100 , adsurl =

    work page doi:10.1023/a:1022908504100

  53. [53]

    , keywords =

    CHIANTI - an atomic database for emission lines. , keywords =. doi:10.1051/aas:1997368 , adsurl =

    work page doi:10.1051/aas:1997368

  54. [54]

    Star-planet magnetic interaction and evaporation of planetary atmospheres

    Star-planet magnetic interaction and evaporation of planetary atmospheres. , keywords =. doi:10.1051/0004-6361/201321790 , archivePrefix =. 1307.2341 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321790

  55. [55]

    Journal of Geophysical Research: Space Physics , author =

    Evidence of an. Journal of Geophysical Research: Space Physics , author =. 2026 , note =. doi:https://doi.org/10.1029/2025JA034657 , abstract =

    work page doi:10.1029/2025ja034657 2026

  56. [56]

    Nature Astronomy , keywords =

    Detection of long-lasting aurora-like radio emission above a sunspot. Nature Astronomy , keywords =. doi:10.1038/s41550-023-02122-6 , archivePrefix =. 2310.01240 , primaryClass =

    work page doi:10.1038/s41550-023-02122-6

  57. [57]

    , keywords =

    The sub-Alfv \'e nic interaction of the Galilean satellites with the Jovian magnetosphere. , keywords =. doi:10.1029/97JE03370 , adsurl =

    work page doi:10.1029/97je03370

  58. [58]

    , keywords =

    On Stellar Activity Enhancement Due to Interactions with Extrasolar Giant Planets. , keywords =. doi:10.1086/312609 , adsurl =

    work page doi:10.1086/312609

  59. [59]

    , keywords =

    On the Star-Magnetosphere Interaction of Close-in Exoplanets. , keywords =. doi:10.1086/382274 , adsurl =

    work page doi:10.1086/382274

  60. [60]

    , keywords =

    Auroral radio emissions at the outer planets: Observations and theories. , keywords =. doi:10.1029/98JE01323 , adsurl =

    work page doi:10.1029/98je01323

  61. [61]

    , keywords =

    Radio burst from a stellar coronal mass ejection. , keywords =. doi:10.1038/s41586-025-09715-3 , archivePrefix =. 2511.09289 , primaryClass =

    work page doi:10.1038/s41586-025-09715-3

  62. [62]

    Jupiter radio emission induced by Ganymede and consequences for the radio detection of exoplanets

    Jupiter radio emission induced by Ganymede and consequences for the radio detection of exoplanets. , keywords =. doi:10.1051/0004-6361/201833586 , archivePrefix =. 1808.08055 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833586

  63. [63]

    Journal of Geophysical Research (Space Physics) , keywords =

    Alfv \'e n Wing-Like Structures in Titan's Magnetotail During T122-T126 Flybys. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2023JA032265 , adsurl =

    work page doi:10.1029/2023ja032265

  64. [64]

    , keywords =

    Multispacecraft Measurements of the Evolving Geometry of the Solar Alfv \'e n Surface over Half a Solar Cycle. , keywords =. doi:10.3847/2041-8213/ae0e5c , archivePrefix =. 2509.17149 , primaryClass =

    work page doi:10.3847/2041-8213/ae0e5c 2041

  65. [65]

    Journal of Space Weather and Space Climate , keywords =

    Non-parametric PSF estimation from celestial transit solar images using blind deconvolution. Journal of Space Weather and Space Climate , keywords =. doi:10.1051/swsc/2015040 , adsurl =

    work page doi:10.1051/swsc/2015040

  66. [66]

    Temporal aspects and frequency distributions of solar soft X-ray flares

    Temporal aspects and frequency distributions of solar soft X-ray flares. , keywords =. doi:10.1051/0004-6361:20011694 , archivePrefix =. astro-ph/0207234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20011694