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REVIEW 2 major objections 5 minor 105 references

SKA can detect magnetic star-planet radio emission and measure exoplanet fields, but only with monitoring time comparable to optical M-SPI campaigns.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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T0 review · grok-4.5

2026-07-12 04:39 UTC pith:VKDUPBZE

load-bearing objection Solid SKA science-case chapter: updated ensemble fluxes + ExPRES visibility sims + a concrete multi-tier observing plan; the β extrapolation is the known soft spot and is shown openly. the 2 major comments →

arxiv 2607.03133 v1 pith:VKDUPBZE submitted 2026-07-03 astro-ph.EP astro-ph.IMastro-ph.SR

Radio emission from star-planet interactions

H.K. Vedantham , A. Strugarek , C.K. Louis , J.R. Callingham , L. Pe\~na-Mo\~nino , M. P\'erez-Torres , P. Zarka , E. Mauduit
show 7 more authors
N. Duch\^ene P. Amado S. Bloot R. D. Kavanagh A. A. Vidotto L. Lamy C. Tasse
This is my paper
classification astro-ph.EP astro-ph.IMastro-ph.SR
keywords magnetic star-planet interactionelectron cyclotron maserSKAexoplanet magnetic fieldsAlfvén wingsradio flux density predictionsM dwarfs
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Close-in exoplanets and their host stars exchange energy through magnetized plasma. That exchange, called magnetic star-planet interaction (M-SPI), can launch electron-cyclotron maser radio waves from both the star and the planet. The radio signal carries the magnetic field strength and topology of the emitter plus the orbital and rotational geometry of the system—quantities that optical and X-ray tracers cannot supply directly. No secure radio detection yet exists, mainly because present telescopes lack sensitivity and because almost no long-term monitoring has been invested. The paper shows that SKA-Low, once it reaches microjansky sensitivity, will open a large fraction of nearby systems to detection, provided observers allocate hundreds of hours per target—the same scale of effort that finally revealed optical M-SPI signatures. The practical path is a shallow all-sky circular-polarization survey followed by multi-orbit campaigns on the brightest candidates.

Core claim

The Square Kilometre Array will make radio detection of magnetic star-planet interaction transformative for exoplanet science, but only if it is given observing time comparable to the multi-year optical campaigns that already established the existence of M-SPI.

What carries the argument

Electron-cyclotron maser instability (ECMI) emission: coherent radiation generated near the local cyclotron frequency (ν_c = 2.8 B MHz) that is strongly beamed along a magnetic cone; its high-frequency cutoff directly measures the surface magnetic field of the emitter and its time-frequency “arch” morphology encodes orbital and rotational geometry.

Load-bearing premise

The fraction of intercepted magnetic energy that becomes radio waves is assumed to be the same few-tenths of a percent measured for solar-system planets, even though close-in exoplanets operate at much higher energies and different plasma conditions.

What would settle it

A multi-orbit SKA-Low campaign on a short-period planet around a nearby M dwarf that fails to recover the predicted arch-like, phase-locked circularly polarized bursts at the expected cyclotron frequencies would falsify the claim that present scaling laws and SKA sensitivity are sufficient for secure detection.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. This chapter for Advancing Astrophysics with the SKA – II reviews magnetic star–planet interaction (M-SPI) and the prospects for detecting its radio signatures (primarily star-side ECMI) with SKA-Low/Mid. It summarises the sub- versus super-Alfvénic regimes, the family of Poynting-flux scaling laws (Alfvén-wing, reconnection, stretch-and-break, and the Paul & Strugarek upper limit), and the conversion of intercepted power into beamed ECMI emission. Ensemble flux-density predictions are constructed for known exoplanets using published stellar magnetic-field catalogues, Parker-wind models and solar-system-calibrated efficiency β ≈ 2 × 10^{-3}. ExPRES simulations illustrate the characteristic arch-like, periodically modulated dynamic spectra that would serve as a smoking-gun signature. The authors conclude that SKA can transformatively detect M-SPI radio emission, but only with substantial, multi-orbit monitoring time comparable to successful optical campaigns, and they outline a two-tier survey-plus-targeted strategy.

Significance. If the advocated observing programme is executed and detections materialise, radio M-SPI would supply the only direct, model-independent measurement of exoplanet magnetic-field strength and topology, together with unique constraints on stellar-wind conditions and orbital–rotational geometry. The manuscript is a well-structured science case rather than a new derivation; its principal strengths are the transparent display of order-of-magnitude model scatter (Figs. 2–4), the use of ExPRES to generate falsifiable time–frequency templates, and the explicit linkage of required telescope time to the optical-band precedent that has already yielded secure M-SPI detections. These elements make the chapter a useful community planning document for SKA exoplanet science.

major comments (2)
  1. §2.1–2.2 and Figs. 3–4: every quantitative flux prediction rests on the solar-system empirical conversion efficiency β = 2 × 10^{-3} (and the associated Poynting-flux scalings). The manuscript correctly notes that the same efficiency may not hold at the higher energies and different plasma conditions of close-in exoplanets, yet the ensemble still presents absolute mJy/μJy values against SKA AA4 sensitivity without error bars or a systematic sensitivity study that varies β over its stated 10^{-4}–10^{-2} range. Because the central claim is that SKA will be transformative once sufficient time is invested, a short quantitative exploration of how the detectable fraction scales with β (or an explicit statement that the numbers are order-of-magnitude only) is needed to keep the advocacy claim load-bearing.
  2. §2.2, emission-escape filter: systems are labelled ‘Emission likely’ solely when f_ce > 10 f_pe at the stellar surface and the flow is sub-Alfvénic. The text itself acknowledges that radiative-transfer absorption near the source and beaming geometry are omitted; the latter is only later assigned a ~10 % visibility fraction. These filters directly determine the ‘few tens of percent’ yield quoted for SKA-Low AA4. A clearer statement of how the quoted fractions change when the beaming duty cycle and a more realistic coronal absorption criterion are folded in would strengthen the quantitative support for the observing strategy in §3.
minor comments (5)
  1. Abstract and opening paragraph: ‘though gravity’ → ‘through gravity’.
  2. Fig. 2 caption and legend: the horizontal dashed lines are described as SKA AA4 sensitivity for 100 MHz / 1 h; a brief note on whether the plotted flux densities already include the assumed beam solid angle Ω would aid direct comparison.
  3. §2.2: the second-order polynomial mass–radius fit is given without a stated validity range or residual scatter; a short clause would help readers assess its impact on the ensemble.
  4. Fig. 5: the colour scale for circular polarisation is described in the caption but the panels themselves would benefit from an explicit colour bar for readers of the printed version.
  5. References: a few arXiv-only or ‘under review’ entries (e.g., Paul & Strugarek 2025, Tasse et al. 2026, Revilla et al. 2026) should be updated or flagged as such at the proof stage.

Circularity Check

0 steps flagged

No significant circularity: science-case flux predictions and strategy rest on openly empirical solar-system scalings plus external catalogs, not on self-definitional reductions or load-bearing self-citation tautologies.

full rationale

This is a community white-paper / SKA science case, not a derivation paper claiming a new first-principles result. The load-bearing quantitative inputs are (i) the family of Poynting-flux scalings (Alfvén-wing, reconnection, stretch-and-break, Paul–Strugarek upper limit) taken from the literature, (ii) the solar-system empirical conversion efficiency β ≈ 2×10^{-3} (Zarka), and (iii) stellar magnetic-field and wind parameters drawn from published catalogs (Duchêne et al., exoplanet.eu, ROSAT, Gaia). These are applied to known exoplanets to produce ensemble flux-density estimates (Figs. 2–4) and ExPRES visibility patterns (Fig. 5). The paper itself displays the order-of-magnitude model scatter and the beaming/duty-cycle caveats; nothing is redefined so that a “prediction” equals its own fit by construction. Self-citations (Callingham, Vedantham, Louis, Strugarek, Tasse, Kavanagh, Mauduit, etc.) supply prior observational non-detections, simulation codes, or magnetic-field compilations that are independently falsifiable or machine-reproducible; they do not close a uniqueness loop that forces the SKA advocacy claim. The optical-band time-investment precedent is an external analogy, not a circular premise. Score 1 reflects only the normal presence of co-author citations that are not load-bearing for any claimed derivation.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

Central claim rests on solar-system-calibrated conversion efficiencies, ideal-MHD wind models, and the assumption that ECMI beaming and escape conditions observed at Jupiter scale to M-dwarf systems. Free parameters are the efficiency β and the various geometric factors in the three scaling laws; axioms are standard plasma-physics results plus domain assumptions about stellar winds and dynamos. No wholly invented entities.

free parameters (3)
  • β (Poynting-to-radio conversion efficiency) = 2e-3
    Fixed at the solar-system empirical value 2×10^{-3} (range 10^{-4}–10^{-2}); every flux-density number in §2 and Figs. 2–4 scales linearly with it.
  • α, γ, f_ap (interaction efficiency factors in Alfvén-wing / reconnection / stretch-and-break models)
    Order-unity geometric or reconnection-efficiency factors left free or set to literature defaults; produce the 1–3 order-of-magnitude model scatter shown in Fig. 2.
  • planetary surface field B_p (geometric mean of Busse/Mizutani/Sano dynamos)
    Unknown for every exoplanet; estimated from mass/radius/rotation via three published scaling laws whose geometric mean is adopted.
axioms (4)
  • domain assumption ECMI emission occurs near the local cyclotron frequency ν_c = 2.8 (B/G) MHz and is beamed into a hollow cone of opening angle ≳70°.
    Standard plasma result (Treumann 2006) used throughout §1.2 and the ExPRES simulations of §2.3.
  • domain assumption Intercepted Poynting flux scales as (B_sw R_eff)^2 v_rel and a fixed fraction β is converted to radio power.
    Core of all three analytic models and the empirical solar-system law (Zarka 2007); enters Eq. (1)–(6).
  • domain assumption Stellar wind can be approximated by a 1-D isothermal Parker solution with base density scaled from solar mass-loss and magnetic field extrapolated as dipole then Parker spiral.
    Used for the entire ensemble calculation in §2.2; acknowledged as conservative.
  • ad hoc to paper Only systems with f_ce > 10 f_pe at the stellar surface and sub-Alfvénic flow are labeled ‘emission likely’.
    Simple binary filter adopted in §2.2 because full radiative-transfer knowledge is unavailable.

pith-pipeline@v1.1.0-grok45 · 24925 in / 3012 out tokens · 33437 ms · 2026-07-12T04:39:18.797050+00:00 · methodology

0 comments
read the original abstract

Stars interact with their exoplanets though gravity, radiation, plasma and magnetic fields. Stellar plasma and magnetic fields impose electrodynamic effects on exoplanet atmospheres and interiors that include heating, aurorae and atmospheric mass loss. The planets in turn can excite Alfv\'enic disturbances that are dissipated on the star leading to chromospheric heating and flares. This interaction, broadly called magnetic star-planet interaction (M-SPI), can also generate radio signatures both from the star and the exoplanet. The radio emission encodes information on the dynamics/energetics of the interaction, the magnetic field strength and topology of the emitter and the orbital/rotational geometry of the system -- information that is difficult or in some cases implausible to obtain by other means. Yet we do not have a conclusive detection of M-SPI in the radio band primarily due to sensitivity limitations and scarce observing time spent monitoring promising targets. Here we describe the scientific motivation to study M-SPI in exoplanetary systems, to get progress in understanding its predicted signal strength and phenomenology. We argue that the SKA telescopes can make a transformative contribution to exoplanet science by detecting M-SPI in the radio band but this will require substantial observing time -- similar to that afforded to successful optical-band searches for M-SPI signatures.

Figures

Figures reproduced from arXiv: 2607.03133 by A. A. Vidotto, A. Strugarek, C.K. Louis, C. Tasse, E. Mauduit, H.K. Vedantham, J.R. Callingham, L. Lamy, L. Pe\~na-Mo\~nino, M. P\'erez-Torres, N. Duch\^ene, P. Amado, P. Zarka, R. D. Kavanagh, S. Bloot.

Figure 1
Figure 1. Figure 1: Sketch showing M-SPI regimes. Left panel: Sub-Alfvénic case where Alfvén wing/s (purple tube) created by the planet’s flow connect back to the star and produce radio emission (cyan cone) in the stellar magnetosphere. Part of the energy can also produce radio emission in the magnetosphere of the planet (not shown in figure). Right panel: Super Alfvénic case where energy flow back to the star is not possible… view at source ↗
Figure 2
Figure 2. Figure 2 [PITH_FULL_IMAGE:figures/full_fig_p009_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Intercepted Poynting flux times 2 × 10−3 (efficiency factor) for an ensemble of representative planet and star properties based on known exoplanets. Left and right panels show the flux against semi-major axis (of the planet’s orbit) and the planet’s mass, respectively. The points are colour coded by whether the interaction is expected to be sub- or super-Alfénic. In rare cases, the regime is sub-Alfénic in… view at source ↗
Figure 4
Figure 4. Figure 4: Predicted stellar radio flux density (only for sub-Alfvénic inter￾action) as a function of the peak cyclotron frequency. The different colours denote cases where escape of radiation is likely (orange) and un￾likely (magenta) respectively. The greenish-blue line marks the antici￾pated SKA telescopes’ AA4 detection limit for a fixed 100 MHz bandwidth and 1 hr integration. expect radio powers of up to 1013−14… view at source ↗
Figure 5
Figure 5. Figure 5: Simulations of SPI radio emissions (left column) for an axi-symmetric dipolar magnetic field and (right column) for a 15◦ -tilted dipolar magnetic field. The observer is fixed in the sky and located at (first row) 0 ◦ , (second row) 15◦ and (third row) 45◦ from the exoplanet orbital plane. The radio emissions are coloured by their degree of circular polarization: blue (-1) is for Right-Handed (i.e., emissi… view at source ↗

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Works this paper leans on

105 extracted references · 57 canonical work pages · 37 internal anchors

  1. [1]

    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 =

    doi:10.48550/arxiv.2510.23277

  2. [2]

    , keywords =

    Ohmic heating in the upper atmosphere of hot exoplanets: The influence of a time-varying magnetic field. , keywords =. doi:10.1051/0004-6361/202452641 , archivePrefix =. 2412.14072 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202452641

  3. [3]

    Coronal Mass Ejection (CME) Activity of Low Mass M Stars as An Important Factor for The Habitability of Terrestrial Exoplanets. II. CME-Induced Ion Pick Up of Earth-like Exoplanets in Close-In Habitable Zones. Astrobiology , year = 2007, month = feb, volume =. doi:10.1089/ast.2006.0128 , adsurl =

    doi:10.1089/ast.2006.0128 2007

  4. [4]

    Journal of Geophysical Research (Space Physics) , year = 2020, month = aug, volume =

    Atmospheric Escape Processes and Planetary Atmospheric Evolution. Journal of Geophysical Research (Space Physics) , year = 2020, month = aug, volume =. doi:10.1029/2019JA02763910.1002/essoar.10502458.1 , adsurl =

    doi:10.1029/2019ja02763910.1002/essoar.10502458.1 2020

  5. [5]

    , keywords =

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

    doi:10.1086/382274

  6. [6]

    , keywords =

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

    doi:10.1051/0004-6361/201118179

  7. [7]

    , 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 =

    doi:10.1016/j.pss.2006.05.045 2007

  8. [8]

    Planet-induced radio emission from the coronae of M dwarfs: the case of Prox Cen and AU Mic

    Planet-induced radio emission from the coronae of M dwarfs: the case of Prox Cen and AU Mic. , keywords =. doi:10.1093/mnras/stab929 , archivePrefix =. 2103.16318 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab929

  9. [9]

    , keywords =

    Evidence for Planet-induced Chromospheric Activity on HD 179949. , keywords =. doi:10.1086/378583 , adsurl =

    doi:10.1086/378583

  10. [10]

    Nature Astronomy , keywords =

    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 =

    Pith/arXiv arXiv doi:10.1038/s41550-019-0840-x 1907

  11. [11]

    , keywords =

    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 =

    Pith/arXiv arXiv doi:10.3847/1538-3881/aae841

  12. [12]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1086/527351

  13. [13]

    Coordinated X-ray and Optical observations of Star-Planet Interaction in HD 17156

    Coordinated X-Ray and Optical Observations of Star-Planet Interaction in HD 17156. , keywords =. doi:10.1088/2041-8205/811/1/L2 , archivePrefix =. 1509.00662 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/811/1/l2 2041

  14. [14]

    X-ray Activity Variations and Coronal Abundances of the Star-Planet Interaction candidate HD 179949

    X-Ray Activity Variations and Coronal Abundances of the Star-Planet Interaction Candidate HD 179949. , keywords =. doi:10.3847/1538-4357/acd054 , archivePrefix =. 2211.01011 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/acd054

  15. [15]

    FUV variability of HD 189733. Is the star accreting material from its hot Jupiter?

    FUV Variability of HD 189733. Is the Star Accreting Material From Its Hot Jupiter?. , keywords =. doi:10.1088/0004-637X/805/1/52 , archivePrefix =. 1503.05590 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/805/1/52

  16. [16]

    MOST detects variability on tau Bootis possibly induced by its planetary companion

    MOST detects variability on Bootis A possibly induced by its planetary companion. , keywords =. doi:10.1051/0004-6361:20078952 , archivePrefix =. 0802.2732 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20078952

  17. [17]

    CoRoT-2a magnetic activity: hints for possible star-planet interaction

    CoRoT-2a Magnetic Activity: Hints for Possible Star Planet Interaction. Earth Moon and Planets , keywords =. doi:10.1007/s11038-009-9301-3 , archivePrefix =. 0905.3633 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11038-009-9301-3

  18. [18]

    Signs of magnetic star-planet interactions in HD 118203. TESS detects stellar variability that matches the orbital period of a close-in eccentric Jupiter-sized companion

    Signs of magnetic star-planet interactions in HD 118203. TESS detects stellar variability that matches the orbital period of a close-in eccentric Jupiter-sized companion. , keywords =. doi:10.1051/0004-6361/202348722 , archivePrefix =. 2401.17272 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202348722

  19. [19]

    , keywords =

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

    doi:10.1038/s41586-025-09236-z

  20. [20]

    MOVES V. Modelling star-planet magnetic interactions of HD 189733

    MOVES - V. Modelling star-planet magnetic interactions of HD 189733. , keywords =. doi:10.1093/mnras/stac778 , archivePrefix =. 2203.10956 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac778

  21. [21]

    The search for radio emission from the exoplanetary systems 55 Cancri, $\upsilon$ Andromedae, and $\tau$ Bo\"{o}tis using LOFAR beam-formed observations

    The search for radio emission from the exoplanetary systems 55 Cancri, Andromedae, and Bo \"o tis using LOFAR beam-formed observations. , keywords =. doi:10.1051/0004-6361/201937201 , archivePrefix =. 2012.07926 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937201 2012

  22. [22]

    Nature Astronomy , keywords =

    Coherent radio bursts from known M-dwarf planet-host YZ Ceti. Nature Astronomy , keywords =. doi:10.1038/s41550-023-01914-0 , archivePrefix =. 2304.00031 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/s41550-023-01914-0

  23. [23]

    , keywords =

    A circularly polarized low-frequency radio burst from the exoplanetary system HD 189733. , keywords =. doi:10.1051/0004-6361/202555209 , archivePrefix =. 2506.07912 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202555209

  24. [24]

    Coherent radio emission from a quiescent red dwarf indicative of star-planet interaction

    Coherent radio emission from a quiescent red dwarf indicative of star-planet interaction. Nature Astronomy , keywords =. doi:10.1038/s41550-020-1011-9 , archivePrefix =. 2002.08727 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-020-1011-9 2002

  25. [25]

    Monitoring the radio emission of Proxima Centauri

    Monitoring the radio emission of Proxima Centauri. , keywords =. doi:10.1051/0004-6361/202039052 , archivePrefix =. 2012.02116 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039052 2012

  26. [26]

    Hint of 150 MHz radio emission from the Neptune-mass extrasolar transiting planet HAT-P-11b

    Hint of 150 MHz radio emission from the Neptune-mass extrasolar transiting planet HAT-P-11b. , keywords =. doi:10.1051/0004-6361/201219789 , archivePrefix =. 1302.4612 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201219789

  27. [27]

    , keywords =

    Search for 150 MHz radio emission from extrasolar planets in the TIFR GMRT Sky Survey. , keywords =. doi:10.1051/0004-6361/201321571 , adsurl =

    work page doi:10.1051/0004-6361/201321571

  28. [28]

    Radio Signatures of Star-Planet Interactions, Exoplanets, and Space Weather

    Radio signatures of star-planet interactions, exoplanets and space weather. Nature Astronomy , keywords =. doi:10.1038/s41550-024-02405-6 , archivePrefix =. 2409.15507 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-024-02405-6

  29. [29]

    , keywords =

    The electron-cyclotron maser for astrophysical application. , keywords =. doi:10.1007/s00159-006-0001-y , adsurl =

    doi:10.1007/s00159-006-0001-y

  30. [30]

    , keywords =

    Modeling the radio signature of the orbital parameters, rotation, and magnetic field of exoplanets. , keywords =. doi:10.1051/0004-6361/201116510 , adsurl =

    doi:10.1051/0004-6361/201116510

  31. [31]

    Hunting for exoplanets via magnetic star-planet interactions: geometrical considerations for radio emission

    Hunting for exoplanets via magnetic star-planet interactions: geometrical considerations for radio emission. , keywords =. doi:10.1093/mnras/stad2035 , archivePrefix =. 2307.02555 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad2035

  32. [32]

    Inhibition of the electron cyclotron maser instability in the dense magnetosphere of a hot Jupiter

    Inhibition of the electron cyclotron maser instability in the dense magnetosphere of a hot Jupiter. , keywords =. doi:10.1093/mnras/sty1652 , archivePrefix =. 1806.08147 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1652

  33. [33]

    Predicting radio emission from the newborn hot Jupiter V830 Tau and its host star

    Predicting radio emission from the newborn hot Jupiter V830 Tauri b and its host star. , keywords =. doi:10.1051/0004-6361/201629700 , archivePrefix =. 1703.03622 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629700

  34. [34]

    , keywords =

    Stellar coronal magnetic fields and star-planet interaction. , keywords =. doi:10.1051/0004-6361/200912367 , archivePrefix =. 0906.1738 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/200912367

  35. [35]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321790

  36. [36]

    doi:10.25546/103091 , editor =

    Planetary, Solar and Heliospheric Radio Emissions IX , date-added =. doi:10.25546/103091 , editor =

    work page doi:10.25546/103091

  37. [37]

    ExPRES: a Tool to Simulate Exoplanetary and Planetary Radio Emissions

    2019 , bdsk-url-1 =. doi:10.1051/0004-6361/201935161 , eid =. arXiv , author =:1901.11523 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935161 2019

  38. [38]

    , keywords =

    Dynamo Scaling Laws and Applications to the Planets. , keywords =. doi:10.1007/s11214-009-9553-2 , adsurl =

    doi:10.1007/s11214-009-9553-2

  39. [39]

    doi:10.1029/2021JA029435 , eid =

    Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2021JA029435 , eid =

    work page doi:10.1029/2021ja029435

  40. [40]

    The population of M dwarfs observed at low radio frequencies

    The population of M dwarfs observed at low radio frequencies. Nature Astronomy , keywords =. doi:10.1038/s41550-021-01483-0 , archivePrefix =. 2110.03713 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-021-01483-0

  41. [41]

    , keywords =

    The Occurrence of Potentially Habitable Planets Orbiting M Dwarfs Estimated from the Full Kepler Dataset and an Empirical Measurement of the Detection Sensitivity. , keywords =. doi:10.1088/0004-637X/807/1/45 , archivePrefix =. 1501.01623 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/807/1/45

  42. [42]

    , keywords =

    V-LoTSS: The circularly polarised LOFAR Two-metre Sky Survey. , keywords =. doi:10.1051/0004-6361/202245567 , archivePrefix =. 2212.09815 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202245567

  43. [43]

    arXiv e-prints , keywords =

    Spectroscopic Characterization of LOFAR Radio-emitting M dwarfs. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.13783 , archivePrefix =. 2507.13783 , primaryClass =

    work page doi:10.48550/arxiv.2507.13783

  44. [44]

    , keywords =

    On the possibility of coherent cyclotron emission from extrasolar planets. , keywords =. doi:10.1029/1998JE900050 , adsurl =

    work page doi:10.1029/1998je900050

  45. [45]

    , keywords =

    The Radiometric Bode's Law and Extrasolar Planets. , keywords =. doi:10.1086/422449 , adsurl =

    doi:10.1086/422449

  46. [46]

    , keywords =

    Magnetically-Driven Planetary Radio Emissions and Application to Extrasolar Planets. , keywords =. doi:10.1023/A:1012221527425 , adsurl =

    doi:10.1023/a:1012221527425

  47. [47]

    The detectability of radio emission from exoplanets

    The detectability of radio emission from exoplanets. , keywords =. doi:10.1093/mnras/sty1138 , archivePrefix =. 1804.11006 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1138

  48. [48]

    , keywords =

    Exoplanet-induced Radio Emission from M Dwarfs. , keywords =. doi:10.3847/1538-4357/aaa59c , archivePrefix =. 1801.01324 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aaa59c

  49. [49]

    PALANTIR: an updated prediction tool for exoplanetary radio emissions

    PALANTIR: An updated prediction tool for exoplanetary radio emissions. Planetary, Solar and Heliospheric Radio Emissions IX , year = 2023, editor =. doi:10.25546/103092 , archivePrefix =. 2311.10033 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.25546/103092 2023

  50. [50]

    Predicting low-frequency radio fluxes of known extrasolar planets

    Predicting low-frequency radio fluxes of known extrasolar planets. , keywords =. doi:10.1051/0004-6361:20077397 , archivePrefix =. 0806.0327 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20077397

  51. [51]

    , keywords =

    The mass-radius relation of exoplanets revisited. , keywords =. doi:10.1051/0004-6361/202348690 , archivePrefix =. 2311.12593 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202348690

  52. [52]

    , year = 1965, month = sep, volume =

    Dynamical Theory of the Solar Wind. , year = 1965, month = sep, volume =. doi:10.1007/BF00216273 , adsurl =

    doi:10.1007/bf00216273 1965

  53. [53]

    The Coronal Temperatures of Low-Mass Main-Sequence Stars

    The coronal temperatures of low-mass main-sequence stars. , keywords =. doi:10.1051/0004-6361/201425283 , archivePrefix =. 1505.00643 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201425283

  54. [54]

    , keywords =

    Measured Mass-Loss Rates of Solar-like Stars as a Function of Age and Activity. , keywords =. doi:10.1086/340797 , archivePrefix =. astro-ph/0203437 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/340797

  55. [55]

    Source of radio emissions induced by the Galilean moons Io, Europa and Ganymede: in situ measurements by Juno

    doi:10.1029/2023JA031985 , eid =. arXiv , author =:2308.05541 , journal =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1029/2023ja031985

  56. [56]

    doi:10.1029/2008GL033656 , eid =

    Geophysical Research Letters , keywords =. doi:10.1029/2008GL033656 , eid =

    work page doi:10.1029/2008gl033656

  57. [57]

    doi:10.1002/2017GL073036 , journal =

    work page doi:10.1002/2017gl073036

  58. [58]

    doi:10.1016/j.pss.2011.06.012 , journal =

    work page doi:10.1016/j.pss.2011.06.012 2011

  59. [59]

    doi:10.1029/2008JA013464 , eid =

    Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2008JA013464 , eid =

    work page doi:10.1029/2008ja013464

  60. [60]

    doi:10.1002/jgra.50404 , eprint =

    Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1002/jgra.50404 , eprint =

    work page doi:10.1002/jgra.50404

  61. [61]

    Astronomy & Astrophysics , year =

  62. [62]

    arXiv e-prints , keywords =

    How to detect periodic radio emissions from an exoplanet, star, or their interaction?. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.18733 , archivePrefix =. 2503.18733 , primaryClass =

    work page doi:10.48550/arxiv.2503.18733

  63. [63]

    Radio masers on WX UMa: hints of a Neptune-sized planet, or magnetospheric reconnection?

    Radio masers on WX UMa: hints of a Neptune-sized planet, or magnetospheric reconnection?. , keywords =. doi:10.1093/mnras/stac1264 , archivePrefix =. 2205.01661 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac1264

  64. [64]

    Unravelling sub-stellar magnetospheres

    Unravelling sub-stellar magnetospheres. , keywords =. doi:10.1051/0004-6361/202452094 , archivePrefix =. 2410.18073 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202452094

  65. [65]

    , keywords =

    An all-sky survey of circular polarization at 200 MHz. , keywords =. doi:10.1093/mnras/sty1304 , archivePrefix =. 1805.05482 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty1304

  66. [66]

    Deep radio interferometric search for decametre radio emission from the exoplanet Tau Bo\"otis b

    Deep radio interferometric search for decametre radio emission from the exoplanet Tau Bo \"o tis b. , keywords =. doi:10.1051/0004-6361/202452868 , archivePrefix =. 2501.06301 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202452868

  67. [67]

    Limits on low frequency radio emission from southern exoplanets with the Murchison Widefield Array

    Limits on low-frequency radio emission from southern exoplanets with the Murchison Widefield Array. , keywords =. doi:10.1093/mnras/stu2253 , archivePrefix =. 1410.6819 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu2253

  68. [68]

    A search for circularly polarised emission from young exoplanets

    A search for circularly polarized emission from young exoplanets. , keywords =. doi:10.1093/mnras/stx354 , archivePrefix =. 1702.01826 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx354

  69. [69]

    A Blind Search for Magnetospheric Emissions from Planetary Companions to Nearby Solar-type Stars

    A Blind Search for Magnetospheric Emissions from Planetary Companions to Nearby Solar-Type Stars. , keywords =. doi:10.1088/0004-6256/139/1/96 , archivePrefix =. 0910.3938 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/139/1/96

  70. [70]

    , keywords =

    Looking for a Pulse: A Search for Rotationally Modulated Radio Emission from the Hot Jupiter, Bo \"o tis b. , keywords =. doi:10.1088/0004-637X/762/1/34 , archivePrefix =. 1210.8259 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/762/1/34

  71. [71]

    , keywords =

    A Search for Radio Emission from Extrasolar Planets. , keywords =. doi:10.1086/317864 , adsurl =

    doi:10.1086/317864

  72. [72]

    ROME. III. The Arecibo Search for Star-Planet Interactions at 5 GHz. , keywords =. doi:10.3847/1538-4357/acd9ad , archivePrefix =. 2202.08899 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/acd9ad

  73. [73]

    Phenomenology and periodicity of radio emission from the stellar system AU Microscopii

    Phenomenology and periodicity of radio emission from the stellar system AU Microscopii. , keywords =. doi:10.1051/0004-6361/202348065 , archivePrefix =. 2312.09071 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202348065

  74. [74]

    One year of AU Mic with HARPS: II -- 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 internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac761

  75. [75]

    , keywords =

    Large-scale magnetic topologies of late M dwarfs*. , keywords =. doi:10.1111/j.1365-2966.2010.17101.x , archivePrefix =. 1005.5552 , primaryClass =

    doi:10.1111/j.1365-2966.2010.17101.x 2010

  76. [76]

    , keywords =

    SPIRou reveals unusually strong magnetic fields of slowly rotating M dwarfs. , keywords =. doi:10.1093/mnras/stad3472 , archivePrefix =. 2311.05039 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stad3472

  77. [77]

    New Observational Constraints on the Winds of M Dwarf Stars

    New Observational Constraints on the Winds of M dwarf Stars. , keywords =. doi:10.3847/1538-4357/abfda5 , archivePrefix =. 2105.00019 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/abfda5

  78. [78]

    X-ray detection of astrospheres around three main-sequence stars and their mass-loss rates

    X-ray detection of astrospheres around three main-sequence stars and their mass-loss rates. Nature Astronomy , keywords =. doi:10.1038/s41550-024-02222-x , archivePrefix =. 2404.14980 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-024-02222-x

  79. [79]

    I: Methods of Calculating Coronal Fields

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

    doi:10.1007/bf00145734

  80. [80]

    Journal of Geomagnetism and Geoelectricity , year = 1993, month = jan, volume =

    The Magnetic Fields of the Planets: A New Scaling Law of the Dipole Moments of the Planetary Magnetism. Journal of Geomagnetism and Geoelectricity , year = 1993, month = jan, volume =. doi:10.5636/jgg.45.65 , adsurl =

    work page doi:10.5636/jgg.45.65 1993

Showing first 80 references.