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REVIEW 3 major objections 6 minor 123 references

A tidally heated rocky planet the size of Jupiter's moon Io can supply the 10^5 kg/s plasma flow that powers the radio bursts of ultracool dwarf LSR J1835+3259.

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2026-08-01 00:58 UTC pith:WI3O7L7C

load-bearing objection Transparent feasibility study making the volcanic-exomoon plasma source for LSR J1835+3259 testable, but the case rests on a single, unobserved outer-planet architecture. the 3 major comments →

arxiv 2607.25964 v1 pith:WI3O7L7C submitted 2026-07-28 astro-ph.EP

Volcanic Satellites and Ion Escape in the Magnetospheres of Ultra-Cool and Brown Dwarf Stars

A. F. Lanza (INAF-Catania , Italy) , A. V. Oza (Caltech , JPL , California , USA) This is my paper
classification astro-ph.EP
keywords ultra-cool dwarfsbrown dwarfselectron-cyclotron maser emissionexomoonstidal heatingmagnetospheric plasmaLSR J1835+3259stellar ionospheric outflow
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.

The paper asks where the plasma in the magnetosphere of the ultracool dwarf LSR J1835+3259 comes from. Its radio bursts, of the electron-cyclotron maser type, require a mass flow of roughly 10^5 kg/s across the stellar magnetosphere. The authors test three sources: a weak outflow from the star's own ionosphere, a tidally heated volcanic planet like Io, and electromagnetic induction heating. They find the ionospheric outflow can work only if the star's effective Pedersen conductance is below about 0.02 mho, a tight constraint; induction heating is too weak. The claim that survives is that an unseen Io-like planet, orbiting within 6-14 stellar radii with an eccentricity of about 10^-3 kept alive by an outer companion, can volcanically supply the required plasma. If true, the radio bursts of ultracool dwarfs become indirect evidence for exomoons or small planets around these stars.

Core claim

On the paper's own terms, the central claim is that a rocky planet with the radius and mass of Io, heated internally by tidal dissipation, is a suitable source of the ~10^5 kg/s magnetospheric mass flux inferred from LSR J1835+3259's electron-cyclotron maser emission, provided its orbit lies within roughly 6-14 stellar radii and its small eccentricity (~10^-3) is continuously forced by an outer planet. The same analysis shows the alternative stellar ionospheric outflow works only if the effective Pedersen conductance is below ~0.02 mho; for an open magnetosphere the allowed conductance is higher but the required flux is smaller. Induction heating by the star's magnetic field cannot reach the

What carries the argument

The load-bearing object is an Io-twin: a small rocky planet with Io's radius and mass whose volcanic outgassing is proportional to tidal dissipation. The argument is carried by three coupled pieces: the tidal heating law, which scales as e^2 a^-15/2 divided by the modified tidal quality factor; an equilibrium-eccentricity mechanism in which a coplanar, non-resonant outer planet keeps the inner planet's eccentricity near 10^-3 for Gyr timescales; and an upper-limit mass-flux formula that ties the plasma density near the planet, the magnetospheric convection speed, and the centrifugal scale height to the observed radio flux. The volcanic source wins because it can deliver 10^5-10^6 kg/s withou

Load-bearing premise

The volcanic-satellite scenario stands on the unobserved outer planet that must keep the inner planet's eccentricity near 10^-3 for gigayears; without that perturber, tidal circularization quenches the heating in roughly 7,800 years.

What would settle it

Continuous photometric monitoring of LSR J1835+3259 looking for the predicted 500-600 ppm transit with period 5.5-12 hours; if many periods pass with no transit and no transit-timing wobble from the outer companion, the volcanic-planet source for the closed-magnetosphere case is ruled out.

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

If this is right

  • If the Io-twin scenario holds, LSR J1835+3259 should host a transiting or non-transiting planet with orbital period roughly 5.5-12 hours; the predicted transit depth is 500-600 ppm for an Io-radius body.
  • The inner planet's eccentricity cannot survive on its own: tidal circularization would erase it in about 7,800 years, so the scenario implies a second, outer planet with the properties needed to force e ~ 10^-3.
  • The same magnetospheric mass flux could be supplied by an ionospheric outflow only if the star's Pedersen conductance is below about 0.02 mho; a measurement above that value rules out the stellar wind as the source.
  • The volcanic-planet scenario is consistent with the statistical result that ultracool dwarfs with distant stellar or substellar companions are more often detected in radio; the distant companion can drive the eccentricity of the outer planet, which in turn keeps the inner planet's orbit eccentric.
  • Induction heating by the star's rotating magnetic field delivers at most about Io's heat flux for a planet orbiting within 10 stellar radii, so it cannot power the required mass loss on its own.

Where Pith is reading between the lines

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

  • A direct test follows from timing: if the plasma source is a single Io-like planet, the ECM burst periodicity should match the planet's orbital period; compiling burst times over many rotations could reveal that periodicity and distinguish the planet-source from an ionospheric wind.
  • The equilibrium-eccentricity requirement implies a specific architecture (inner planet at a, outer companion near 3.5a with ~0.4 Earth masses, e~0.5). A transit-timing search for such an outer companion is a concrete way to falsify or confirm the hypothesis.
  • The same scaling could be applied to other radio-emitting ultracool dwarfs and brown dwarfs: targets with stronger ECM flux require either a larger volcanic planet or a closer orbit, so a statistical comparison of radio luminosity with predicted transit depth could map the occurrence rate of Io-like planets.
  • The paper's parameter choices for the unseen outer planet are not independently constrained; exploring the full range of mass and semimajor axis would show how fine-tuned the volcanic scenario really is.

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

3 major / 6 minor

Summary. The paper addresses the plasma source that powers the observed electron-cyclotron maser (ECM) radio emission from the ultra-cool dwarf LSR J1835+3259. Using two published frameworks — ionospheric-magnetospheric coupling (Turnpenney et al. 2017) and Alfvén-wing star-planet interaction (Noyola et al. 2014) — the authors convert the observed 8.4 GHz bursty flux into an order-of-magnitude required mass flux through the stellar magnetosphere: ~10^5 kg/s for a closed magnetosphere, ~10^3 kg/s for an open magnetosphere, and 0.05×10^4–1.8×10^7 kg/s for Alfvén-wing scenarios depending on the effective Pedersen conductance. They then derive theoretical mass supply rates from a stellar ionospheric outflow (Appendix A), a tidally heated Io-like planet whose eccentricity is forced by an unseen outer planet (Sect. 3.4), and induction heating (Sect. 3.5). The main conclusions are that the ionospheric outflow can supply the closed-magnetosphere requirement only if the Pedersen conductance is below ~0.02 mho, while tidal heating of an Io-like planet at 6–14 stellar radii can supply 10^5 kg/s provided an outer perturber maintains e ~ 10^-3. The paper further suggests that the observed enhancement of radio emission in ultra-cool dwarfs with distant companions could be understood through Kozai–Lidov excitation of the outer planet, and it proposes transit and Doppler observability of the inner planet.

Significance. If correct, the paper offers a concrete and testable answer to the long-standing question of what feeds the radiation belts around ultra-cool dwarfs: either a stellar ionospheric outflow or a volcanically active Io-analog. The main strengths are transparency and falsifiability. The estimates are built on published equations (Hill et al. 1981; Neubauer 1980; Turnpenney et al. 2017; Mardling 2007), all parameter choices are explicitly listed, and Table 2 summarizes the comparison between required and predicted mass fluxes. The predictions — a ~500–600 ppm transit of the inner planet with a 5.5–12 h period, an SO2 torus, and Doppler-shifted sodium — are testable with current or near-term facilities. The paper also makes good use of recent measurements, including Q'_Io ~ 100 and the resolved magnetosphere of LSR J1835+3259. However, the central volcanic-planet scenario rests on an unseen, hand-picked outer planet and on a linear tidal-power-to-mass-loss scaling, and the dynamical survival of the architecture is asserted rather than demonstrated. The ionospheric-outflow claim also contains an internal inconsistency regarding open versus closed field lines. These issues do not invalidate

major comments (3)
  1. [§3.3, Table 2, Appendix A] The ionospheric outflow model is constructed for open magnetic field lines: Eq. (A.9) contains f_w, the fraction of the surface covered by open field lines, and the text adopts f_w = 0.15 from solar coronal holes. However, Table 2 and the Conclusions apply this source to the 'M-I model, closed magnetosphere' case, where the required mass flux is 10^5 kg/s, and claim viability if Sigma_p* <~ 0.02 mho. In a closed magnetosphere there are no open field lines, so f_w should vanish and the outflow cannot be launched. The only self-consistent application is to the open-magnetosphere row, where the required mass flux is 10^3 kg/s and the outflow is viable for Sigma_p* <~ 2 mho. Please either remove the closed-magnetosphere entry or extend the model to a closed-field interchange-driven outflow and recompute the effective f_w.
  2. [§3.4, Eq. (12), Fig. 2] The volcanic-planet scenario relies on a specific unseen outer perturber (m_c = 0.4 M_Earth, a_c = 3.5a, e_c = 0.5) to maintain the inner eccentricity, and the paper explicitly declines to explore the parameter space, stating that such exploration 'would not change our conclusion' without justification. More importantly, the outer planet's own eccentricity must be maintained. Using the paper's own Eq. (12) with Q'_m = 100 and a radius appropriate for a 0.4 M_Earth rocky body gives an e-folding time for e_c of order ~10 Myr, comparable to the 22 ± 4 Myr system age. The claim in Fig. 2 (bottom) that the decay time is longer than the Hubble time is therefore not transparent and depends on the outer planet's radius and tidal quality factor, which are not stated. If e_c decays, the forced inner eccentricity and hence P_tide drop, potentially below the 10^5 kg/s threshold. Please provide the o
  3. [§2.4.1 and §3.4, Eq. (11)] The conversion from tidal power to mass-loss rate assumes a linear scaling with P_tide, normalized to Io's 10^3 kg/s. The paper does not model the volcanic-atmosphere-sputtering chain that connects tidal heating to the neutral/ion escape that eventually populates the magnetosphere; it simply asserts proportionality. Because the tidal-heating scenario meets the 10^5 kg/s requirement only by a modest margin at a ~ 13 R_s (top panel of Fig. 2), an efficiency factor of only ~3 below the assumed value would shrink the allowed semimajor-axis range below ~10 R_s and could alter the comparison in Table 2 for the Alfvén-wing rows. A sensitivity analysis over the normalization and the scaling exponent is needed to make the central feasibility claim robust.
minor comments (6)
  1. [Abstract and §5] The abstract states the threshold as 'semimajor axis lower than about 10 stellar radii', while the conclusions state '6–14 stellar radii' and §3.4 states '~13 R_s'. Please harmonize these numbers and specify the exact criterion (10^5 kg/s) used.
  2. [Table 2] The 'YES/NO' entries lack an explicit comparison rule. State whether a theoretical model is considered viable when its mass-flux range overlaps the required range, and whether the Alfvén-wing rows use the same S = 2500 μJy burst flux as the M-I rows.
  3. [§2.2 and Fig. 1] The symbol '3' used for velocity in Eq. (7) and Eq. (8) is unconventional and easily mistaken for a numeric factor; use a bold 'v' or an arrow notation, and define it explicitly.
  4. [Appendix D] The text first adopts Q'_p = 10^12 as the optimistic upper bound and then states that Oza et al. (2019) reassessed values 'may be as large as 10^11'. Please reconcile these numbers.
  5. [Fig. 2 caption] The bottom-panel caption says it shows the decay timescale 'of the equilibrium eccentricity of the inner planet and of the eccentricity of the outer planet', but the text only describes the inner equilibrium timescale. Specify which curves correspond to which body and which Q' values were used.
  6. [§4] The claim that the apsidal precession period of the inner planet is 'a few tens or hundreds of years' is not derived; please show the formula and numerical values used, since this argument is the basis for rejecting direct Kozai–Lidov forcing of the inner planet.

Circularity Check

0 steps flagged

No significant circularity: the required magnetospheric mass flux is derived from observed radio emission and compared with independently computed source rates from tidal heating and ionospheric outflow.

full rationale

The paper's central derivation is not circular. The required magnetospheric mass flux (~1e5 kg/s) is estimated from the observed ECM flux using two external models (Turnpenney et al. 2017 for ionospheric-magnetospheric coupling; Noyola et al. 2014 for Alfvén-wing star-planet interaction) and the Hill transport prescription. The theoretical source rates are then computed independently: the ionospheric outflow rate uses the X-ray luminosity upper limit and stellar parameters in Eq. (A.9); the volcanic-planet rate uses Eq. (10) with Io-like parameters (R_m, M_m, Q'_m=100), an equilibrium eccentricity from Mardling (2007), and the observed Io mass-loss rate (~1e3 kg/s) as a calibration anchor. No parameter is fitted to the ECM flux to force agreement; the comparison in Table 2 yields constraints (a ≲ 6–14 R_s; Σ*_p ≲ 0.02 mho) rather than fitted predictions. Self-citations (Gebek & Oza 2020; Oza et al. 2019, 2024, 2026) support plausibility and scaling but the numerical anchor is Io's observed rate and standard tidal physics, so they are not load-bearing. The main weaknesses—unexplored two-planet parameter space (Sect. 3.4) and unquantified Kozai pumping of the outer planet's eccentricity (Sect. 4)—are unproven dynamical assumptions, which are limitations or correctness risks, not circular reductions of the derivation to its inputs.

Axiom & Free-Parameter Ledger

6 free parameters · 6 axioms · 2 invented entities

The paper's central comparison rests on a chain of adopted parameters, most of which are taken from Jupiter-Io scaling, solar coronal-hole statistics, or a hand-picked two-planet architecture. The most consequential ad hoc choice is the unseen outer planet, without which the volcanic scenario fails within ~10^4 years.

free parameters (6)
  • Outer perturbing planet parameters = m_c = 0.4 M_Earth, a_c = 3.5a, e_c = 0.5
    Chosen by hand to maintain the inner planet's equilibrium eccentricity e ~ 1e-3; no observational evidence or stability constraint is provided.
  • Effective Pedersen conductance Sigma*_p = 0.01-10 mho (scan)
    Unknown for UCDs; all viability thresholds are quoted against this range. The ionospheric-outflow route requires Sigma*_p <~ 0.02 mho.
  • Modified tidal quality factor Q'_m = 100
    Taken from Io (Lainey et al. 2009; Park et al. 2024) and applied to the putative exoplanet; drives the tidal power and eccentricity decay timescale.
  • Open-field fraction f_w = 0.15
    Mean fractional area of solar coronal holes adopted for the ionospheric outflow model in Eq. (A.9).
  • Coronal temperature T_cor = 1.5 MK
    Assumed to convert the X-ray upper limit into a coronal base density via Eq. (A.1).
  • Alfvén-wing efficiency and beaming angle = beta_S = 0.01, Omega = 0.15 sr
    Taken from Jupiter-Io radio scaling and used in Eq. (4) to convert flux to plasma density.
axioms (6)
  • domain assumption Stellar magnetic field is a dipole scaling as B_m = B_p (R_s/r)^3, with B_p inferred from ECM frequency via nu_ECM = 2.8 B.
    Used throughout to evaluate B_m at the planet and in the emission region; supported by the resolved quiescent morphology but not uniquely determined.
  • domain assumption The observed ECM emission is powered entirely by either magnetospheric-ionospheric coupling or by a single planet's Alfvén wings, and the full observed flux S = 2500 microJy is attributed to that single mechanism.
    The authors explicitly consider each mechanism alone; the physical attribution is not observationally settled.
  • standard math Hill et al. (1981) corotating-convection model describes the magnetospheric plasma transport and provides upper-limit convective velocities.
    Equations (3), (7)-(9) are standard magnetospheric results adopted without derivation.
  • domain assumption Io-like volcanic processes (SO2 sputtering, electron-impact ionization) imply Mdot proportional to P_tide, calibrated to Io's average mass-loss rate of about 10^3 kg/s.
    Sect. 2.4.1 builds the volcanic mass-loss estimate on the Jupiter-Io analogy, including a linear scaling to P_tide.
  • domain assumption Mardling (2007) two-planet secular model maintains an equilibrium inner eccentricity e ~ 1e-3 for Gyr.
    Sect. 2.4.2 and Fig. 2 rely on this model; the required outer planet is not observed.
  • domain assumption The stellar ionospheric outflow is isothermal, field-aligned, and starts from an X-ray-derived base density.
    Appendix A: momentum equation (A.2), isothermal sound speed (A.4), and density profile (A.6) assume this specific outflow geometry.
invented entities (2)
  • Inner Io-like volcanically active planet or moon around LSR J1835+3259 no independent evidence
    purpose: Supplies the ~10^5 kg/s magnetospheric plasma mass flow via tidal heating
    Hypothetical; not detected. The paper gives transit-depth and Doppler signatures that could test it.
  • Outer perturbing planet (m_c = 0.4 M_Earth, a_c = 3.5a, e_c = 0.5) no independent evidence
    purpose: Maintains the inner planet's eccentricity at e ~ 1e-3 against tidal damping
    Introduced to make the volcanic scenario work; no transit, radial-velocity, or timing detection is available or modeled.

pith-pipeline@v1.3.0-alltime-deepseek · 29599 in / 14777 out tokens · 142349 ms · 2026-08-01T00:58:36.969839+00:00 · methodology

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read the original abstract

Radio emissions at $\sim$ GHz frequencies of ultra-cool dwarf and brown dwarf stars suggest the presence of radiation belts not unlike Jupiter's. We investigate the possibility the inferred magnetospheric plasma at the primary star is sourced by an active planet or via ion escape modeled as a weak ionospheric outflow. We consider indirect methods to estimate the magnetospheric plasma mass flow from auroral radio emission and apply them to the ultra-cool dwarf LSR J1835+3259. We find that an ionospheric outflow is a viable source of the order of $10^{5}$ kg s$^{-1}$, if the ionospheric effective Pedersen conductance is lower than $\sim 0.02$ mho. On the other hand, a tidally-heated volcanic satellite with the same mass and radius as Io and an orbit with a semimajor axis lower than about $10$ stellar radii, whose eccentricity ($e \sim 10^{-3}$) is maintained by perturbations by other planets in the system, is found to be a viable source of magnetospheric plasma without strong limitations on the ionospheric conductance. The volcanic satellite scenario is also naturally in sync with the recent finding that ultra-cool dwarfs with distant substellar or stellar companions are remarkably more likely to be detected as radio emitters.

Figures

Figures reproduced from arXiv: 2607.25964 by A. F. Lanza (INAF-Catania, A. V. Oza (Caltech, California, Italy), JPL, USA).

Figure 1
Figure 1. Figure 1: Upper limit to the mass flux M˙ SPI across the magnetosphere of LSR J1835+3259 vs. the orbital radius of a planet with the radius of Io as estimated by means of Eq. (8) assuming the star-planet interac￾tion and magnetospheric convection model in Sect. 2.2 and an observed auroral radio flux S = 2500 µJy. Different line colours and linestyle re￾fer to different values of the effective Pedersen conductance: Σ… view at source ↗
Figure 2
Figure 2. Figure 2: Top panel: The ratio of the tidal power dissipated in the putative inner planet to the tidal power dissipated inside Io (on the left axis) and mass loss rate (on the right axis) vs. the orbit semimajor axis of the planet; middle panel: equilibrium eccentricity of the orbit of the inner planet vs. the semimajor axis of its orbit; bottom panel: timescale for the decay of the equilibrium eccentricity of the i… view at source ↗
Figure 3
Figure 3. Figure 3: Schematic maps of the microwave emission assuming different plasma sources for the magnetospheric environment of LSR J1835+3259 modeled over a 80 × 80 RJ field of view. Six radio flux maps are simulated at 8.4 GHz following the six plasma source processes presented as toy models in Section 2 and applied in Section 3. (1) Auroral Oval, (2) Satellite Footprints, (3) Volcanic Planet, (4) Volcanic Satellite, (… view at source ↗

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Reference graph

Works this paper leans on

123 extracted references · 28 canonical work pages · 3 internal anchors

  1. [1]

    Nature , year = 2026, month = jul, volume =

    Planetary-mass exosatellite detected around the substellar companion of a star. Nature , year = 2026, month = jul, volume =

    2026

  2. [2]

    McGrath, M. A. and Johnson, R. E. , title =. J. Geophys. Res. , volume =

  3. [3]

    Johnson, R. E. , title =

  4. [4]

    McGrath, M. A. and Johnson, R. E. , title =. Icarus , volume =

  5. [5]

    arXiv e-prints , keywords =

    On the Detectability of Volcanic Exo-Ios That May Fuel Auroras on Super-Jupiters. arXiv e-prints , keywords =

  6. [6]

    Journal of Geophysical Research (Space Physics) , keywords =

    Parallel Electron Beams at Io: Numerical Simulations of the Dense Plasma Wake. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2023JA031763 , adsurl =

    work page doi:10.1029/2023ja031763

  7. [7]

    Io: A New View of Jupiter's Moon , year = 2023, editor =

    Space Environment of Io. Io: A New View of Jupiter's Moon , year = 2023, editor =. doi:10.1007/978-3-031-25670-7_9 , adsurl =

    work page doi:10.1007/978-3-031-25670-7_9 2023

  8. [8]

    , keywords =

    Three-dimensional plasma simulation of Io's interaction with the Io plasma torus: Asymmetric plasma flow. , keywords =. doi:10.1029/1999JA900304 , adsurl =

    work page doi:10.1029/1999ja900304

  9. [9]

    , keywords =

    Volcanic satellites tidally venting Na, K, and SO _ 2 in optical and infrared light. , keywords =. doi:10.1093/mnras/staf1526 , archivePrefix =. 2509.08349 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    Annales Geophysicae , year = 2004, month = may, volume =

    Magnetosphere-ionosphere coupling currents in Jupiter's middle magnetosphere: effect of precipitation-induced enhancement of the ionospheric Pedersen conductivity. Annales Geophysicae , year = 2004, month = may, volume =. doi:10.5194/angeo-22-1799-2004 , adsurl =

    work page doi:10.5194/angeo-22-1799-2004 2004

  11. [11]

    , keywords =

    Confirmation of the Electron Cyclotron Maser Instability as the Dominant Source of Radio Emission from Very Low Mass Stars and Brown Dwarfs. , keywords =. doi:10.1086/590360 , archivePrefix =. 0805.4010 , primaryClass =

    Pith/arXiv arXiv

  12. [12]

    Simultaneous Multiwavelength Observations of Magnetic Activity in Ultracool Dwarfs. I. The Complex Behavior of the M8.5 Dwarf TVLM 513-46546. , keywords =. doi:10.1086/524769 , archivePrefix =. 0708.1511 , primaryClass =

    Pith/arXiv arXiv

  13. [13]

    , keywords =

    Modelling the environment around five ultracool dwarfs via the radio domain. , keywords =. doi:10.1093/mnras/stw2597 , archivePrefix =. 1610.02989 , primaryClass =

    Pith/arXiv arXiv

  14. [14]

    , keywords =

    A survey of the plasma electron environment of Jupiter: a view from voyager. , keywords =. doi:10.1029/JA086iA10p08157 , adsurl =

    work page doi:10.1029/ja086ia10p08157

  15. [15]

    , keywords =

    Magnetosphere-ionosphere coupling at Jupiter-like exoplanets with internal plasma sources: implications for detectability of auroral radio emissions. , keywords =. doi:10.1111/j.1365-2966.2011.18528.x , archivePrefix =. 1102.2737 , primaryClass =

    arXiv 2011

  16. [16]

    , keywords =

    Electron-cyclotron masers as the source of certain solar and stellar radio bursts. , keywords =. doi:10.1086/160219 , adsurl =

    doi:10.1086/160219

  17. [17]

    , keywords =

    Direct Radio Discovery of a Cold Brown Dwarf. , keywords =. doi:10.3847/2041-8213/abc256 , archivePrefix =. 2010.01915 , primaryClass =

    Pith/arXiv arXiv 2041

  18. [18]

    , keywords =

    Polarised radio pulsations from a new T-dwarf binary. , keywords =. doi:10.1051/0004-6361/202244965 , archivePrefix =. 2301.01003 , primaryClass =

    Pith/arXiv arXiv

  19. [19]

    , keywords =

    Radio maps of Jupiter's radiation belts and planetary disk at lambda 6 CM. , keywords =

  20. [20]

    , keywords =

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

    doi:10.1029/98je01323

  21. [21]

    Nature Astronomy , keywords =

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

    Pith/arXiv arXiv

  22. [22]

    Experimental Astronomy , keywords =

    The CHEOPS mission. Experimental Astronomy , keywords =. doi:10.1007/s10686-020-09679-4 , archivePrefix =. 2009.11633 , primaryClass =

    Pith/arXiv arXiv 2009

  23. [23]

    , keywords =

    Temperate Earth-sized planets transiting a nearby ultracool dwarf star. , keywords =. doi:10.1038/nature17448 , archivePrefix =. 1605.07211 , primaryClass =

    Pith/arXiv arXiv

  24. [24]

    The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations. , keywords =. doi:10.3847/1538-4357/aab158 , archivePrefix =. 1802.07319 , primaryClass =

    Pith/arXiv arXiv

  25. [25]

    , keywords =

    Constraining Ongoing Volcanic Outgassing Rates and Interior Compositions of Extrasolar Planets with Mass Measurements of Plasma Tori. , keywords =. doi:10.3847/2041-8213/adde5e , archivePrefix =. 2506.08177 , primaryClass =

    Pith/arXiv arXiv 2041

  26. [26]

    Journal of Geophysical Research (Space Physics) , keywords =

    The Space Environment of Io and Europa. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2019JA027485 , adsurl =

    doi:10.1029/2019ja027485

  27. [27]

    Scientific Reports , year = 2014, month = jul, volume =

    Electrical conductivity of ice VII. Scientific Reports , year = 2014, month = jul, volume =. doi:10.1038/srep05778 , adsurl =

    work page doi:10.1038/srep05778 2014

  28. [28]

    , keywords =

    Binarity enhances the occurrence rate of radiation belt emissions in ultracool dwarfs. , keywords =. doi:10.1093/mnras/stae905 , archivePrefix =. 2403.08860 , primaryClass =

    Pith/arXiv arXiv

  29. [29]

    , keywords =

    Extreme exomoons in WASP-49 Ab: Dynamics and detectability. , keywords =. doi:10.1051/0004-6361/202452968 , archivePrefix =. 2501.05866 , primaryClass =

    Pith/arXiv arXiv

  30. [30]

    , keywords =

    Nonlinear standing Alfv \'e n wave current system at Io: Theory. , keywords =. doi:10.1029/JA085iA03p01171 , adsurl =

    doi:10.1029/ja085ia03p01171

  31. [31]

    , year = 2000, month = jan, volume =

    Variations of solar coronal hole area and terrestrial lower tropospheric air temperature from 1979 to mid-1998: astronomical forcings of change in earth's climate?. , year = 2000, month = jan, volume =. doi:10.1016/S1384-1076(00)00002-6 , adsurl =

    work page doi:10.1016/s1384-1076(00)00002-6 1979

  32. [32]

    , keywords =

    Brown dwarfs as ideal candidates for detecting UV aurora outside the Solar System: Hubble Space Telescope observations of 2MASS J1237+6526. , keywords =. doi:10.1051/0004-6361/202040230 , archivePrefix =. 2109.00827 , primaryClass =

    Pith/arXiv arXiv

  33. [33]

    , keywords =

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

    doi:10.1029/97je03370

  34. [34]

    , keywords =

    On the Relation between Hot Jupiters and the Roche Limit. , keywords =. doi:10.1086/500734 , archivePrefix =. astro-ph/0512632 , primaryClass =

    Pith/arXiv arXiv

  35. [35]

    Journal of Geophysical Research (Space Physics) , keywords =

    Jupiter's low-frequency radio spectrum from Cassini/Radio and Plasma Wave Science (RPWS) absolute flux density measurements. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2003JA010260 , adsurl =

    doi:10.1029/2003ja010260

  36. [36]

    , year = 2001, month = mar, volume =

    Flux, power, energy and polarization of Jovian S-bursts. , year = 2001, month = mar, volume =. doi:10.1016/S0032-0633(00)00157-4 , adsurl =

    doi:10.1016/s0032-0633(00)00157-4 2001

  37. [37]

    , 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

  38. [38]

    , keywords =

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

    doi:10.1023/a:1012221527425

  39. [39]

    , keywords =

    Fine Structures of Radio Bursts from Flare Star AD Leo with FAST Observations. , keywords =. doi:10.3847/1538-4357/acdb77 , archivePrefix =. 2306.00895 , primaryClass =

    Pith/arXiv arXiv

  40. [40]

    , year = 2007, month = jan, volume =

    Io Jupiter interaction, millisecond bursts and field-aligned potentials. , year = 2007, month = jan, volume =. doi:10.1016/j.pss.2006.05.016 , adsurl =

    work page doi:10.1016/j.pss.2006.05.016 2007

  41. [41]

    , keywords =

    Comparative Analysis of Two Formation Scenarios of Bursty Radio Emission from Ultracool Dwarfs. , keywords =. doi:10.1088/0004-637X/746/1/99 , archivePrefix =. 1111.7019 , primaryClass =

    Pith/arXiv arXiv

  42. [42]

    Hint of star exoplanet interaction?

    Probing the magnetosphere of the M8.5 dwarf TVLM 513-46546 by modelling its auroral radio emission. Hint of star exoplanet interaction?. , keywords =. doi:10.1093/mnras/stx995 , archivePrefix =. 1611.00511 , primaryClass =

    Pith/arXiv arXiv

  43. [43]

    , keywords =

    The Jovian auroral oval. , keywords =. doi:10.1029/2000JA000302 , adsurl =

    doi:10.1029/2000ja000302

  44. [44]

    , keywords =

    On a Transition from Solar-Like Coronae to Rotation-Dominated Jovian-Like Magnetospheres in Ultracool Main-Sequence Stars. , keywords =. doi:10.1088/0004-637X/699/2/L148 , archivePrefix =. 0905.1354 , primaryClass =

    Pith/arXiv arXiv

  45. [45]

    Simultaneous Multiwavelength Observations of Magnetic Activity in Ultracool Dwarfs. II. Mixed Trends in VB 10 and LSR 1835+32 and the Possible Role of Rotation. , keywords =. doi:10.1086/529131 , archivePrefix =. 0710.3383 , primaryClass =

    Pith/arXiv arXiv

  46. [46]

    , keywords =

    Auroral radio emission from ultracool dwarfs: a Jovian model. , keywords =. doi:10.1093/mnras/stx1508 , archivePrefix =. 1706.04679 , primaryClass =

    Pith/arXiv arXiv

  47. [47]

    , keywords =

    Magnetically Controlled Outflows from Hot Jupiters. , keywords =. doi:10.1088/0004-637X/730/1/27 , archivePrefix =. 1101.4234 , primaryClass =

    Pith/arXiv arXiv

  48. [48]

    Living Reviews in Solar Physics , keywords =

    The evolution of the solar wind. Living Reviews in Solar Physics , keywords =. doi:10.1007/s41116-021-00029-w , archivePrefix =. 2103.15748 , primaryClass =

    Pith/arXiv arXiv

  49. [49]

    Notes on the Dipole Coordinate System

    Notes on the Dipole Coordinate System. arXiv e-prints , keywords =. doi:10.48550/arXiv.physics/0606044 , archivePrefix =. physics/0606044 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.physics/0606044

  50. [50]

    , keywords =

    Corotating magnetospheric convection. , keywords =. doi:10.1029/JA086iA11p09020 , adsurl =

    work page doi:10.1029/ja086ia11p09020

  51. [51]

    , keywords =

    Centrifugally driven diffusion of Iogenic plasma. , keywords =. doi:10.1029/JA086iA10p08471 , adsurl =

    work page doi:10.1029/ja086ia10p08471

  52. [52]

    , keywords =

    New Mass-Loss Measurements from Astrospheric Ly Absorption. , keywords =. doi:10.1086/432716 , archivePrefix =. astro-ph/0506401 , primaryClass =

    Pith/arXiv arXiv

  53. [53]

    Frontiers in Astronomy and Space Sciences , keywords =

    Doppler-Shifted Alkali D Absorption as Indirect Evidence for Exomoons. Frontiers in Astronomy and Space Sciences , keywords =. doi:10.3389/fspas.2022.801873 , archivePrefix =. 2202.13815 , primaryClass =

    arXiv 2022

  54. [54]

    , keywords =

    Sputter ejection of matter from Io. , keywords =. doi:10.1029/JA086iA08p06933 , adsurl =

    work page doi:10.1029/ja086ia08p06933

  55. [55]

    , keywords =

    The Magnetospheric Plasma-driven Evolution of Satellite Atmospheres. , keywords =. doi:10.1086/422912 , adsurl =

    work page doi:10.1086/422912

  56. [56]

    , keywords =

    Turbulent Viscosity and Jupiter's Tidal Q. , keywords =. doi:10.1016/0019-1035(77)90163-4 , adsurl =

    doi:10.1016/0019-1035(77)90163-4

  57. [57]

    Origin of Tidal Dissipation in Jupiter. II. The Value of Q. , keywords =. doi:10.1086/497355 , archivePrefix =. astro-ph/0407628 , primaryClass =

    Pith/arXiv arXiv

  58. [58]

    , keywords =

    First Detection of a Strong Magnetic Field on a Bursty Brown Dwarf: Puzzle Solved. , keywords =. doi:10.3847/1538-4357/aa866b , archivePrefix =. 1709.02861 , primaryClass =

    Pith/arXiv arXiv

  59. [59]

    , keywords =

    Resolved imaging confirms a radiation belt around an ultracool dwarf. , keywords =. doi:10.1038/s41586-023-06138-w , archivePrefix =. 2302.12841 , primaryClass =

    Pith/arXiv arXiv

  60. [60]

    , keywords =

    Detection of Exomoons through Observation of Radio Emissions. , keywords =. doi:10.1088/0004-637X/791/1/25 , archivePrefix =. 1308.4184 , primaryClass =

    Pith/arXiv arXiv

  61. [61]

    , 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

  62. [62]

    Journal of Geophysical Research (Space Physics) , keywords =

    Electron Acceleration to MeV Energies at Jupiter and Saturn. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1029/2018JA025665 , adsurl =

    work page doi:10.1029/2018ja025665

  63. [63]

    doi:10.1007/978-3-642-49300-3 , adsurl =

    Dynamics of geomagnetically trapped radiation. doi:10.1007/978-3-642-49300-3 , adsurl =

    work page doi:10.1007/978-3-642-49300-3

  64. [64]

    Science , keywords =

    Evidence for a radiation belt around a brown dwarf. Science , keywords =. doi:10.1126/science.adg6635 , archivePrefix =. 2303.06453 , primaryClass =

    Pith/arXiv arXiv

  65. [65]

    , keywords =

    Multifrequency analysis of the Jovian electron-belt radiation during the Cassini flyby of Jupiter. , keywords =. doi:10.1051/0004-6361/201423896 , adsurl =

    work page doi:10.1051/0004-6361/201423896

  66. [66]

    , year = 2003, month = jun, volume =

    VLA observations of Jupiter's synchrotron radiation at 15 and 22 GHz. , year = 2003, month = jun, volume =. doi:10.1016/S0019-1035(03)00068-X , adsurl =

    work page doi:10.1016/s0019-1035(03)00068-x 2003

  67. [67]

    , year = 2003, month = jun, volume =

    Jupiter's radio spectrum from 74 MHz up to 8 GHz. , year = 2003, month = jun, volume =. doi:10.1016/S0019-1035(03)00067-8 , adsurl =

    doi:10.1016/s0019-1035(03)00067-8 2003

  68. [68]

    , keywords =

    Inflating and Deflating Hot Jupiters: Coupled Tidal and Thermal Evolution of Known Transiting Planets. , keywords =. doi:10.1088/0004-637X/702/2/1413 , archivePrefix =. 0907.1268 , primaryClass =

    Pith/arXiv arXiv

  69. [69]

    , keywords =

    An internal heating mechanism operating in ultra-short-period planets orbiting magnetically active stars. , keywords =. doi:10.1051/0004-6361/202140284 , archivePrefix =. 2107.03044 , primaryClass =

    Pith/arXiv arXiv

  70. [70]

    Nature Astronomy , keywords =

    Magma oceans and enhanced volcanism on TRAPPIST-1 planets due to induction heating. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0284-0 , archivePrefix =. 1710.08761 , primaryClass =

    Pith/arXiv arXiv

  71. [71]

    Annual Review of Earth and Planetary Sciences , year = 2013, month = may, volume =

    Electrical Conductivity of Mantle Minerals: Role of Water in Conductivity Anomalies. Annual Review of Earth and Planetary Sciences , year = 2013, month = may, volume =. doi:10.1146/annurev-earth-050212-124022 , adsurl =

    doi:10.1146/annurev-earth-050212-124022 2013

  72. [72]

    , keywords =

    Centrifugal breakout reconnection as the electron acceleration mechanism powering the radio magnetospheres of early-type stars. , keywords =. doi:10.1093/mnras/stac341 , archivePrefix =. 2202.05449 , primaryClass =

    Pith/arXiv arXiv

  73. [73]

    Hydrodynamic and hydromagnetic stability

  74. [74]

    , keywords =

    Radio-flaring Ultracool Dwarf Population Synthesis. , keywords =. doi:10.3847/1538-4357/aa7ede , archivePrefix =. 1707.02212 , primaryClass =

    Pith/arXiv arXiv

  75. [75]

    , keywords =

    The occurrence rate of quiescent radio emission for ultracool dwarfs using a generalized semi-analytical Bayesian framework. , keywords =. doi:10.1093/mnras/stad2272 , archivePrefix =. 2306.16460 , primaryClass =

    Pith/arXiv arXiv

  76. [76]

    , keywords =

    Radio Emission from Binary Ultracool Dwarf Systems. , keywords =. doi:10.3847/1538-4357/ac660b , archivePrefix =. 2206.01754 , primaryClass =

    Pith/arXiv arXiv

  77. [77]

    , keywords =

    Constraints on magnetospheric radio emission from Y dwarfs. , keywords =. doi:10.1093/mnras/stz1372 , adsurl =

    work page doi:10.1093/mnras/stz1372

  78. [78]

    , keywords =

    The Strongest Magnetic Fields on the Coolest Brown Dwarfs. , keywords =. doi:10.3847/1538-4365/aac2d5 , archivePrefix =. 1808.02485 , primaryClass =

    Pith/arXiv arXiv

  79. [79]

    , keywords =

    Auroral Radio Emission from Late L and T Dwarfs: A New Constraint on Dynamo Theory in the Substellar Regime. , keywords =. doi:10.3847/0004-637X/818/1/24 , archivePrefix =. 1511.03661 , primaryClass =

    Pith/arXiv arXiv

  80. [80]

    , keywords =

    Tidal Heating in a Magma Ocean within Jupiter's Moon Io. , keywords =. doi:10.1088/0067-0049/218/2/22 , adsurl =

    work page doi:10.1088/0067-0049/218/2/22

Showing first 80 references.