Pith. sign in

REVIEW 4 major objections 4 minor 123 references

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

T0 review · 4 major / 4 minor · reviewed 2026-08-03 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Tidally heated Io-like planets can supply the plasma behind ultra-cool dwarf radio bursts.

desk verdict First quantitative Io-analog plasma-source model for UCD radio magnetospheres—plausible, falsifiable, and honestly bounded; the linear mass-loss scaling and hand-picked two-planet architecture are the main soft spots. read the letter →

arxiv 2607.25964 v2 pith:WI3O7L7C submitted 2026-07-28 astro-ph.EP

A. F. Lanza , A. V. Oza , A. V. Oza (Caltech , JPL , California , USA) This is my paper · ORCID
classification astro-ph.EP
keywords ultra-cooldwarfsbrownelectroncyclotronmasermagnetosphericmassflowtidalheatingexomoonsionosphericoutflowLSRJ1835+3259
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper asks where the plasma comes from that powers the GHz radio bursts of ultra-cool dwarfs and brown dwarfs, using the nearby dwarf LSR J1835+3259 as a concrete test case. The observed electron-cyclotron maser emission implies a magnetospheric mass flow of order 10^5 kg/s, comparable with what Jupiter's moon Io injects into Jupiter's magnetosphere. The paper argues this flow can be supplied by an Io-like tidally heated rocky planet orbiting within about 6 to 14 stellar radii, with a small eccentricity kept alive by an outer companion; a stellar ionospheric outflow is also viable but only if the star's effective Pedersen conductance is below about 0.02 mho. If true, this ties the radio brightness of ultra-cool dwarfs to the presence of close-in volcanic planets and offers a natural explanation for why ultra-cool dwarfs with distant companions are more often detected as radio emitters.

What carries the argument

The central mechanism is a four-step scaling chain. First, the electron-cyclotron maser radio flux is converted into a required magnetospheric mass flow through either an ionospheric-magnetospheric coupling model or an Alfvén-wing star-planet interaction model. Second, the Hill corotating-convection model translates a plasma density near the inner source into an upper limit on the outward mass flux through the magnetosphere. Third, tidal heating of an Io-like rocky planet scales as eccentricity squared over semimajor axis to the power 15/2, so a small but sustained eccentricity can keep a planet volcanically active. Fourth, an outer companion on a coplanar non-resonant orbit pumps the inner

What would settle it

A dedicated photometric campaign looking for 500 to 600 parts-per-million transits with periods between 5.5 and 12 hours around LSR J1835+3259; if no such planet is found while the star's effective Pedersen conductance is measured to exceed ~0.02 mho, the paper's central volcanic-planet and ionospheric-outflow scenarios would both fail under the model's assumptions.

Watch

Extended reading notes

Core claim

The paper's central claim is that the magnetosphere of the ultra-cool dwarf LSR J1835+3259, whose 8.4 GHz bursts require a maser-emitting field of about 3 kG, can be fed by either of two sources. A weak stellar ionospheric outflow can supply the required ~10^5 kg/s mass flow only if the effective Pedersen conductance of the stellar ionosphere is below about 0.02 mho for a closed magnetosphere; above that, the outflow falls short. The more robust source is a rocky planet with the mass and radius of Jupiter's moon Io, orbiting between about 6 and 14 stellar radii, tidally heated by an eccentricity of ~10^-3 that an outer companion continuously pumps; its volcanic outgassing can supply the need

Load-bearing premise

The load-bearing premise is that the observed electron-cyclotron maser burst flux is entirely produced by one of the two considered mechanisms operating alone at maximum efficiency, so the inferred required mass flow of ~10^5 kg/s follows directly from the radio flux; if flares or other electron acceleration processes contribute significantly, the required mass flow could be much smaller and the paper's source conclusions would change.

Editorial extensions

If this is right

  • A volcanically active Io-sized planet within about 6 to 14 stellar radii can supply the ~10^5 kg/s mass flow required by the ionospheric-magnetospheric coupling model for LSR J1835+3259.
  • A stellar ionospheric outflow can power the observed emission only if the effective Pedersen conductance is below ~0.02 mho (closed magnetosphere) or ~2 mho (open magnetosphere); otherwise the outflow is insufficient.
  • Induction heating of an Io-like planet by the star's magnetic field generally provides too little power to account for the needed mass loss, except in the low-flux, open-magnetosphere case.
  • If the emission is powered by Alfvén-wing interaction with a close-in planet, the required mass flow can reach 10^6 to 10^7 kg/s at low Pedersen conductance, demanding a rocky planet roughly 1.6 to 2.5 times Io's radius.
  • The inner planet should have a transit probability of about 10 to 17 percent, an orbital period under 12 hours, and a transit depth near 500 to 600 parts per million, making it detectable with dedicated space photometry.

Reading between the lines

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

  • If the volcanic-planet explanation is right, radio bursts from ultra-cool dwarfs can serve as a discovery channel for exomoons: an otherwise invisible Io-sized body could reveal itself through its star's radio light before any transit is detected.
  • A testable extension is that the burst morphology should differ between the two powering mechanisms: ionospheric coupling would produce auroral ovals tied to the magnetic poles, while Alfvén-wing footprints would produce bursts modulated at the planet's orbital period, allowing the two scenarios to be distinguished by high-cadence radio monitoring.
  • Because tidal heating scales steeply with radius, the model predicts that the most radio-loud ultra-cool dwarfs at low Pedersen conductance should host larger close-in rocky planets (roughly 1.6 to 2.5 Io radii), a prediction that transit surveys could check.
  • The induction-heating calculation suggests that the same framework could be extended to brown dwarfs with magma oceans or subsurface oceans, where induction heating may compete more strongly with tidal heating.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 4 minor

Summary. The paper addresses the plasma source for the ECM radio emission of the ultra-cool dwarf LSR J1835+3259. It estimates the magnetospheric mass flow required by two radio-emission models — the Turnpenney et al. (2017) ionospheric-magnetospheric coupling model and the Noyola et al. (2014) Alfvén-wing star-planet interaction model — and compares those requirements with three plasma-source models: a stellar ionospheric outflow (Appendix A), a tidally heated Io-like planet/satellite (Sect. 2.4.1-2.4.2), and an induction-heated planet (Sect. 2.4.3, Appendices B/B.1). The main quantitative result is that a tidally heated Io-analog at a ~ 6-14 R_s, with eccentricity e ~ 10^-3 maintained by an outer companion, can supply the ~10^5 kg/s needed by the closed-magnetosphere M-I model, whereas the ionospheric outflow can do so only for an effective Pedersen conductance below ~0.02 mho. The paper connects the tidal-heating scenario to the observed excess of radio emitters among ultra-cool dwarfs with companions.

Significance. The volcanic-satellite mechanism is an interesting and timely explanation for the inferred plasma supply in ultra-cool dwarf magnetospheres, and the paper makes concrete, falsifiable predictions (transit depth ~500-600 ppm, orbital periods of 5.5-12 h, Doppler-shifted sodium/potassium signatures). The use of standard tidal, Mardling, and Hill-model equations is a strength, as are the analytical outflow and induction appendices. However, the central quantitative claim is not yet robust: it depends on an uncalibrated linear scaling of mass loss with tidal power, on one arbitrary outer-perturber configuration, and on the assumption that the entire observed ECM burst is powered by a single mechanism at maximum efficiency. As written, the paper convincingly demonstrates a plausible scenario rather than a robust inference.

major comments (4)
  1. [§2.4.1, Eq. (11); §3.4, Fig. 2] The central positive claim is obtained by setting Mdot = 10^3 (P_tide/P_Io) kg/s. The text justifies this through a chain of proportionalities (eruption rate ∝ P_tide, atmospheric density ∝ eruption rate, sputtering loss ∝ atmospheric density), but no derivation, data, or modeling is supplied for the combined scaling. At P_tide/P_Io ~ 10^2 the model requires an escape rate ~10^5 kg/s, two orders of magnitude above Io. Collisionally thick atmospheres, limited SO2 inventories, or saturation of sputtering/ionization could break linearity; a factor-of-few sublinearity would push the 10^5 kg/s threshold inside 10 R_s and contradict the abstract. Please either derive the scaling from a surface-atmosphere/sputtering model or present sensitivity cases bracketing the constant.
  2. [§2.4.2 and §3.4 (outer-perturber parameters)] The equilibrium eccentricity e_eq from Mardling (2007) is evaluated for one assumed outerplanet configuration (m_c = 0.4 M_earth, e_c = 0.5, a_c = 3.5a). Since P_tide ∝ e_eq^2 in Eq. (10), the quoted semimajor-axis window (a ≲ 13 R_s in §3.4, 'below about 10 R_s' in the abstract) and the Table 2 YES/NO entries are contingent on that choice. The manuscript explicitly states that other configurations are not explored and asserts they would not change the conclusion, but no scaling or stability argument is provided. A parameter scan, or at least an analytic expression for the dependence of e_eq on (m_c, e_c, a_c/a), is needed to make the threshold claim robust.
  3. [§3.5 vs. Table 2 (induction-heating entries)] Table 2 marks 'YES' for planet induction heating in two rows (M-I model with open magnetosphere; Alfvén-wing model with Sigma*_p = 10.0 mho). In §3.5, that positive result is reached only for the outer-2% global salty-ocean conductivity <sigma> = 3.5 mho/m, and the same paragraph then rules out such an ocean on temperature grounds (T_eq ≈ 510 K at the substellar point; the nightside is frozen). The table entries are therefore internally inconsistent. This does not affect the central volcanic-satellite conclusion, but the table should be corrected or footnoted to reflect the adopted conductivity scenario.
  4. [§2.1–§2.2, §3.1, and Table 2 (ECM flux attribution)] The required mass flows are computed assuming the entire burst flux S ≈ 2500 μJy is produced by one mechanism alone, each at maximum efficiency. The paper acknowledges this in §2, but the Table 2 conclusions are then stated as physical thresholds without propagating uncertainties in the conversion efficiency beta_S, the beaming solid angle, the open/closed magnetosphere assumption, or the possible contribution of other ECM drivers. In particular, the ionospheric-outflow condition Sigma*_p <~ 0.02 mho is a point estimate resting on the upper-limit X-ray luminosity and f_w = 0.15; a lower required Mdot would relax the constraint, and a higher one would challenge the volcanic source. A sensitivity estimate around Mdot ~ 10^5 kg/s for the M-I route would strengthen the comparison.
minor comments (4)
  1. [Abstract vs. §3.4] The abstract states 'semimajor axis lower than about 10 stellar radii', while §3.4 gives ~13 R_s and the Conclusions say 6-14 R_s. These should be made consistent.
  2. [Eq. (11)] The sputtering formula is rendered as 'Mdot_sputtering ∼ PV U R2 x Mdot_Io' with no visible fraction bars or definitions in the equation itself. Please typeset it as (P V)/(U R_x^2) Mdot_Io and define every symbol locally.
  3. [Fig. 3 and Appendix C] The panel labels and text use 'Volcanic Planet' and 'Volcanic Satellite' inconsistently (Appendix C lists both as separate scenarios; §4 refers mainly to the 'volcanic planet' scenario). Clarify whether the tidal-heating source is a planet or a satellite and keep the terminology uniform.
  4. [Throughout] Several minor typographical issues remain, e.g., 'V oyager 1' in the Introduction. A careful proofreading pass is recommended.

Circularity Check

0 steps flagged · score 0.0 of 10

No circular derivation: radio-derived mass-flow requirements and theoretical source models are computed from independent inputs.

full rationale

The paper's central comparison in Table 2 is a forward-model consistency check, not a circular fit. The observed ECM flux enters only on the 'required mass flow' side via the Turnpenney et al. (2017) ionospheric-magnetospheric coupling model and the Noyola et al. (2014) Alfvén-wing model. The theoretical source rates are derived independently: the ionospheric outflow uses the observed X-ray luminosity upper limit and a coronal outflow model (Appendix A), while the volcanic-satellite mass supply uses tidal power computed from Eq. (10), the Mardling (2007) equilibrium eccentricity, and an Io-calibrated linear scaling Mdot ~ 1e3 (P_tide/P_Io) kg/s. None of these source calculations uses the radio flux as an input, and no fitted parameter is renamed as a prediction. The Io calibration (Mdot_Io ~ 1e3 kg/s, Q'_m ~ 100) is external and measured, and the assumed outer-planet parameters are stated rather than adjusted to match the radio-derived mass flow. The Gebek & Oza (2020) self-citation for the sputtering scaling is not load-bearing in a circular sense: the same scaling is supported by external Io-based work (Saur et al. 2003; Haff et al. 1981; Johnson 2004) and is externally falsifiable. The main limitations—the untested linearity of the tidal-heating-to-mass-loss scaling and the assumption that one mechanism powers the entire ECM flux—are scientific robustness concerns, not circularity by construction.

Assumptions & free parameters 9 free parameters · 8 assumptions · 3 invented entities

The central claims rest on a large set of adopted parameters and scaling assumptions: the Io-analog scaling of sputtering/mass-loss, the assumed outer perturbing planet, the specific Pedersen-conductance range, and the interpretation of ECM flux as a measure of Mdot. None of these are machine-checked or shipped as code/data. The numbers in Table 2 are order-of-magnitude estimates with wide input ranges.

free parameters (9)
  • Outer perturbing planet mass mc = 0.4 M_Earth
    Required in Sect. 3.4 / Fig. 2 to maintain the inner planet's eccentricity through Mardling (2007). Chosen by hand; the paper explicitly says different ac/a, ec, mc are not explored.
  • Outer perturbing planet eccentricity ec = 0.5
    Same as above—hand-chosen input forcing the equilibrium eccentricity of the inner volcanic planet.
  • Outer perturbing planet semimajor axis ratio ac/a = 3.5
    Hand-chosen for the Mardling equilibrium-eccentricity calculation; not justified by stability or formation arguments, only by giving a plausible e_pp ~ 10^-3.
  • Planet modified tidal quality factor Q'_m = 100
    Taken from Io (Lainey et al. 2009; Park et al. 2024). Adopted for the putative planet; the paper acknowledges rheology is unknown and considers values up to 10^5 for other systems.
  • Coronal temperature T_cor = 1.5 MK
    Adopted from Schrijver (2009) to convert the X-ray luminosity upper limit into a coronal base density (Eq. A.1). Affects the ionospheric-outflow density directly.
  • Coronal-hole area fraction f_w = 0.15
    Mean solar coronal-hole fractional area from Soon et al. (2000); applied to LSR J1835+3259 without independent constraint.
  • Induction-heating conductivity <sigma> = 0.01-3.5 mho/m
    Chosen in Appendix B based on Earth-mantle analogs and a 'hypothetical salty ocean'; directly sets the induction-heating power, though this scenario is found insufficient anyway.
  • Magnetospheric plasma temperature T = Teq = T_eff sqrt(Rs/a)
    Assumed blackbody equilibrium temperature for the centrifugal scale height; no thermal model of the plasma torus.
  • Observed ECM flux S = 2500 muJy
    Input from Hallinan et al. (2008) / Kao et al. (2023); drives all Mdot estimates through both mechanisms.
assumptions (8)
  • domain assumption The observed bursty 8.4 GHz ECM flux is entirely powered by either ionospheric-magnetospheric coupling or star-planet Alfven wings, each alone.
    Stated in Sect. 2: 'we consider each mechanism as operating alone and being responsible for the entire ECM emission.' This is a monotonicity assumption; if other processes contribute, required Mdot shrinks.
  • domain assumption The stellar magnetic field is a simple dipole scaling from the polar field Bp inferred from the ECM frequency.
    Used throughout (Eq. 4, Eq. B.6); the resolved lobes of quiescent emission support a large-scale dipole, but the field geometry near the surface/planet is not directly measured.
  • standard math The Hill corotating-convection model (Hill et al. 1981) applies with a constant Mdot, and Eq. (8) is a valid upper limit when the outflow cylinder is at radius a with centrifugal scale height Hc.
    The paper explicitly adopts this model from Hill et al. (1981), including the 1/sqrt(6) factor and the R_H scaling. It is not re-derived.
  • domain assumption The plasma mass-loss rate from the volcanic planet is linearly proportional to tidal power P_tide, following Io's sputtering/scaling model (Eq. 10-11).
    Sect. 2.4.1: 'the mass flow rate will be proportional to the tidal heating power P_tide'. This assumes the atmospheric density responds linearly to volcanic output, extrapolating Io's complex magnetosphere chemistry to an exoplanet around a UCD.
  • domain assumption SO2 ions are the dominant plasma species, mass 64 amu.
    Assumed for the centrifugal scale height (Sect. 3.2); appropriate for Io analog, but unverified for the putative exoplanet.
  • domain assumption LSR J1835+3259's X-ray luminosity upper limit gives a valid coronal base density through Eq. (A.1) with standard radiative-loss function and solar composition.
    Appendix A; used to normalize the ionospheric outflow. The paper itself cites the thin/UCD corona work of Magaudda et al. (2024), but the electron density derived from an upper limit is only an upper limit.
  • standard math Mardling (2007) equilibrium-eccentricity mechanism (with GR and stellar oblateness precession) maintains a two-planet system with inner e ~ 10^-3 for Gyr timescales.
    Sect. 2.4.2 and Fig. 2; the paper implements Eq. (36) of Mardling (2007) with rotational-deformation contribution; relies on the cited model's validity for this parameter regime.
  • domain assumption The magnetosphere can be treated as either fully open or fully closed when applying Turnpenney et al. (2017) mass-flux estimates.
    Sect. 2.1/3.1; the open/closed dichotomy is taken from Turner et al. (2017) and sets the 10^5 vs 10^3 kg/s scale.
invented entities (3)
  • Volcanically active Io-like planet (or satellite) around LSR J1835+3259, with an outer perturbing planet (mc=0.4 M_Earth, ec=0.5, ac=3.5a).
    purpose: To supply ~10^5 kg/s of magnetospheric plasma via tidal heating and to maintain the inner planet's orbital eccentricity so tidal heating persists.
    The system is postulated to make the numbers work; no direct detection is reported. The paper provides a falsifiable handle (transit depth ~500-600 ppm, period 5.5-12 h, SO2 torus signatures), but no current evidence.
  • Stellar ionospheric outflow with f_w = 0.15 open coronal-field fraction. independent evidence
    purpose: Alternative plasma source to the magnetosphere; normalized to the X-ray upper limit.
    Its supply rate is tied to an observed upper limit (X-ray luminosity) and a physical model in Appendix A, so it is partly falsifiable, though f_w is adopted from solar values.
  • Salty-ocean outer-shell planet model for induction heating (sigma ~3.5 mho/m).
    purpose: To test whether induction heating could be as strong as tidal heating.
    Considered only to show it fails (the equilibrium temperature is too high for a stable ocean); this is an invented scenario but not a load-bearing one.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Volcanic Satellites and Ion Escape in the Magnetospheres of Ultra-Cool and Brown Dwarf Stars." pith.science (2026). https://pith.science/paper/WI3O7L7C

@misc{pith2026260725964,
  author       = {Pith},
  title        = {Pith review of: Volcanic Satellites and Ion Escape in the Magnetospheres of Ultra-Cool and Brown Dwarf Stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/WI3O7L7C}},
  note         = {Machine review of arXiv:2607.25964}
}
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 the authors.

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 ∗ p = 0.0… view at source ↗
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 inner plane… view at source ↗
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, (5) Stellar… view at source ↗

Review history (2 revisions) →

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

123 extracted references · 63 linked inside Pith

  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 =

    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 =

    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 =

    doi:10.1029/1999ja900304

Show all 123 references
  1. [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 =

    arXiv

  2. [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 =

    2004 doi

  3. [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 =

    arXiv

  4. [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 =

    arXiv

  5. [13]

    , keywords =

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

    arXiv

  6. [14]

    , keywords =

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

    doi

  7. [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 =

    2011

  8. [16]

    , keywords =

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

    doi

  9. [17]

    , keywords =

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

    arXiv

  10. [18]

    , keywords =

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

    arXiv

  11. [19]

    , keywords =

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

  12. [20]

    , keywords =

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

    doi

  13. [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 =

    arXiv

  14. [22]

    Experimental Astronomy , keywords =

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

    2009 arXiv

  15. [23]

    , keywords =

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

    arXiv

  16. [24]

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

    arXiv

  17. [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 =

    arXiv

  18. [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

  19. [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 =

    2014 doi

  20. [28]

    , keywords =

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

    arXiv

  21. [29]

    , keywords =

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

    arXiv

  22. [30]

    , keywords =

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

    doi

  23. [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 =

    1979 doi

  24. [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 =

    arXiv

  25. [33]

    , keywords =

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

    doi

  26. [34]

    , keywords =

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

    arXiv

  27. [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

  28. [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 =

    2001 doi

  29. [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 =

    2007 doi

  30. [38]

    , keywords =

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

    doi

  31. [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 =

    arXiv

  32. [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 =

    2007 doi

  33. [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 =

    arXiv

  34. [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 =

    arXiv

  35. [43]

    , keywords =

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

    doi

  36. [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 =

    arXiv

  37. [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 =

    arXiv

  38. [46]

    , keywords =

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

    arXiv

  39. [47]

    , keywords =

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

    arXiv

  40. [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 =

    arXiv

  41. [49]

    arXiv e-prints , keywords =

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

    doi arXiv

  42. [50]

    , keywords =

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

    doi

  43. [51]

    , keywords =

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

    doi

  44. [52]

    , keywords =

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

    arXiv

  45. [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 =

    2022

  46. [54]

    , keywords =

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

    doi

  47. [55]

    , keywords =

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

    doi

  48. [56]

    , keywords =

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

    doi

  49. [57]

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

    arXiv

  50. [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 =

    arXiv

  51. [59]

    , keywords =

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

    arXiv

  52. [60]

    , keywords =

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

    arXiv

  53. [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

  54. [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 =

    doi

  55. [63]

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

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

    doi

  56. [64]

    Science , keywords =

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

    arXiv

  57. [65]

    , keywords =

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

    doi

  58. [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 =

    2003 doi

  59. [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 =

    2003 doi

  60. [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 =

    arXiv

  61. [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 =

    arXiv

  62. [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 =

    arXiv

  63. [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 =

    2013 doi

  64. [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 =

    arXiv

  65. [73]

    Hydrodynamic and hydromagnetic stability

  66. [74]

    , keywords =

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

    arXiv

  67. [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 =

    arXiv

  68. [76]

    , keywords =

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

    arXiv

  69. [77]

    , keywords =

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

    doi

  70. [78]

    , keywords =

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

    arXiv

  71. [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 =

    arXiv

  72. [80]

    , keywords =

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

    doi

  73. [81]

    , keywords =

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

    arXiv

  74. [82]

    Essential Radio Astronomy

  75. [83]

    , keywords =

    Doppler shifted transient sodium detection by KECK/HIRES. , keywords =. doi:10.1093/mnrasl/slaf031 , archivePrefix =. 2504.03974 , primaryClass =

    arXiv

  76. [84]

    , keywords =

    Tidal dissipation in satellites prevents Hill sphere escape. , keywords =. doi:10.1093/mnras/stad3543 , archivePrefix =. 2309.11609 , primaryClass =

    arXiv

  77. [85]

    and Hakim, Kaustubh and Manoj, P

    Narang, Mayank and Oza, Apurva V. and Hakim, Kaustubh and Manoj, P. and Banyal, Ravinder K. and Thorngren, Daniel P. , title =. The Astronomical Journal , abstract =. 2022 , month =. doi:10.3847/1538-3881/ac9eb8 , url =

    2022 doi

  78. [86]

    , keywords =

    uGMRT observations of the hot-Saturn WASP-69b: Radio-Loud Exoplanet-Exomoon Survey II (RLEES II). , keywords =. doi:10.1093/mnras/stad1027 , archivePrefix =. 2303.17269 , primaryClass =

    arXiv

  79. [87]

    , keywords =

    Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets. , keywords =. doi:10.3847/1538-4357/ab40cc , archivePrefix =. 1908.10732 , primaryClass =

    1908 arXiv

  80. [88]

    , keywords =

    X-ray astronomy of stellar coronae. , keywords =. doi:10.1007/s00159-004-0023-2 , archivePrefix =. astro-ph/0406661 , primaryClass =

    arXiv

  81. [89]

    , year = 2002, month = feb, volume =

    Ultra-relativistic electrons in Jupiter's radiation belts. , year = 2002, month = feb, volume =. doi:10.1038/415987a , adsurl =

    2002 doi

  82. [90]

    , keywords =

    On the Detection of Exomoons Transiting Isolated Planetary-mass Objects. , keywords =. doi:10.3847/2041-8213/ac1e2d , archivePrefix =. 2108.08323 , primaryClass =

    arXiv

  83. [91]

    , keywords =

    Tidal Evolution of Close-in Extrasolar Planets. , keywords =. doi:10.1086/529187 , archivePrefix =. 0802.1543 , primaryClass =

    arXiv

  84. [92]

    , keywords =

    Secular Evolution of Hierarchical Triple Star Systems. , keywords =. doi:10.1086/308815 , adsurl =

    doi

  85. [93]

    , keywords =

    Long-term tidal evolution of short-period planets with companions. , keywords =. doi:10.1111/j.1365-2966.2007.12500.x , archivePrefix =. 0706.0224 , primaryClass =

    2007

  86. [94]

    , keywords =

    Calculating the Tidal, Spin, and Dynamical Evolution of Extrasolar Planetary Systems. , keywords =. doi:10.1086/340752 , adsurl =

    doi

  87. [95]

    , keywords =

    A Panchromatic View of Brown Dwarf Aurorae. , keywords =. doi:10.3847/1538-4357/aa8596 , archivePrefix =. 1708.02942 , primaryClass =

    arXiv

  88. [96]

    , keywords =

    Individual Dynamical Masses of Ultracool Dwarfs. , keywords =. doi:10.3847/1538-4365/aa5e4c , archivePrefix =. 1703.05775 , primaryClass =

    arXiv

  89. [97]

    , keywords =

    An N-body population synthesis framework for the formation of moons around Jupiter-like planets. , keywords =. doi:10.1093/mnras/stab1179 , archivePrefix =. 2011.11513 , primaryClass =

    2011 arXiv

  90. [98]

    , keywords =

    Radiation Belt Radial Diffusion at Earth and Beyond. , keywords =. doi:10.1007/s11214-020-0642-610.1002/essoar.10501074.2 , adsurl =

    doi

  91. [99]

    , keywords =

    Transitions in magnetic behavior at the substellar boundary. , keywords =. doi:10.1051/0004-6361/202449403 , archivePrefix =. 2401.17292 , primaryClass =

    arXiv

  92. [100]

    Journal of Geophysical Research (Space Physics) , keywords =

    The analytical solution of the transient radial diffusion equation with a nonuniform loss term. Journal of Geophysical Research (Space Physics) , keywords =. doi:10.1002/2017JA023868 , adsurl =

    doi

  93. [101]

    , keywords =

    X-Ray/Microwave Relation of Different Types of Active Stars. , keywords =. doi:10.1086/186766 , adsurl =

    doi

  94. [102]

    , year = 2003, month = jun, volume =

    The ion mass loading rate at Io. , year = 2003, month = jun, volume =. doi:10.1016/S0019-1035(03)00085-X , adsurl =

    2003 doi

  95. [103]

    , keywords =

    Tidal Heating of Extrasolar Planets. , keywords =. doi:10.1086/587641 , archivePrefix =. 0803.0026 , primaryClass =

    arXiv

  96. [104]

    , year = 2009, month = jun, volume =

    Strong tidal dissipation in Io and Jupiter from astrometric observations. , year = 2009, month = jun, volume =. doi:10.1038/nature08108 , adsurl =

    2009 doi

  97. [105]

    , keywords =

    Io's heat flow from infrared radiometry: 1983-1993. , keywords =. doi:10.1029/94JE00637 , adsurl =

    1983 doi

  98. [106]

    arXiv e-prints , keywords =

    Mass supply from Io to Jupiter's magnetosphere. arXiv e-prints , keywords =. doi:10.48550/arXiv.2403.13970 , archivePrefix =. 2403.13970 , primaryClass =

    doi arXiv

  99. [107]

    , keywords =

    Stable satellites around extrasolar giant planets. , keywords =. doi:10.1111/j.1365-2966.2006.11104.x , adsurl =

    2006

  100. [108]

    , keywords =

    Massive Satellites of Close-In Gas Giant Exoplanets. , keywords =. doi:10.1088/0004-637X/704/2/1341 , archivePrefix =. 0909.0770 , primaryClass =

    arXiv

  101. [109]

    , keywords =

    Can close-in giant exoplanets preserve detectable moons?. , keywords =. doi:10.1093/mnras/stz3548 , archivePrefix =. 1912.08049 , primaryClass =

    1912 arXiv

  102. [110]

    , keywords =

    The effect of close-in giant planets' evolution on tidal-induced migration of exomoons. , keywords =. doi:10.1093/mnras/stx1745 , archivePrefix =. 1707.02906 , primaryClass =

    arXiv

  103. [111]

    Planet occurrence rates from a subsample of 71 stars

    The CARMENES search for exoplanets around M dwarfs. Planet occurrence rates from a subsample of 71 stars. , keywords =. doi:10.1051/0004-6361/202140968 , archivePrefix =. 2107.03802 , primaryClass =

  104. [112]

    HADES RV Programme with HARPS-N at TNG. XV. Planetary occurrence rates around early-M dwarfs. , keywords =. doi:10.1051/0004-6361/202142828 , archivePrefix =. 2203.04648 , primaryClass =

    arXiv

  105. [113]

    , keywords =

    Hierarchical Bayesian calibration of tidal orbit decay rates among hot Jupiters. , keywords =. doi:10.1093/mnras/sty292 , archivePrefix =. 1801.10561 , primaryClass =

    arXiv

  106. [114]

    , year = 1964, month = sep, volume =

    Influence of the Satellite Io on Jupiter's Decametric Emission. , year = 1964, month = sep, volume =. doi:10.1038/2031008a0 , adsurl =

    1964 doi

  107. [115]

    , year = 1974, month = feb, volume =

    High-Resolution Spectra of Sodium Emission from IO. , year = 1974, month = feb, volume =. doi:10.1086/181413 , adsurl =

    1974 doi

  108. [116]

    Science , keywords =

    Discovery of Currently Active Extraterrestrial Volcanism. Science , keywords =. doi:10.1126/science.204.4396.972 , adsurl =

    doi

  109. [117]

    , keywords =

    Redshifted Sodium Transient near Exoplanet Transit. , keywords =. doi:10.3847/2041-8213/ad6b29 , archivePrefix =. 2409.19844 , primaryClass =

    arXiv

  110. [118]

    , in press, arXiv e-prints , keywords =

    Extreme exomoons in WASP-49 Ab: dynamics and detectability. , in press, arXiv e-prints , keywords =. doi:10.48550/arXiv.2501.05866, 10.1051/0004-6361/202452968 , archivePrefix =. 2501.05866 , primaryClass =

    doi arXiv

  111. [119]

    Park, R. S. and Jacobson, R. A. and Gomez Casajus, L. and Nimmo, F. and Ermakov, A. I. and Keane, J. T. and McKinnon, W. B. and Stevenson, D. J. and Akiba, R. and Idini, B. and Buccino, D. R. and Magnanini, A. and Parisi, M. and Tortora, P. and Zannoni, M. and Mura, A. and Dur...

    2024 doi

  112. [120]

    , keywords =

    Alkaline exospheres of exoplanet systems: evaporative transmission spectra. , keywords =. doi:10.1093/mnras/staa2193 , archivePrefix =. 2005.02536 , primaryClass =

    2005 arXiv

  113. [121]

    The Io neutral clouds and plasma torus. Jupiter. The Planet, Satellites and Magnetosphere , year = 2004, editor =

    2004

  114. [122]

    , keywords =

    Detection and characterization of Io's atmosphere from high-resolution 4- m spectroscopy. , keywords =. doi:10.1016/j.icarus.2015.02.018 , archivePrefix =. 1502.05620 , primaryClass =

    2015 arXiv

  115. [123]

    Planetary Science Journal , keywords =

    Io's Optical Aurorae in Jupiter's Shadow. Planetary Science Journal , keywords =. doi:10.3847/PSJ/ac85b0 , archivePrefix =. 2302.10849 , primaryClass =

    arXiv

Pith tools

Reviewed August 3, 2026 · model on record in the stance chip above.