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arxiv: 1907.05088 · v1 · pith:GT4SPTFTnew · submitted 2019-07-11 · 🌌 astro-ph.EP

Detecting volcanically produced tori along orbits of exoplanets using UV spectroscopy

Kristina G. Kislyakova , Luca Fossati , Denis Shulyak , Eike G\"unther , Manuel G\"udel , Colin P. Johnstone , Vladimir Airapetian , Sudeshna Boro Saikia
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Allan Sacha Brun Vera Dobos Kevin France Eric Gaidos Maxim L. Khodachenko Antonino F. Lanza Helmut Lammer Lena Noack Rodrigo Luger Antoine Strugarek Aline Vidotto Allison Youngblood
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Pith reviewed 2026-05-24 23:02 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanetsplasma torivolcanic activityUV spectroscopyM dwarfsHubble Space TelescopeTESSatmospheric escape
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The pith

Plasma tori from volcanic activity on M-dwarf exoplanets could be detected by HST in UV light

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

The paper proposes that volcanic material lost from exoplanets orbiting M dwarfs can form plasma tori along their orbits, driven by tidal or electromagnetic induction heating. These tori would resemble the Io plasma torus around Jupiter. The authors argue that follow-up HST observations of TESS targets would be able to detect such tori through their ultraviolet emission. A reader would care because this offers an indirect way to identify active internal heating and atmospheric escape on distant planets.

Core claim

The authors propose using Hubble Space Telescope follow-up observations of TESS targets for detecting possible plasma tori along the orbits of exoplanets orbiting M dwarfs. The source of the torus could be planetary volcanic activity due to tidal or electromagnetic induction heating. Fast losses to space for planets orbiting these active stars can lead to the lost material forming a torus along the planetary orbit, similar to the Io plasma torus. They show that such a torus would be potentially detectable by the HST in the UV.

What carries the argument

The stable plasma torus formed by volcanically outgassed material distributed along the planetary orbit, analogous to the Io torus

Load-bearing premise

Material lost from the planet due to volcanic activity will form a stable, detectable plasma torus along the orbit rather than dispersing or being removed by stellar wind on short timescales

What would settle it

An HST UV observation of a TESS target showing no excess emission along the planetary orbit, or a dynamical model demonstrating that the lost material disperses before completing even one orbit

Figures

Figures reproduced from arXiv: 1907.05088 by Aline Vidotto, Allan Sacha Brun, Allison Youngblood, Antoine Strugarek, Antonino F. Lanza, Colin P. Johnstone, Denis Shulyak, Eike G\"unther, Eric Gaidos, Helmut Lammer, Kevin France, Kristina G. Kislyakova, Lena Noack, Luca Fossati, Manuel G\"udel, Maxim L. Khodachenko, Rodrigo Luger, Sudeshna Boro Saikia, Vera Dobos, Vladimir Airapetian.

Figure 1
Figure 1. Figure 1: Observation of the Io plasma torus in SIII line by Hisaki satellite (Murakami et al., 2016). Murakami et al., 2016). Io’s torus has been observed both from space by the UVIS instrument on-board Cassini (Steffl et al., 2004) and by Voyager 1 (Volwerk, 2018), and from the ground (e.g., Thomas, 1996). Techniques for the removal of the geocoronal emission produced by neutral hydrogen and oxygen have been only … view at source ↗
Figure 2
Figure 2. Figure 2: Synthetic Gaussian profile of the Oi line at 1304.858 ˚A (blue) su￾perposed to a synthetic Voigt absorption feature (red) computed assuming a column density of 1013 cm−2 . The final emission line (black), which includes the torus absorption, was computed assuming a signal-to-noise ratio of 10. The spectral resolution is that of the E140M HST/STIS grating. From Kislyakova et al. (2018). 3. Science goals of … view at source ↗
read the original abstract

We suggest to use the Hubble Space Telescople (HST) follow-up observations of the TESS targets for detecting possible plasma tori along the orbits of exoplanets orbiting M dwarfs. The source of the torus could be planetary volcanic activity due to tidal or electromagnetic induction heating. Fast losses to space for planets orbiting these active stars can lead to the lost material forming a torus along the planetary orbit, similar to the Io plasma torus. We show that such torus would be potentially detectable by the HST in the UV.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 1 minor

Summary. The manuscript proposes using HST UV spectroscopy to detect plasma tori along the orbits of exoplanets around M dwarfs, with the tori sourced from volcanic outgassing driven by tidal or electromagnetic induction heating. It draws an analogy to the Io plasma torus and suggests such features around TESS targets would be potentially detectable.

Significance. If the central claim holds after quantitative validation, the work would introduce a new observational channel for inferring volcanic activity and internal heating on exoplanets. The suggestion is conceptually novel within the exoplanet-atmosphere literature, but the manuscript supplies no supporting calculations, error budgets, or signal predictions, so the significance remains prospective rather than demonstrated.

major comments (2)
  1. [Abstract] Abstract: the statement that 'such torus would be potentially detectable by the HST in the UV' is presented without any estimate of torus density, emission measure, line fluxes, or comparison to HST sensitivity and background levels. This quantitative gap is load-bearing for the detectability claim.
  2. [Abstract] Abstract (and throughout): no supply-rate versus stellar-wind removal-rate comparison is given for M-dwarf parameters, nor is the continuity equation integrated along the orbit to show that material accumulates into a stable torus rather than being stripped on orbital timescales. The Io analogy alone does not establish persistence under the higher ram pressure and EUV flux of M dwarfs.
minor comments (1)
  1. [Abstract] Abstract: 'Telescople' is a typographical error and should read 'Telescope'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their review and constructive comments on our manuscript proposing HST UV observations to detect possible volcanically sourced plasma tori around exoplanets orbiting M dwarfs. The work is a short conceptual proposal drawing an analogy to the Io torus. We respond to each major comment below and will make revisions to address the identified gaps by qualifying our claims.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the statement that 'such torus would be potentially detectable by the HST in the UV' is presented without any estimate of torus density, emission measure, line fluxes, or comparison to HST sensitivity and background levels. This quantitative gap is load-bearing for the detectability claim.

    Authors: We agree that the manuscript provides no quantitative estimates of torus density, emission measure, line fluxes, or direct comparison to HST sensitivity. The detectability statement is based on scaling from the well-observed Io torus rather than new calculations. As this is a brief proposal paper, performing the full radiative transfer and sensitivity analysis lies outside its scope. We will revise the abstract and main text to remove the unqualified claim of potential detectability and instead state that the torus could be detectable if its properties are comparable to Io's, pending detailed modeling. revision: yes

  2. Referee: [Abstract] Abstract (and throughout): no supply-rate versus stellar-wind removal-rate comparison is given for M-dwarf parameters, nor is the continuity equation integrated along the orbit to show that material accumulates into a stable torus rather than being stripped on orbital timescales. The Io analogy alone does not establish persistence under the higher ram pressure and EUV flux of M dwarfs.

    Authors: The referee is correct that we have not compared supply and removal rates for M-dwarf stellar winds or integrated the continuity equation. The persistence argument rests solely on the Io analogy without quantitative adjustment for the stronger EUV flux and ram pressure around M dwarfs. We will add a new paragraph in the discussion section explicitly noting this limitation, stating that torus stability under M-dwarf conditions remains to be verified by future work that solves the relevant plasma transport equations. revision: yes

Circularity Check

0 steps flagged

No circularity; qualitative observational proposal with no internal derivations or fitted predictions

full rationale

The paper is an observational suggestion to use HST UV spectroscopy on TESS targets to search for plasma tori around M-dwarf exoplanets, motivated by analogy to the Io torus and volcanic outgassing. No equations, parameter fits, continuity-equation integrations, or supply/removal-rate calculations are presented that could reduce to inputs by construction. The detectability claim is a qualitative assertion rather than a derived prediction. No self-citations function as load-bearing uniqueness theorems or ansatzes. The work is self-contained as a proposal and does not exhibit any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review supplies no explicit free parameters, axioms, or invented entities; the suggestion implicitly relies on the existence of Io-like tori around exoplanets but does not introduce new ones.

pith-pipeline@v0.9.0 · 5703 in / 1033 out tokens · 24636 ms · 2026-05-24T23:02:42.883495+00:00 · methodology

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Reference graph

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