Resonant structures in exozodiacal clouds created by exo-Earths in the habitable zone of late-type stars

Hangbin Jo; Masateru Ishiguro; Seung-Yoo Lee; Sung-Chul Yoon

REVIEW 3 major objections 6 minor 10 references

Resonant structures in exozodiacal clouds created by exo-Earths in the habitable zone of late-type stars

T0 review · 3 major / 6 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 Stellar wind drag—not just starlight—shapes planet-carved dust rings, and around old M dwarfs it cuts ring contrast by roughly half.

desk verdict Solid extension of resonant-dust modeling to late-type stars; the K–M contrast ordering is gyrochronology-selection dependent, but the qualitative wind effect and K-type asymmetric flux result stand. read the letter →

arxiv 2511.17872 v1 pith:LBPLDYSL submitted 2025-11-22 astro-ph.EP astro-ph.SR

Seung-Yoo Lee , Masateru Ishiguro , Hangbin Jo , Sung-Chul Yoon This is my paper

classification astro-ph.EPastro-ph.SR

keywords exozodiacaldustmeanmotionresonancesPoynting-Robertsondragstellarwindhabitablezonelate-typestarsnullinginterferometryresonantring

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

This paper tries to establish that resonant dust rings created by Earth-like planets in the habitable zone look different around F4, G4, K4, and M4 stars because stellar wind drag strength varies with spectral type. In a modeled 4 Gyr M4 system, the stellar wind dominates over Poynting-Robertson drag by a factor of about 44, so dust migrates inward faster and resonant trapping becomes less efficient; the ring's contrast falls by roughly a factor of two compared with a model that assumes Solar-like wind everywhere. At a fixed background dust level, the optical-depth contrast of the ring rises toward lower-mass stars, reaching about 9.85 for M4 versus 1.95 for F4. The result matters because future mid-infrared nulling interferometry will use exozodi models to distinguish planets from dust, and K-type stars are predicted to give the strongest asymmetric 10-micron signal—about 31% of the planet's own flux.

What carries the argument

The load-bearing object is the dimensionless ratio of stellar wind drag to Poynting-Robertson drag, denoted ψ. It enters the equations through effective beta parameters—radial drag close to the radiation-pressure-to-gravity ratio, and tangential drag proportional to (1+ψ)—so that ψ controls how quickly dust spirals inward past mean motion resonances. Higher ψ means faster migration, fewer grains trapped in resonance, and weaker resonant rings. The paper also builds a modified contrast parameter, ap^{1/2}[β_PR(1+ψ)]^{-1}M*^{-1/2}, and a closed-form contrast fit that turns ψ and stellar mass into ring prominence.

What would settle it

Measure the rotation period and mass-loss rate of a 4 Gyr M4 dwarf to compute the ratio of wind drag to light drag directly; if it comes out near the Solar value of about 0.3 rather than about 44, the model's M-dwarf contrast suppression is falsified. A complementary check is deep mid-infrared observation of old M dwarfs with known habitable-zone planets: rings near the no-wind prediction would contradict the wind-suppression result.

Watch

Extended reading notes

Core claim

Resonant ring structures form in every simulated spectral type. The central quantitative discovery is the spectral-type dependence of the drag ratio: for an old M4 star, stellar wind drag is about 44 times stronger than Poynting-Robertson drag, versus about 0.37 for a G4 star. Because the inward drift time scales inversely with the combined drag, the M4 wind shortens dust lifetimes and lowers the resonant-trapping probability, producing a ring that is roughly half as contrasted as a solar-wind model predicts. Across the four spectral types, size-integrated optical-depth contrast is 1.95, 5.98, 8.07, and 9.85 for F4, G4, K4, and M4 respectively, and the 10-micron asymmetric flux peaks at K4 w

Load-bearing premise

The results depend on the assumption that old M dwarfs really blow winds as strong as the adopted spin-down and mass-loss models say; if a real 4-billion-year-old M dwarf has a much weaker wind, the predicted halving of the dust ring disappears.

Editorial extensions

If this is right

Exozodi noise models for nulling interferometry must include spectral-type-dependent stellar wind; using a fixed Solar-like wind overestimates M-dwarf resonant-ring optical depth by about a factor of two.
At a fixed 3-zodi background level, resonant rings reach optical depths of roughly 6, 18, 24, and 30 zodis for F4, G4, K4, and M4, so structured dust becomes increasingly important around lower-mass stars.
K-type stars are the worst case for false-planet confusion: their asymmetric 10-micron emission is about 31% of the planet's flux, roughly twice the G-type value.
Stellar wind drag remains dynamically important around old K and M stars, supporting wind-driven removal as an explanation for the scarcity of warm infrared excess around mature M dwarfs when dust replenishment is limited.
If older M dwarfs follow a faster-spindown model giving a drag ratio near 127 instead of 44, the M4 ring contrast drops below K4, shifting the peak but leaving the wind-dominance conclusion intact.

Reading between the lines

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

By the same drag scaling, young (~1 Gyr) M dwarfs would have wind-to-light drag ratios of order a hundred or more, implying dust removal so fast that resonant rings in those systems may be transient; the paper estimates the age trend but does not simulate young disks.
An exo-Earth survey might reasonably de-prioritize K stars for confusion-limited observations even though M dwarfs show the highest ring contrast, because compact M-dwarf systems emit less total asymmetric flux; this prioritization follows from the flux maps but the paper does not make it.
If measured M-dwarf wind speeds turn out to be lower than the assumed 400 km/s, the drag ratio drops and the M4 ring becomes more prominent again, so wind speed is a directly testable lever on the headline result.

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.

Desk Editor's Note

read the letter

Short version: this is a useful, honest extension of Stark & Kuchner (2008) to F4–M4 stars with spectral-type-dependent stellar wind drag. The headline quantitative claims — ψ≈44 for a 4 Gyr M4 star, stellar wind cutting M-dwarf ring contrast by roughly half, ⟨Cτ⟩ rising from ~2 to ~10 from F to M, and K-type stars peaking in asymmetric 10-µm flux at ~31% of the planet's flux — will be of genuine interest to anyone building exozodi noise models for LIFE. The paper deserves a serious referee and probably conditional acceptance after some reporting fixes.

The genuinely new content is the ψ estimates at Gyr ages, the Model I/II comparison, the multi-size optical depth grid, and the K-type peak in asymmetric flux. The framework is a straightforward extension, but that is not a criticism; it is clearly explained and the dynamical equations and timescale checks are coherent. Credit also for the appendices: the paper explicitly works through the alternative gyrochronology and shows how the M4 numbers change. That is the right way to handle a known uncertainty.

The soft spot is exactly that alternative gyrochronology. The abstract says 'optical depth contrast of the resonant ring increased for lower-mass stars,' and the summary repeats the monotonic trend. But the paper's own Appendix B.3 shows that using Lu et al. gyrochrones for M4 (ψ≈127 instead of 44) drops ⟨Cτ⟩ for M4 from 9.85 to about 6.9, below K4. So the ordering is selection-dependent. The qualitative conclusion — stellar wind matters and must be included for late-type stars — is robust; the quantitative M-dwarf numbers are not. That needs to be stated in the abstract and conclusions, not just in an appendix.

Two smaller reproducibility issues: the dust bulk density ρ is listed in Table A.1 but never given a value, and no code is shipped. The ρ value affects β_PR and thus all contrast numbers; a reader cannot reproduce the simulations without it. Neither is fatal, but both are easy to fix.

Overall: the central argument holds up in its robust form. The paper is aimed at exozodi modelers and LIFE mission planners, and it gives them a concrete, if upper-bound, estimate of resonant-structure noise across spectral types. I would send it to peer review.

Referee Report

3 major / 6 minor

Summary. The paper studies resonant structures in exozodiacal dust around F4–M4 main-sequence stars with an Earth-mass planet in the conservative habitable zone, extending the Stark & Kuchner (2008) framework by adding spectral-type-dependent stellar wind drag in addition to Poynting-Robertson drag. Using MERCURY6 simulations in a pilot setup (100 particles, fixed 50 µm grains, Model I vs II) and a main multi-size setup (5000 particles, 0.1–300 µm, Model II only), it reports that resonant rings form for all four spectral types; that stellar wind drag can dominate PR drag for old M dwarfs (ψ≈44 at 4 Gyr), reducing the M4 ring contrast by roughly a factor of two; that the optical-depth contrast of the resonant ring increases toward lower-mass stars (⟨Cτ⟩ = 1.95, 5.98, 8.07, 9.85 for F4, G4, K4, M4) at a fixed background level; and that asymmetric 10 µm emission peaks for K-type stars (~30.8% of the planetary flux). The paper also provides a semi-analytical contrast function and discusses timescale and model limitations.

Significance. If the results hold, the paper fills a genuine gap: it provides the first spectral-type dependent survey of resonant exozodi structures relevant to future MIR nulling interferometry (LIFE), where previous work was largely limited to Solar analogs. The inclusion of stellar wind drag in the dust equation of motion is physically well motivated, and the paper is unusually transparent about its caveats: the age-dependence of ψ, the uncertain mass-loss scaling for fully convective M dwarfs, and the alternative gyrochronology estimates are all acknowledged in the text and appendices. The timescale comparison in §4.5 is a useful sanity check for the collisionless assumption. The main quantitative headline — that optical-depth contrast increases monotonically toward lower stellar mass — is, however, not robust to the plausible range of the input ψ for M dwarfs, as the paper's own Appendix B.3 shows. The broader qualitative conclusion — that spectral-type-dependent stellar wind matters and resonant structures exist across FGK and M stars — is defensible, but the abstract and §3.2.2 currently state the non-robust ordering as a central result.

major comments (3)

[Abstract & §3.2.2] The abstract and §3.2.2 claim that 'the optical depth contrast of the resonant ring increased for lower-mass stars', citing ⟨Cτ⟩ = 1.95, 5.98, 8.07, 9.85. Appendix B.3 shows that with the alternative Lu et al. (2024) gyrochrone, ψ_M4 ≈ 127 and the semi-analytical estimate gives ⟨Cτ⟩_M4 ≈ 6.9, below K4 (8.07). Since ψ enters the drag as β_PR(1+ψ) (Eq. 5), a factor of ~3 in ψ changes resonant trapping efficiency and the derived contrasts materially. The paper's own Appendix B.3 states that, under this alternative, 'K4-type stars exhibit the highest contrasts'. Thus the monotonic F4→M4 ordering is not robust. The main text should present the ordering as F→K with M dependent on the wind model, or the authors should run the main multi-size simulations with ψ_M4 = 127 and report the resulting ⟨Cτ⟩.
[§3.1.1, §4.1, App. B.3] The load-bearing input ψ_M4 ≈ 44 is obtained by stitching three gyrochronology relations and applying the Johnstone et al. (2015, 2021) mass-loss scaling (Eq. 9). Section 4.1 itself states that this scaling is 'less certain for fully convective M-dwarfs', and no direct observational calibration is provided for old M-dwarf winds. The choice of ψ = 44 is defended only as 'conservative'. Because the headline results — ψ ≈ 44, 'stellar wind halves M4 contrast', and the M4 position in the ordering — all rest on this choice, the manuscript needs a quantitative sensitivity test, not only the semi-analytical estimate in Appendix B.3. At minimum, the pilot study should be repeated with ψ_M4 = 127, and ideally the main study as well, so that the claimed ordering is an actual simulation outcome rather than a model-input selection.
[§4.3, App. B.2/B.3] The semi-analytical contrast function (Eq. 14) is fitted to the same simulation data that it is then used to explain, and its own values for ⟨Cτ⟩ in Appendix B.2 (1.71, 4.40, 5.81, 6.55) are ~30% lower than the direct simulated values in §3.2.2. In Appendix B.3 this same fitted function is used to predict the effect of ψ_M4 = 127 and to conclude that M4 falls below K4. Because the function is an empirical fit rather than a validated theory, and because it under-predicts the direct simulation values, the Appendix B.3 inversion should be labeled as a tentative extrapolation. The distinction between 'direct simulation' and 'semi-analytical estimate' must be made explicit in the main text and abstract, otherwise readers may take the M4-vs-K4 inversion as a simulated result. This concern is separate from the input uncertainty: it is about the weight that can be placed on the sensitivity estim

minor comments (6)

[§3.1.2] Text reads 'the lower contrast of the red points in the right panel of Fig. 3 compared to the left'; Fig. 3 shows ψ values without left/right panels. This should refer to the Model I/Model II panels of Fig. 4.
[Table A.1] The definitions for ⟨QPR⟩ and ⟨QSW⟩ appear swapped: ⟨QPR⟩ is the radiation-pressure efficiency averaged over the stellar spectrum, while ⟨QSW⟩ is the stellar-wind efficiency averaged over wind species. Correct the table entries.
[Abstract / §3.2.2] The phrase 'increased for lower-mass stars' is too strong given the Appendix B.3 caveat. A phrase such as 'increased from F to K, with the low-mass M-type behavior depending on the stellar-wind model' would be more accurate.
[§2.2.1 / §3.1.2] The pilot study uses 100 particles and the text notes that such runs 'can yield unreliable contrast estimates' (citing Stark & Kuchner 2008). The statement that internal 5000-particle tests show consistent trends would be more useful if quantified or shown in an appendix.
[§4.3] The sentence 'the contrast can be described by extending the semi-analytical functional form of Eq. 4 from Stark & Kuchner (2008)' is ambiguous; the intended equation number in the present paper (Eq. 14) should be cited explicitly.
[§3.2.2 / Eq. (12)] The notation τ_BG ≈ 2.1×10^-7 at r=2a_p is consistent with 3 zodis (3 × 7.12×10^-8), but the text states 'the optical depth at r=2a_p is τ_BG≈2.1×10^-7 for all spectral types.' Clarify that this is the assumed constant background level, not a measured value from the simulations.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: stellar-wind ψ is an external input, the headline contrasts are simulation outputs, and the fit-based alternative-gyrochronology estimate is transparently a fit, not an independent prediction.

full rationale

The paper's derivation chain is input → simulation → output. ψ is computed from published gyrochronology relations (Lu et al. 2024; Mamajek & Hillenbrand 2008; Dungee et al. 2022) and the Johnstone et al. (2015, 2021) mass-loss scaling (Eq. 9), all external to this work; it enters the equation of motion (Eq. 5) as an input and is not recovered from the simulations. The headline quantities — ψ≈44, the pilot-study contrasts, the main-study ⟨Cτ⟩ values (1.95, 5.98, 8.07, 9.85), and the asymmetric fluxes — are direct simulation outputs or integrals over the simulated optical-depth maps. The semi-analytical contrast function (Eq. 14) is explicitly fitted to those outputs ('best-fit parameters ... obtained through non-linear least-squares fitting to all simulated contrast values'), so its later use in Appendices B.2–B.3 is interpolation/estimation, not a prediction claimed to be independent; the paper even states that the fit-based ⟨Cτ⟩ values are about 30% smaller than the directly simulated ones. The sensitivity of the K–M ordering to the gyrochronology choice is openly disclosed (Section 3.1.1, Appendix B.3, and Section 5: 'the exact K–M trend depends on rotational evolution and wind environment of M-type stars'), and Section 4.1 openly states that the mass-loss scaling is 'less certain for fully convective M-dwarfs' — a robustness caveat, not a hidden circular step. The only same-author citation (Jo & Ishiguro 2024) concerns the numerical implementation of radiation pressure in the MERCURY6 integrator and is not load-bearing for the physical conclusions. No definition, fitted parameter, or self-citation reduces the claimed results to the paper's own inputs by construction.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The central results rest on one strongly model-dependent input (ψ for M4, with a 44–127 spread), one observationally unconstrained normalization (τ_BG=3 zodis for all stars), and an unstated dust density. No new physical entities are introduced. The simulations themselves are honest about their steady-state, collisionless, most-favorable-for-resonance assumptions.

free parameters (4)

ψ (M4, adopted) = ≈44 (range 44–127 across gyrochronology models)
Ratio of stellar wind drag to PR drag, chosen via the 'conservative' Dungee et al. (2022) gyrochrone rather than Lu et al. (2024), which gives ≈127; the choice determines M4-vs-K4 contrast ordering (§3.1.1, §B.3).
τ_BG (background zodi level) = 3 zodis (27 zodis also checked)
Assumed constant background optical depth for all spectral types from HOSTS median (Ertel et al. 2020); flux and asymmetry maps scale linearly with this choice; M stars unconstrained by HOSTS (§3.2.2).
Dust bulk density ρ = not stated
Appears in Eq. (2) for βPR and in Mie calculation of blowout sizes; never given a numerical value in text or Table A.1, so βPR and sBO,eff are not reproducible from the paper alone.
Stellar wind speed vSW = ≈400 km/s for all spectral types
Fixed to the solar wind value with no spectral-type dependence; enters ψ linearly (Eq. 4) and hence the drag dominance factor (§2.1.1).

assumptions (6)

domain assumption Johnstone et al. (2015, 2021) mass-loss scaling (Eq. 9) with gyrochronology rotation periods determines ψ.
Central to ψ; less certain for fully convective M dwarfs (§4.1).
ad hoc to paper Stellar wind speed is isotropic and equal to 400 km/s for all spectral types.
Adopted from solar wind value; no variation across spectral types (§2.1.1).
domain assumption Dust is collisionless and in steady state with constant replenishment.
Collisional timescale comparison supports it at τ_BG=3 zodis (§4.5), but it maximizes resonant contrast.
domain assumption βr ≈ βPR (neglect ψ vSW/c) for blowout-size derivation.
Valid because ψ < ~1000 (§2.1.3, App. B.1).
domain assumption Main-sequence L∗ ∝ M∗^3.5 and ap ∝ sqrt(L∗) scaling used in contrast trend arguments.
Empirical mass-luminosity relation invoked in Section 4.3.
domain assumption Mie theory with astronomical silicate optical constants (Draine 2003); ⟨QPR⟩=⟨QSW⟩=1 for s≥0.3 µm.
Common practice; the 0.1-µm cases are approximated by larger grains with matched βPR (§2.2.2).

how reviews work

0 comments

Cite this review

Pith. "Pith review of Resonant structures in exozodiacal clouds created by exo-Earths in the habitable zone of late-type stars." pith.science (2026). https://pith.science/paper/LBPLDYSL

@misc{pith2026251117872,
  author       = {Pith},
  title        = {Pith review of: Resonant structures in exozodiacal clouds created by exo-Earths in the habitable zone of late-type stars},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LBPLDYSL}},
  note         = {Machine review of arXiv:2511.17872}
}

read the original abstract

Earth-like exoplanets can create resonant structures in exozodiacal dust through mean motion resonances (MMRs). These structures not only suggest the presence of such planets, but also act as potential noise sources in future mid-infrared (MIR) nulling interferometry observations. We aim to investigate how resonant structures in exozodiacal dust vary across stellar spectral types (F4--M4), and to evaluate how stellar wind drag affects their morphology and brightness in mature planetary systems. We conducted numerical simulations of dust dynamics, extending earlier studies by including spectral type variation in stellar wind drag in addition to Poynting-Robertson (PR) drag. Our models represented systems of a few Gyr hosting an Earth-like exoplanet in the habitable zone (HZ). We produced spatially resolved maps of optical depth and thermal emission for different stellar spectral types. Our simulations showed that resonant ring structures were formed for all stellar spectral types considered. In particular, we found that stellar wind drag played a critical role in shaping dust dynamics around old M-type stars, where it could dominate over PR drag by a factor of approximately 44. This reduced the contrast of resonant rings relative to the background disk, compared to cases without spectral type variation in stellar wind. Across different spectral types, the optical depth contrast of the resonant ring increased for lower-mass stars, assuming a fixed background level. Asymmetric thermal emission distributions were derived across all spectral types, which peaked for K-type stars. Our findings highlight the importance of incorporating both resonant dynamics and stellar wind effects when modeling exozodiacal dust around stars of different spectral types.

Figures

Figures reproduced from arXiv: 2511.17872 by the authors.

**Figure 1.** (Left) Example of face-on surface density distribution of dust in a planet’s co-rotating frame, with a K4-type star located at the origin. The white dot indicates an Earth-like planet placed at the inner boundary of the CHZ. A total of 100 dust particles with a size of 50 µm are used. The resonant ring structure is visible around the planet’s position. The color scale indicates surface density in arbitrary units, wi… view at source ↗

**Figure 2.** ⟨QPR⟩ values for grain sizes s ∼ 0.1–300 µm (left) and the corresponding βPR values (right; analogous to [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗

**Figure 3.** ψ values given by Eqs. (4) and (9) for main-sequence stars of spectral types F4 to M4 at an age of ∼ 4 Gyr (2–3 Gyr for F-type stars). The four spectral types used in this study are marked in blue, green, yellow, and red, respectively. The dashed line shows ψ = 1, where the stellar wind drag equals the PR drag. a few Gyr, systems with stellar masses below ∼ 0.8 M⊙ (approximately K3 type) are more strongly influence… view at source ↗

Figures from the paper (9 more)

**Figure 4.** Figure 4: Contrast values from the pilot study, plotted against the [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]

**Figure 5.** Figure 5: Contrast values from the main study plotted against grain [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]

**Figure 6.** Figure 6: Distributions of optical depth (upper row) and flux (10 µm; lower row) are presented for spectral types F4, G4, K4, and M4, from left to right, assuming a constant τBG ∼ 3 zodis. The star is located at the center, and the planet is marked with a white dot to the right …

**Figure 7.** Figure 7: Stellar rotation period (P∗, left), mass-loss rate (M˙ ∗, middle), and ψ (right) for main-sequence stars of spectral types F4–M4, at age 4 Gyr (2–3 Gyr for F-type). Different symbols/colors show results from the three gyrochronology models, with approximate uncertainti…

**Figure 8.** Figure 8: ψ values given by Eqs. (4) and (9) for main-sequence stars of spectral types F4–M4 at an age of 1 Gyr (empty circles), 4 Gyr (2–3 Gyr for F-type stars; filled circles), and 10 Gyr (empty triangles) using gyrochrones from Lu et al. (2024). For 10 Gyr, only values for s…

**Figure 9.** Figure 9: Flux with central regions masked (10 µm; upper row), and corresponding asymmetric flux relative to the planet flux Fp (lower row), following the format of [PITH_FULL_IMAGE:figures/full_fig_p013_9.png]

**Figure 10.** Figure 10: Maximum value of the resonant ring flux at [PITH_FULL_IMAGE:figures/full_fig_p013_10.png]

**Figure 11.** Figure 11: Comparison of timescales for effective migration driven by PR and stellar wind drag (solid black lines), with the collisional timescale corresponding to the optical depths τBG = 3 and 27 zodis referenced from the HOSTS survey (purple dashed lines; see Sections 3.2.2 a…

**Figure 12.** Figure 12: Comparison of timescales for resonant trapping from simulation data (black dots) with the median values (solid black lines) [PITH_FULL_IMAGE:figures/full_fig_p016_12.png]

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

10 extracted references · 1 linked inside Pith

[1]

2006, PhD thesis, University of Liege, Belgium Baraffe, I., Homeier, D., Allard, F., & Chabrier, G

Absil, O. 2006, PhD thesis, University of Liege, Belgium Baraffe, I., Homeier, D., Allard, F., & Chabrier, G. 2015, A&A, 577, A42 Binks, A. 2016, in IAU Symposium, V ol. 314, Young Stars & Planets Near the Sun, ed. J. H. Kastner, B. Stelzer, & S. A. Metchev, 159–162 Burns, J. A., Lamy, P. L., & Soter, S. 1979, Icarus, 40, 1 Carrión-González, Ó., Kammerer,...

2006
[2]

K4 (yellow) and M4 (red) appear to have one fewer point because their 0.3µm and 1µm data replace the 0.1µm points respectively, causing overlap (see Section 2.2.2)

anda p is fixed, larger x-values indicate larger grains. K4 (yellow) and M4 (red) appear to have one fewer point because their 0.3µm and 1µm data replace the 0.1µm points respectively, causing overlap (see Section 2.2.2). See the caption of Fig. 5 for more details on colors and symbols. A single solid fit line is shown per spectral type, as onlyM p =1M ⊕ ...

2024
[4]

which is comparable to the threshold ψmin,s BO as shown in Fig. B.1. The discrepancy arises because the presentedψ min,s BO values are based on typical main-sequence stellar masses and luminosities, whereas AU Mic is a pre-main- sequence star. Nonetheless, the comparison demonstrates that the highψvalue for AU Mic is sufficient to produce an effective blo...

2005
[7]

Nev- ertheless, the semi-analytical⟨C τ⟩values can be used to approx- imately estimateτ BG·⟨Cτ⟩when the background level of dust is given

and fitting un- certainties, since the function is not entirely reliable for extreme values ofβ PR andM p, as noted by Stark & Kuchner (2008). Nev- ertheless, the semi-analytical⟨C τ⟩values can be used to approx- imately estimateτ BG·⟨Cτ⟩when the background level of dust is given. Thus, the semi-analytical functions remain valuable as a first-order method...

2008
[8]

See the caption of Fig

is used for convenience. See the caption of Fig. 4 for details on colors and symbols. Solid lines show new fits (see Eq. 14 for functional form), truncated to remain within the range relevant to each spectral type for clarity, as the contrast depends on bothM∗ andM p unlike the original fits from Stark & Kuchner (2008). Multiple lines of the same color co...

2008
[10]

In this scenario, exozodi resonant structures in M-type systems would clearly pose the least hindrance on MIR interferometric detection of exo-Earths

In fact, it would reinforce the peak appearing at K-type, since the flux from M4-type sys- tems would further decrease due to their reduced optical depth. In this scenario, exozodi resonant structures in M-type systems would clearly pose the least hindrance on MIR interferometric detection of exo-Earths. This potentially stronger influence of stellar wind...

2020
[11]

F., Jayaraman, S., Xu, Y

Dermott, S. F., Jayaraman, S., Xu, Y . L., Gustafson, B. Å. S., & Liou, J. C. 1994, Nature, 369, 719 Dermott, S. F., Nicholson, P. D., Burns, J. A., & Houck, J. R. 1984, Nature, 312, 505 Dohnanyi, J. S. 1969, J. Geophys. Res., 74, 2531 Draine, B. T. 2003, ARA&A, 41, 241 Dungee, R., van Saders, J., Gaidos, E., et al. 2022, ApJ, 938, 118 Eddington, A. S. 19...

arXiv 1994
[14]

expanded from the formulation of Stark & Kuchner (2008), were used to fit the results presented in Sections 3.1.2 and 3.2.1. Fig. B.2 show the same datasets from the pilot study plotted against the mod- ified expressiona 1/2 p βPR (1+ψ ) −1 M−1/2 ∗ from Eq. (15), along with the improved contrast fits. Since this modifiedx-axis ex- pression increases with ...

2008

Show all 10 references

[2015]

(2005) on a young M0 dwarf AU Mic of∼15 Myr age withM ∗ =0.5M ⊙,L ∗ =1.3L ⊙, assuming vSW ∼400 km/s and ˙M∗ ∼1000 ˙M⊙

and the estima- tion by Plavchan et al. (2005) on a young M0 dwarf AU Mic of∼15 Myr age withM ∗ =0.5M ⊙,L ∗ =1.3L ⊙, assuming vSW ∼400 km/s and ˙M∗ ∼1000 ˙M⊙. This corresponds to a value ofψ∼2308 (Eq

2005
[2024]

This value is derived from observations (e.g., Metchev et al

use the minimum grain size of∼0.25µm for systems without ra- diative blowout sizes. This value is derived from observations (e.g., Metchev et al. 2005; Matthews et al

2005

Pith tools

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

[1] [1]

2006, PhD thesis, University of Liege, Belgium Baraffe, I., Homeier, D., Allard, F., & Chabrier, G

Absil, O. 2006, PhD thesis, University of Liege, Belgium Baraffe, I., Homeier, D., Allard, F., & Chabrier, G. 2015, A&A, 577, A42 Binks, A. 2016, in IAU Symposium, V ol. 314, Young Stars & Planets Near the Sun, ed. J. H. Kastner, B. Stelzer, & S. A. Metchev, 159–162 Burns, J. A., Lamy, P. L., & Soter, S. 1979, Icarus, 40, 1 Carrión-González, Ó., Kammerer,...

2006

[2] [2]

K4 (yellow) and M4 (red) appear to have one fewer point because their 0.3µm and 1µm data replace the 0.1µm points respectively, causing overlap (see Section 2.2.2)

anda p is fixed, larger x-values indicate larger grains. K4 (yellow) and M4 (red) appear to have one fewer point because their 0.3µm and 1µm data replace the 0.1µm points respectively, causing overlap (see Section 2.2.2). See the caption of Fig. 5 for more details on colors and symbols. A single solid fit line is shown per spectral type, as onlyM p =1M ⊕ ...

2024

[3] [4]

which is comparable to the threshold ψmin,s BO as shown in Fig. B.1. The discrepancy arises because the presentedψ min,s BO values are based on typical main-sequence stellar masses and luminosities, whereas AU Mic is a pre-main- sequence star. Nonetheless, the comparison demonstrates that the highψvalue for AU Mic is sufficient to produce an effective blo...

2005

[4] [7]

Nev- ertheless, the semi-analytical⟨C τ⟩values can be used to approx- imately estimateτ BG·⟨Cτ⟩when the background level of dust is given

and fitting un- certainties, since the function is not entirely reliable for extreme values ofβ PR andM p, as noted by Stark & Kuchner (2008). Nev- ertheless, the semi-analytical⟨C τ⟩values can be used to approx- imately estimateτ BG·⟨Cτ⟩when the background level of dust is given. Thus, the semi-analytical functions remain valuable as a first-order method...

2008

[5] [8]

See the caption of Fig

is used for convenience. See the caption of Fig. 4 for details on colors and symbols. Solid lines show new fits (see Eq. 14 for functional form), truncated to remain within the range relevant to each spectral type for clarity, as the contrast depends on bothM∗ andM p unlike the original fits from Stark & Kuchner (2008). Multiple lines of the same color co...

2008

[6] [10]

In this scenario, exozodi resonant structures in M-type systems would clearly pose the least hindrance on MIR interferometric detection of exo-Earths

In fact, it would reinforce the peak appearing at K-type, since the flux from M4-type sys- tems would further decrease due to their reduced optical depth. In this scenario, exozodi resonant structures in M-type systems would clearly pose the least hindrance on MIR interferometric detection of exo-Earths. This potentially stronger influence of stellar wind...

2020

[7] [11]

F., Jayaraman, S., Xu, Y

Dermott, S. F., Jayaraman, S., Xu, Y . L., Gustafson, B. Å. S., & Liou, J. C. 1994, Nature, 369, 719 Dermott, S. F., Nicholson, P. D., Burns, J. A., & Houck, J. R. 1984, Nature, 312, 505 Dohnanyi, J. S. 1969, J. Geophys. Res., 74, 2531 Draine, B. T. 2003, ARA&A, 41, 241 Dungee, R., van Saders, J., Gaidos, E., et al. 2022, ApJ, 938, 118 Eddington, A. S. 19...

arXiv 1994

[8] [14]

expanded from the formulation of Stark & Kuchner (2008), were used to fit the results presented in Sections 3.1.2 and 3.2.1. Fig. B.2 show the same datasets from the pilot study plotted against the mod- ified expressiona 1/2 p βPR (1+ψ ) −1 M−1/2 ∗ from Eq. (15), along with the improved contrast fits. Since this modifiedx-axis ex- pression increases with ...

2008