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arxiv: 2606.08773 · v1 · pith:F3LDTIOZnew · submitted 2026-06-07 · 🌌 astro-ph.SR · astro-ph.HE

Mapping the Landscape of M Dwarf X-ray Flares: New Discoveries in Context

Imri A. Dickstein , Maayane T. Soumagnac , Eran O. Ofek , Param Rekhi , Volker Perdelwitz , Sagi Ben-Ami , Thomas Kupfer This is my paper

Pith reviewed 2026-06-27 17:44 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords M dwarfsX-ray flaresatmospheric escapeexoplanet habitabilityflare frequencyeROSITAChandra
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0 comments X

The pith

M dwarf X-ray flares occur at an average rate of nine per day, implying habitable Earth-like planets lose their atmospheres in 0.5-30 million years.

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

The paper identifies 11 previously unknown X-ray flares on 7 M dwarfs through cross-matching of eROSITA and Chandra data. It assembles a combined sample of flares from 15 M0-M6 stars to measure occurrence rates, energy ranges, durations, and other properties such as flux enhancements and temporal asymmetries. A strong correlation appears between flare strength and duration across energies from 10^29 to 10^33 erg. These observed flare statistics are then combined with existing simulations of flare-driven atmospheric escape to place an upper bound on the time for complete atmosphere loss around habitable planets.

Core claim

We report 11 new X-ray flares from 7 M dwarfs and compile all reported flares from the 15 known flaring M dwarfs in the literature. This yields an average flare rate of approximately 10^{-1} ks^{-1} (roughly 9 flares per day), with events spanning 10^{29} to 10^{33} erg and displaying a clear strength-duration correlation. Incorporating these flare properties into recent simulations of atmospheric escape produces an upper limit of 0.5-30 Myr for the complete loss of atmospheres on habitable Earth-like planets orbiting these stars.

What carries the argument

The compiled sample of X-ray flares from 15 M0-M6 stars, integrated with flare-driven atmospheric escape simulations to derive the cumulative erosion timescale.

If this is right

  • Flares from M0-M6 stars follow a frequency distribution with average rate near 0.1 per kilosecond.
  • Flare energy correlates strongly with duration across four orders of magnitude in energy.
  • Atmospheric loss timescales for habitable planets fall between 0.5 and 30 million years under the derived flare statistics.
  • Temporal asymmetries, flux enhancements, and temperature changes in the flares provide additional constraints on flare physics.

Where Pith is reading between the lines

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

  • Surveys targeting less active M dwarfs may be required to find planets that retain atmospheres long enough for life to develop.
  • Extending the flare sample to fainter or more distant M dwarfs could tighten or revise the 0.5-30 Myr bound.
  • The same flare statistics could be used to model erosion of non-Earth-like atmospheres with different compositions or magnetic shielding.

Load-bearing premise

The observed flare sample combined with the atmospheric-escape simulations accurately captures the total effect on planets across millions of years.

What would settle it

A direct measurement or refined simulation showing that the integrated X-ray energy from flares at the measured rate does not remove an Earth-like atmosphere within 30 Myr.

Figures

Figures reproduced from arXiv: 2606.08773 by Eran O. Ofek, Imri A. Dickstein, Maayane T. Soumagnac, Param Rekhi, Sagi Ben-Ami, Thomas Kupfer, Volker Perdelwitz.

Figure 1
Figure 1. Figure 1: Parent sample: M dwarfs presents in both eROSITA and the Chandra archive. [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The instruments which captured flares from M dwarfs in the X-ray up to the publication date of this work. (2023) [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Left: The Flux measured during the flare, as a function of the flux measured during the quiescent phase (estimated as the minimum of the fluxes measured before and after the flare), for the 11 flares we report. Right: The temperature increase during the flare (defined as the ratio of the temperature measured during the flare to the temperature measured during the quiescent phase), as a function of the flux… view at source ↗
Figure 4
Figure 4. Figure 4: Left panel: A comparison between the flare rise and decay time for our sample (blue) and the literature sample (other colors). We include J. P. Pye et al. (2015) but we note they did not provide error bars. Right panel: the asymmetry of the flare temporal shape as a function of the flare duration [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: shows the distribution of flare energies for the full sample, spanning four orders of magnitude, with a mean energy E = 8.8 × 1031 , erg. 4.5. Correlation between Flare Duration and Flare Strength Long-duration flares are predicted by theoretical mod￾els to exhibit higher energies. Specifically, H. Maehara et al. (2015) predicted a tf lare ∝ E1/3 dependence for solar-type star flares at optical wavelengths… view at source ↗
Figure 6
Figure 6. Figure 6: The correlation between the flare duration and the flare strength. [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Spectral type distribution of the flaring stars identified in this work (yellow) and from the literature (blue) [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Left: The number of observed flares and the exposure time, for all the stars in the full sample for which exposure times are available. Right: zoom-in view of the left panel [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Histogram of the percentage of observing time spent in a flaring state, for all the stars in the combined sample for which flare duration and observing time where provided. and report the best-fit parameters in [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Left panel: the FFD measured for the combined sample (this work+literature), with a power law fit. Right panel: the best fit model we obtain compared with previous measurements of the FFD at other wavelengths. where η is the hydrogen escape efficiency due to the XUV, RXUV is the radius of influence (measured from the center of the planet, which indicates how much the XUV can penetrate into the atmosphere … view at source ↗
Figure 11
Figure 11. Figure 11: Light curves of the flares. All panels share the same x-axis, showing photon arrival times measured from the beginning of each observation. From top to bottom, the panels display: (1) the number of detected photons, (2) the total photon energy per time bin, (3) individual photon energies (keV), and (4) the hardness ratio as defined in §4.1. Regions shaded in orange indicate the time intervals during which… view at source ↗
Figure 12
Figure 12. Figure 12: Evolution of the temperature and flux of the flares [PITH_FULL_IMAGE:figures/full_fig_p017_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Selecting a subsample to minimize biases. [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
read the original abstract

We report the discovery of 11 X-ray flares from 7 M dwarfs previously unknown to exhibit flaring activity, by cross-matching eROSITA observations of bright, nearby M dwarfs with the Chandra telescope archive. To analyze the properties of these flares in a broader context, we compile the sample of all reported X-ray flares from the 15 M dwarfs identified as flaring in the literature. We use this combined sample to derive constraints on the X-ray flare frequency distributions of M0-M6 stars. The average flare occurrence rate we measure is $\sim 10^{-1}\,\rm ks^{-1}$ (corresponding to $\sim 9$ flares per day). The X-ray flares in this sample span energies from $10^{29}\,\rm erg$ to $10^{33}\,\rm erg$ and exhibit a strong correlation between flare strength and duration. The flare properties we characterize include their durations, flux and temperature enhancements, and temporal asymmetries. Using these results and recent simulations of flare-driven atmospheric escape, we derive an upper limit on the time required for habitable Earth-like planets orbiting these M dwarfs to completely lose their atmospheres: 0.5-30 Myr.

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

3 major / 2 minor

Summary. The manuscript reports the discovery of 11 new X-ray flares from 7 M dwarfs via cross-matching eROSITA observations with the Chandra archive. It compiles all reported X-ray flares from a total of 15 M0-M6 dwarfs, measures an average occurrence rate of ~10^{-1} ks^{-1} (~9 flares/day), characterizes flare energies (10^{29}-10^{33} erg), durations, flux/temperature enhancements, and temporal asymmetries, and combines these with recent atmospheric-escape simulations to derive an upper limit of 0.5-30 Myr for complete loss of atmospheres on habitable Earth-like planets orbiting such stars.

Significance. If the flare compilation and integration with escape models are robust, the work supplies a useful observational baseline for M-dwarf flare statistics and quantifies a potentially rapid atmospheric-erosion timescale relevant to exoplanet habitability. The new flare detections and the reported energy-duration correlation constitute concrete additions to the literature.

major comments (3)
  1. [Abstract] Abstract, final paragraph: The 0.5-30 Myr upper limit is stated as following directly from the measured flare rate and 'recent simulations,' yet the text provides no explicit integration steps, no statement of the assumed constant flare rate over 10^6-10^7 yr, and no assessment of whether the 15-star sample remains representative after accounting for stellar evolution or selection biases; this assumption is load-bearing for the numerical bound.
  2. [Sample compilation and rate derivation] Section describing the compiled sample (likely §2-3): The occurrence rate ~10^{-1} ks^{-1} appears to be a direct count from the 15 M dwarfs without reported Poisson uncertainties, completeness corrections, or a fitted frequency distribution; if the central claim of 'constraints on the X-ray flare frequency distributions' rests on this count, the derivation must be shown explicitly (e.g., via cumulative distribution or power-law fit parameters).
  3. [Flare property analysis] Discussion of flare properties: The reported strong correlation between flare strength and duration is used to support the escape calculation, but no quantitative fit (slope, scatter, or significance) or test against selection effects in the Chandra/eROSITA cross-match is provided; this affects whether the energy-duration relation can be extrapolated to the Myr-integrated input.
minor comments (2)
  1. [Abstract] The abstract cites 'recent simulations' without a reference; the main text should supply the specific papers and a brief summary of the escape model assumptions.
  2. [Introduction/Sample section] Notation for units (ks^{-1}, erg) is clear, but the manuscript should state whether the 15-star sample is volume-limited or magnitude-limited and how that affects the quoted average rate.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thoughtful and constructive report. We address each major comment below, indicating revisions where appropriate to strengthen the manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract, final paragraph: The 0.5-30 Myr upper limit is stated as following directly from the measured flare rate and 'recent simulations,' yet the text provides no explicit integration steps, no statement of the assumed constant flare rate over 10^6-10^7 yr, and no assessment of whether the 15-star sample remains representative after accounting for stellar evolution or selection biases; this assumption is load-bearing for the numerical bound.

    Authors: We agree the abstract is too concise on this point. In revision we will expand the final abstract paragraph to briefly outline the integration of the observed flare rate with the escape simulations (cross-referencing the explicit steps already given in Section 4), state the constant-rate assumption, and add a short caveat on sample representativeness and evolutionary biases. The numerical bound itself is unchanged, but its presentation will be more transparent. revision: yes

  2. Referee: [Sample compilation and rate derivation] Section describing the compiled sample (likely §2-3): The occurrence rate ~10^{-1} ks^{-1} appears to be a direct count from the 15 M dwarfs without reported Poisson uncertainties, completeness corrections, or a fitted frequency distribution; if the central claim of 'constraints on the X-ray flare frequency distributions' rests on this count, the derivation must be shown explicitly (e.g., via cumulative distribution or power-law fit parameters).

    Authors: The quoted rate is the simple average (total flares divided by total exposure) across the 15 stars. We will revise §2–3 to report Poisson uncertainties on this average, discuss completeness of the eROSITA–Chandra cross-match, and explicitly show the derivation. Because the sample is heterogeneous we do not attempt a power-law fit, but we will add the cumulative flare-energy distribution to support the frequency-distribution claim. revision: yes

  3. Referee: [Flare property analysis] Discussion of flare properties: The reported strong correlation between flare strength and duration is used to support the escape calculation, but no quantitative fit (slope, scatter, or significance) or test against selection effects in the Chandra/eROSITA cross-match is provided; this affects whether the energy-duration relation can be extrapolated to the Myr-integrated input.

    Authors: We will add a quantitative characterization of the strength–duration correlation (best-fit slope, Pearson coefficient, and significance) in the revised §3, together with a brief assessment of selection effects arising from the cross-match. This will clarify the robustness of using the relation for the Myr-scale extrapolation. revision: yes

Circularity Check

0 steps flagged

No circularity: flare rates are direct counts; atmosphere-loss bound combines observations with external simulations

full rationale

The paper compiles reported X-ray flares from 15 M dwarfs and states the average occurrence rate as a direct measurement (~10^{-1} ks^{-1}) from that sample, with energies and durations likewise taken from the observed events. The 0.5-30 Myr upper limit is obtained by feeding these empirical quantities into separate 'recent simulations' of atmospheric escape; the text does not define any quantity in terms of itself, fit a parameter on a subset then rename the fit as a prediction, or rely on self-citations for the central result. The derivation therefore remains independent of its own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; free parameters, axioms, and invented entities cannot be enumerated from the provided text.

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Works this paper leans on

124 extracted references · 123 canonical work pages · 9 internal anchors

  1. [1]

    Arnaud, K. A. 1996, in Astronomical Society of the Pacific Conference Series, Vol. 101, Astronomical Data Analysis Software and Systems V, ed. G. H. Jacoby & J. Barnes, 17

    1996

  2. [2]

    2021, AJ, 161, 147, doi: 10.3847/1538-3881/abd806

    Demleitner, M., & Andrae, R. 2021, AJ, 161, 147, doi: 10.3847/1538-3881/abd806

    work page internal anchor Pith review doi:10.3847/1538-3881/abd806 2021

  3. [3]

    2018, AJ, 156, 58, doi: 10.3847/1538-3881/aacb21

    Mantelet, G., & Andrae, R. 2018, AJ, 156, 58, doi: 10.3847/1538-3881/aacb21

    work page doi:10.3847/1538-3881/aacb21 2018

  4. [4]

    2018, A&A, 619, A177, doi: 10.1051/0004-6361/201834062

    Baraffe, I., & Chabrier, G. 2018, A&A, 619, A177, doi: 10.1051/0004-6361/201834062

    work page doi:10.1051/0004-6361/201834062 2018

  5. [5]

    J., Hawley, S

    Bochanski, J. J., Hawley, S. L., Covey, K. R., et al. 2010, AJ, 139, 2679, doi: 10.1088/0004-6256/139/6/2679

    work page doi:10.1088/0004-6256/139/6/2679 2010

  6. [6]

    arXiv , author =:2106.14517 , journal =

    Brunner, H., Liu, T., Lamer, G., et al. 2022, A&A, 661, A1, doi: 10.1051/0004-6361/202141266

    work page doi:10.1051/0004-6361/202141266 2022

  7. [7]

    2014, Statistics and Computing, 26, 383–392, doi: 10.1007/s11222-014-9512-y

    Buchner, J. 2016, Statistics and Computing, 26, 383, doi: 10.1007/s11222-014-9512-y

    work page doi:10.1007/s11222-014-9512-y 2016

  8. [8]

    2019, Publications of the Astronomical Society of the Pacific, 131, 108005, doi: 10.1088/1538-3873/aae7fc

    Buchner, J. 2019, PASP, 131, 108005, doi: 10.1088/1538-3873/aae7fc

    work page doi:10.1088/1538-3873/aae7fc 2019

  9. [9]

    2021, Journal of Open Source Software, 6, 3001, doi: 10.21105/joss.03001

    Buchner, J. 2021, The Journal of Open Source Software, 6, 3001, doi: 10.21105/joss.03001

    work page doi:10.21105/joss.03001 2021

  10. [10]

    2025, A&A, 702, A112, doi: 10.1051/0004-6361/202555738

    Caldiroli, A., Haardt, F., Gallo, E., et al. 2025, A&A, 702, A112, doi: 10.1051/0004-6361/202555738

    work page doi:10.1051/0004-6361/202555738 2025

  11. [11]

    1979, ApJ, 228, 939, doi: 10.1086/156922

    Cash, W. 1979, ApJ, 228, 939, doi: 10.1086/156922

    work page doi:10.1086/156922 1979

  12. [12]

    A., Mullan, D

    Cassak, P. A., Mullan, D. J., & Shay, M. A. 2008, ApJL, 676, L69, doi: 10.1086/587055

    work page doi:10.1086/587055 2008

  13. [13]

    Structure and evolution of low-mass stars

    Chabrier, G., & Baraffe, I. 1997, A&A, 327, 1039, doi: 10.48550/arXiv.astro-ph/9704118

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9704118 1997

  14. [14]

    R., et al

    Chavali, S., Youngblood, A., Paudel, R. R., et al. 2022, Research Notes of the American Astronomical Society, 6, 201, doi: 10.3847/2515-5172/ac9591

    work page doi:10.3847/2515-5172/ac9591 2022

  15. [15]

    Lin, R. P. 2008, ApJ, 677, 1385, doi: 10.1086/529011

    work page doi:10.1086/529011 2008

  16. [16]

    R., Hawley, S

    Covey, K. R., Hawley, S. L., Bochanski, J. J., et al. 2008, AJ, 136, 1778, doi: 10.1088/0004-6256/136/5/1778

    work page doi:10.1088/0004-6256/136/5/1778 2008

  17. [17]

    M., & Cameron, C

    Matthews, J. M., & Cameron, C. 2016, ApJL, 829, L31, doi: 10.3847/2041-8205/829/2/L31 do Amaral, L. N. R., Shkolnik, E. L., Loyd, R. O. P., &

    work page doi:10.3847/2041-8205/829/2/l31 2016

  18. [18]

    2025, ApJ, 985, 100, doi: 10.3847/1538-4357/adc932

    Peacock, S. 2025, ApJ, 985, 100, doi: 10.3847/1538-4357/adc932

    work page doi:10.3847/1538-4357/adc932 2025

  19. [19]

    G., & Wu, K

    Doyle, L., Ramsay, G., Doyle, J. G., & Wu, K. 2019, MNRAS, 489, 437, doi: 10.1093/mnras/stz2205

    work page doi:10.1093/mnras/stz2205 2019

  20. [20]

    V., Kulikov, Y

    Erkaev, N. V., Kulikov, Y. N., Lammer, H., et al. 2007, A&A, 472, 329, doi: 10.1051/0004-6361:20066929

    work page doi:10.1051/0004-6361:20066929 2007

  21. [21]

    arXiv , author =:2407.10799 , journal =

    Evans, I. N., Evans, J. D., Mart´ ınez-Galarza, J. R., et al. 2024, ApJS, 274, 22, doi: 10.3847/1538-4365/ad6319

    work page doi:10.3847/1538-4365/ad6319 2024

  22. [22]

    An extreme X-ray flare observed on EV Lac by ASCA in July 1998

    Favata, F., Reale, F., Micela, G., et al. 2000, A&A, 353, 987, doi: 10.48550/arXiv.astro-ph/9909491

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9909491 2000

  23. [23]

    W., Million, C., Osten, R

    Fleming, S. W., Million, C., Osten, R. A., Kolotkov, D. Y., & Brasseur, C. E. 2022, ApJ, 928, 8, doi: 10.3847/1538-4357/ac5037

    work page doi:10.3847/1538-4357/ac5037 2022

  24. [24]

    C., Redfield, S., & Slavin, J

    Frisch, P. C., Redfield, S., & Slavin, J. D. 2011, ARA&A, 49, 237, doi: 10.1146/annurev-astro-081710-102613

    work page doi:10.1146/annurev-astro-081710-102613 2011

  25. [25]

    S., Kowalski, A., France, K., et al

    Froning, C. S., Kowalski, A., France, K., et al. 2019, ApJL, 871, L26, doi: 10.3847/2041-8213/aaffcd

    work page doi:10.3847/2041-8213/aaffcd 2019

  26. [26]

    C., Allen, G

    Fruscione, A., McDowell, J. C., Allen, G. E., et al. 2006, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 6270, Observatory Operations: Strategies, Processes, and Systems, ed. D. R. Silva & R. E. Doxsey, 62701V, doi: 10.1117/12.671760

    work page doi:10.1117/12.671760 2006

  27. [27]

    2011, A&A, 534, A133, doi: 10.1051/0004-6361/201117447

    Fuhrmeister, B., Lalitha, S., Poppenhaeger, K., et al. 2011, A&A, 534, A133, doi: 10.1051/0004-6361/201117447

    work page doi:10.1051/0004-6361/201117447 2011

  28. [28]

    Fuhrmeister, B., Liefke, C., & Schmitt, J. H. M. M. 2007, A&A, 468, 221, doi: 10.1051/0004-6361:20066229 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018a, A&A, 616, A1, doi: 10.1051/0004-6361/201833051 Gaia Collaboration, Babusiaux, C., van Leeuwen, F., et al. 2018b, A&A, 616, A10, doi: 10.1051/0004-6361/201832843 Gaia Collaboration, Valle...

    work page doi:10.1051/0004-6361:20066229 2007

  29. [29]

    , keywords =

    Gehrels, N. 1986, ApJ, 303, 336, doi: 10.1086/164079

    work page doi:10.1086/164079 1986

  30. [30]

    Gershberg, R. E. 1972, Ap&SS, 19, 75, doi: 10.1007/BF00643168

    work page doi:10.1007/bf00643168 1972

  31. [31]

    L., Grießmeier, J.-M., von Paris, P., et al

    Grenfell, J. L., Grießmeier, J.-M., von Paris, P., et al. 2012, Astrobiology, 12, 1109, doi: 10.1089/ast.2011.0682 G¨ udel, M. 2004, A&A Rv, 12, 71, doi: 10.1007/s00159-004-0023-2 G¨ udel, M., & Naz´ e, Y. 2009, A&A Rv, 17, 309, doi: 10.1007/s00159-009-0022-4

    work page doi:10.1089/ast.2011.0682 2012

  32. [32]

    F., Engle, S

    Guinan, E. F., Engle, S. G., & Durbin, A. 2016, ApJ, 821, 81, doi: 10.3847/0004-637X/821/2/81 G¨ unther, M. N., Zhan, Z., Seager, S., et al. 2020, AJ, 159, 60, doi: 10.3847/1538-3881/ab5d3a

    work page doi:10.3847/0004-637x/821/2/81 2016

  33. [33]

    L., Davenport, J

    Hawley, S. L., Davenport, J. R. A., Kowalski, A. F., et al. 2014, ApJ, 797, 121, doi: 10.1088/0004-637X/797/2/121

    work page internal anchor Pith review doi:10.1088/0004-637x/797/2/121 2014

  34. [34]

    L., Walkowicz, L

    Hawley, S. L., Walkowicz, L. M., Allred, J. C., & Valenti, J. A. 2007, PASP, 119, 67, doi: 10.1086/510561 Høg, E., Fabricius, C., Makarov, V. V., et al. 2000, A&A, 355, L27

    work page doi:10.1086/510561 2007

  35. [35]

    S., Corbett, H., Law, N

    Howard, W. S., Corbett, H., Law, N. M., et al. 2019, ApJ, 881, 9, doi: 10.3847/1538-4357/ab2767

    work page doi:10.3847/1538-4357/ab2767 2019

  36. [36]

    M., Hilton, E

    Hunt-Walker, N. M., Hilton, E. J., Kowalski, A. F., Hawley, S. L., & Matthews, J. M. 2012, PASP, 124, 545, doi: 10.1086/666495 23

    work page doi:10.1086/666495 2012

  37. [37]

    2024, A&A, 687, A138, doi: 10.1051/0004-6361/202449541

    Ilin, E., Poppenh¨ ager, K., Stelzer, B., & Dsouza, D. 2024, A&A, 687, A138, doi: 10.1051/0004-6361/202449541

    work page doi:10.1051/0004-6361/202449541 2024

  38. [38]

    2024, PASJ, 76, 175, doi: 10.1093/pasj/psae001

    Inoue, S., Enoto, T., Namekata, K., et al. 2024, PASJ, 76, 175, doi: 10.1093/pasj/psae001

    work page doi:10.1093/pasj/psae001 2024

  39. [39]

    2009, in American Institute of Physics Conference Series, Vol

    Irwin, J., Charbonneau, D., Nutzman, P., & Falco, E. 2009, in American Institute of Physics Conference Series, Vol. 1094, 15th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, ed. E. Stempels, 445–448, doi: 10.1063/1.3099143 Ivezi´ c,ˇZ., Kahn, S. M., Tyson, J. A., et al. 2019, ApJ, 873, 111, doi: 10.3847/1538-4357/ab042c

    work page doi:10.1063/1.3099143 2009

  40. [40]

    M., Kitchatinov, L

    Katsova, M. M., Kitchatinov, L. L., Livshits, M. A., et al. 2018, Astronomy Reports, 62, 72, doi: 10.1134/S106377291801002X

    work page doi:10.1134/s106377291801002x 2018

  41. [41]

    and Bean, Jacob L

    Kempton, E. M.-R., Bean, J. L., Louie, D. R., et al. 2018, PASP, 130, 114401, doi: 10.1088/1538-3873/aadf6f

    work page doi:10.1088/1538-3873/aadf6f 2018

  42. [42]

    2021, A&A, 646, A34, doi: 10.1051/0004-6361/202039003

    Koller, F., Leitzinger, M., Temmer, M., et al. 2021, A&A, 646, A34, doi: 10.1051/0004-6361/202039003

    work page doi:10.1051/0004-6361/202039003 2021

  43. [43]

    K., Ramirez, R

    Kopparapu, R. K., Ramirez, R. M., SchottelKotte, J., et al. 2014, ApJL, 787, L29, doi: 10.1088/2041-8205/787/2/L29

    work page doi:10.1088/2041-8205/787/2/l29 2014

  44. [44]

    K., Ramirez, R., Kasting, J

    Kopparapu, R. K., Ramirez, R., Kasting, J. F., et al. 2013, ApJ, 765, 131, doi: 10.1088/0004-637X/765/2/131

    work page doi:10.1088/0004-637x/765/2/131 2013

  45. [45]

    T., Yelle, R

    Koskinen, T. T., Yelle, R. V., Harris, M. J., & Lavvas, P. 2013, Icarus, 226, 1695, doi: 10.1016/j.icarus.2012.09.026

    work page doi:10.1016/j.icarus.2012.09.026 2013

  46. [46]

    Kowalski, A. F. 2024, Living Reviews in Solar Physics, 21, 1, doi: 10.1007/s41116-024-00039-4

    work page doi:10.1007/s41116-024-00039-4 2024

  47. [47]

    P., & Hilton, E

    Wisniewski, J. P., & Hilton, E. J. 2010, ApJL, 714, L98, doi: 10.1088/2041-8205/714/1/L98

    work page doi:10.1088/2041-8205/714/1/l98 2010

  48. [48]

    F., Wisniewski, J

    Kowalski, A. F., Wisniewski, J. P., Hawley, S. L., et al. 2019, ApJ, 871, 167, doi: 10.3847/1538-4357/aaf058

    work page doi:10.3847/1538-4357/aaf058 2019

  49. [49]

    A., Karakotov, R

    Kuznetsov, A. A., Karakotov, R. R., Chandrashekhar, K., & Banerjee, D. 2023, Research in Astronomy and Astrophysics, 23, 015006, doi: 10.1088/1674-4527/aca190

    work page doi:10.1088/1674-4527/aca190 2023

  50. [50]

    A., & Kolotkov, D

    Kuznetsov, A. A., & Kolotkov, D. Y. 2021, ApJ, 912, 81, doi: 10.3847/1538-4357/abf569

    work page doi:10.3847/1538-4357/abf569 2021

  51. [51]

    2018, A&A, 616, A132, doi: 10.1051/0004-6361/201832832

    Lallement, R., Capitanio, L., Ruiz-Dern, L., et al. 2018, A&A, 616, A132, doi: 10.1051/0004-6361/201832832

    work page doi:10.1051/0004-6361/201832832 2018

  52. [52]

    Lammer, H., Lichtenegger, H. I. M., Kulikov, Y. N., et al. 2007, Astrobiology, 7, 185, doi: 10.1089/ast.2006.0128 L´ epine, S., & Gaidos, E. 2011, AJ, 142, 138, doi: 10.1088/0004-6256/142/4/138

    work page doi:10.1089/ast.2006.0128 2007

  53. [53]

    Liefke, C., Fuhrmeister, B., & Schmitt, J. H. M. M. 2010, A&A, 514, A94, doi: 10.1051/0004-6361/201014012

    work page doi:10.1051/0004-6361/201014012 2010

  54. [54]

    Loredo, T. J. 1992, in Statistical Challenges in Modern Astronomy, ed. E. D. Feigelson & G. J. Babu, 275–297, doi: 10.1007/978-1-4613-9290-3 31

    work page doi:10.1007/978-1-4613-9290-3 1992

  55. [55]

    Loyd, R. O. P., Shkolnik, E. L., Schneider, A. C., et al. 2018a, ApJ, 867, 70, doi: 10.3847/1538-4357/aae2ae

    work page doi:10.3847/1538-4357/aae2ae

  56. [56]

    Loyd, R. O. P., France, K., Youngblood, A., et al. 2018b, ApJ, 867, 71, doi: 10.3847/1538-4357/aae2bd

    work page doi:10.3847/1538-4357/aae2bd

  57. [57]

    2015, Astrobiology, 15, 119, doi: 10.1089/ast.2014.1231

    Luger, R., & Barnes, R. 2015, Astrobiology, 15, 119, doi: 10.1089/ast.2014.1231

    work page doi:10.1089/ast.2014.1231 2015

  58. [58]

    2015, Astrobiology, 15, 57, doi: 10.1089/ast.2014.1215

    Luger, R., Barnes, R., Lopez, E., et al. 2015, Astrobiology, 15, 57, doi: 10.1089/ast.2014.1215

    work page doi:10.1089/ast.2014.1215 2015

  59. [59]

    2015, Earth, Planets and Space, 67, 59, doi: 10.1186/s40623-015-0217-z

    Maehara, H., Shibayama, T., Notsu, Y., et al. 2015, Earth, Planets and Space, 67, 59, doi: 10.1186/s40623-015-0217-z

    work page doi:10.1186/s40623-015-0217-z 2015

  60. [60]

    2022, A&A, 661, A29, doi: 10.1051/0004-6361/202141617

    Magaudda, E., Stelzer, B., Raetz, S., et al. 2022, A&A, 661, A29, doi: 10.1051/0004-6361/202141617

    work page doi:10.1051/0004-6361/202141617 2022

  61. [61]

    2007, ApJ, 660, 1462, doi: 10.1086/513088

    Maggio, A., Flaccomio, E., Favata, F., et al. 2007, ApJ, 660, 1462, doi: 10.1086/513088

    work page doi:10.1086/513088 2007

  62. [62]

    W., Feiden, G

    Mann, A. W., Feiden, G. A., Gaidos, E., Boyajian, T., & von Braun, K. 2015, ApJ, 804, 64, doi: 10.1088/0004-637X/804/1/64

    work page doi:10.1088/0004-637x/804/1/64 2015

  63. [63]

    W., Feiden, G

    Mann, A. W., Feiden, G. A., Gaidos, E., Boyajian, T., & von Braun, K. 2016, ApJ, 819, 87, doi: 10.3847/0004-637X/819/1/87

    work page doi:10.3847/0004-637x/819/1/87 2016

  64. [64]

    D., Wycoff, G

    Mason, B. D., Wycoff, G. L., Hartkopf, W. I., Douglass, G. G., & Worley, C. E. 2001, AJ, 122, 3466, doi: 10.1086/323920

    work page doi:10.1086/323920 2001

  65. [65]

    S., Reinhard, C

    Meadows, V. S., Reinhard, C. T., Arney, G. N., et al. 2018, Astrobiology, 18, 630, doi: 10.1089/ast.2017.1727

    work page doi:10.1089/ast.2017.1727 2018

  66. [66]

    , keywords =

    Miller, A. A., Abrams, N. S., Aldering, G., et al. 2025, PASP, 137, 094204, doi: 10.1088/1538-3873/ae02c5

    work page doi:10.1088/1538-3873/ae02c5 2025

  67. [67]

    K., Williams, D

    Mitra-Kraev, U., Harra, L. K., Williams, D. R., & Kraev, E. 2005a, A&A, 436, 1041, doi: 10.1051/0004-6361:20052834

    work page doi:10.1051/0004-6361:20052834

  68. [68]

    K., G¨ udel, M., et al

    Mitra-Kraev, U., Harra, L. K., G¨ udel, M., et al. 2005b, A&A, 431, 679, doi: 10.1051/0004-6361:20041201

    work page doi:10.1051/0004-6361:20041201

  69. [69]

    2019, ApJ, 870, 10, doi: 10.3847/1538-4357/aaee64

    Mondrik, N., Newton, E., Charbonneau, D., & Irwin, J. 2019, ApJ, 870, 10, doi: 10.3847/1538-4357/aaee64

    work page doi:10.3847/1538-4357/aaee64 2019

  70. [70]

    A., Queloz, D., Gillon, M., et al

    Murray, C. A., Queloz, D., Gillon, M., et al. 2022, MNRAS, 513, 2615, doi: 10.1093/mnras/stac1078

    work page doi:10.1093/mnras/stac1078 2022

  71. [71]

    A., Chiang, E

    Murray-Clay, R. A., Chiang, E. I., & Murray, N. 2009, ApJ, 693, 23, doi: 10.1088/0004-637X/693/1/23

    work page doi:10.1088/0004-637x/693/1/23 2009

  72. [72]

    2020, PASJ, 72, 68, doi: 10.1093/pasj/psaa051

    Namekata, K., Maehara, H., Sasaki, R., et al. 2020, PASJ, 72, 68, doi: 10.1093/pasj/psaa051

    work page doi:10.1093/pasj/psaa051 2020

  73. [73]

    R., Irwin, J., Charbonneau, D., et al

    Newton, E. R., Irwin, J., Charbonneau, D., et al. 2017, ApJ, 834, 85, doi: 10.3847/1538-4357/834/1/85

    work page doi:10.3847/1538-4357/834/1/85 2017

  74. [74]

    A., & Shue, D

    Nousek, J. A., & Shue, D. R. 1989, ApJ, 342, 1207, doi: 10.1086/167676

    work page doi:10.1086/167676 1989

  75. [75]

    A., Hawley, S

    Osten, R. A., Hawley, S. L., Allred, J. C., Johns-Krull, C. M., & Roark, C. 2005, ApJ, 621, 398, doi: 10.1086/427275

    work page doi:10.1086/427275 2005

  76. [76]

    A., Godet, O., Drake, S., et al

    Osten, R. A., Godet, O., Drake, S., et al. 2010, ApJ, 721, 785, doi: 10.1088/0004-637X/721/1/785

    work page doi:10.1088/0004-637x/721/1/785 2010

  77. [77]

    C., & Szapudi, I

    Pandey, J. C., & Singh, K. P. 2008, MNRAS, 387, 1627, doi: 10.1111/j.1365-2966.2008.13342.x 24

    work page doi:10.1111/j.1365-2966.2008.13342.x 2008

  78. [78]

    L., Siemiginowska, A., et al

    Park, T., Kashyap, V. L., Siemiginowska, A., et al. 2006, ApJ, 652, 610, doi: 10.1086/507406

    work page doi:10.1086/507406 2006

  79. [79]

    Parker, E. N. 1993, ApJ, 408, 707, doi: 10.1086/172631

    work page doi:10.1086/172631 1993

  80. [80]

    Intrinsic Colors, Temperatures, and Bolometric Corrections of Pre-Main Sequence Stars

    Pecaut, M. J., & Mamajek, E. E. 2013, ApJS, 208, 9, doi: 10.1088/0067-0049/208/1/9

    work page internal anchor Pith review doi:10.1088/0067-0049/208/1/9 2013

Showing first 80 references.