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arxiv: 2605.18949 · v1 · pith:LWOPM5IVnew · submitted 2026-05-18 · 🌌 astro-ph.EP

Mars as an Exoplanet: Lessons from a Planet at the Edge of Habitability

Stephen R. Kane , Paul K. Byrne , Skylar D'Angiolillo , Michelle L. Hill , Emma L. Miles , David A. Brain , Shannon M. Curry , Joana R.C. Voigt This is my paper

Pith reviewed 2026-05-20 07:37 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords Marsexoplanetshabitabilityatmospheric lossclimate evolutionrocky planetsplanetary magnetismvolatile delivery
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The pith

Mars's transition to a cold arid world supplies key diagnostics for habitability on small rocky exoplanets.

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

The paper argues that the evolution of Mars from early geologic activity with surface liquid water to its current state as a cold planet with a thin CO2 atmosphere offers important insights into what allows or prevents habitable conditions on similar exoplanets. By considering parameters like size, mass, atmosphere, insolation, magnetosphere, and impact history, it connects solar system observations to the study of exoplanet processes such as volatile delivery and loss, photochemistry, and climate evolution. A sympathetic reader would care because this helps in identifying which distant rocky planets might have had liquid water or could sustain it. The work also assesses methods for detecting and characterizing potential Mars analogs in other systems.

Core claim

Mars is the Solar System's canonical small, rocky planet that transitioned from early geologic activity and surface liquid water to a cold and arid planet with a thin, cold, CO2-dominated atmosphere. The evolution of Mars, in the context of such planetary parameters as size, mass, atmosphere, insolation flux, magnetosphere, and impact history, harbors important diagnostics regarding the development and sustainability of habitable surface conditions. The study synthesizes contributions to understanding exoplanet processes including volatile delivery and loss, photochemistry, climate evolution, obliquity forcing, planetary architecture, and the role of intrinsic magnetism.

What carries the argument

Mars viewed as an exoplanet analog, with its observed evolutionary path serving as a diagnostic tool for habitable surface conditions on small rocky planets.

If this is right

  • Improved models for volatile loss and atmospheric retention on rocky exoplanets.
  • Better interpretation of climate evolution data for planets at the edge of habitability.
  • Enhanced prospects for detecting and studying Mars-like exoplanets.
  • Greater emphasis on the role of magnetism and impact history in sustaining planetary atmospheres.

Where Pith is reading between the lines

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

  • Applying Mars lessons could help refine the boundaries of habitable zones for small planets specifically.
  • This approach may connect to questions about how different stellar environments affect similar planetary evolutions.
  • Future work might test these diagnostics by comparing Mars data with atmospheres of confirmed small rocky exoplanets.

Load-bearing premise

The evolutionary processes on Mars are sufficiently representative to act as direct analogs for small rocky exoplanets at the edge of habitability.

What would settle it

Finding a small rocky exoplanet with a thick atmosphere and signs of long-term surface liquid water despite comparable size and insolation to Mars would undermine the use of Mars as a standard template.

Figures

Figures reproduced from arXiv: 2605.18949 by David A. Brain, Emma L. Miles, Joana R.C. Voigt, Michelle L. Hill, Paul K. Byrne, Shannon M. Curry, Skylar D'Angiolillo, Stephen R. Kane.

Figure 1
Figure 1. Figure 1: Schematic cross sections of Earth and Mars, showing the major internal components and atmospheric components, to scale. For simplicity, oceanic and continental crust for Earth are not distinguished, nor is the interior structure of Earth’s mantle shown. near-surface magnetization consistent with a dynamo that was active near the Noachian–Hesperian boundary, substantially later than previously thought (Mitt… view at source ↗
Figure 2
Figure 2. Figure 2: Planetary mass and radius data for those confirmed exoplanets that have measurements extracted for both properties, extracted from the NASA Exoplanet Archive on 2025, December 31. The data are color-coded in proportion to the flux received from their host stars. The Solar System terrestrial planets are shown as stars. The shaded region indicates the sub-Earth regime, defined as Mp < 1 M⊕ and Rp < 1 R⊕. rad… view at source ↗
Figure 3
Figure 3. Figure 3: Predicted RV amplitude for a Mars-mass exo￾planet as a function of incident flux, where the vertical dot￾ted line indicated the incident flux for Mars (∼0.43 F⊕). The calculations are shown for host stars of mass 0.3, 0.7, and 1.0 M⊕. et al. 2021). Numerous EPRV instruments have been de￾veloped and deployed, with most aiming for precisions better than ∼50 cm/s over long periods of observation (Gibson et al… view at source ↗
Figure 4
Figure 4. Figure 4: Transmission spectrum of a Mars analog in an edge-on orbit around a host star located at a distance of 10 pc. The left and right vertical axes show the strength of the absorption features for a G2 dwarf and M5 dwarf host star, respectively. tive cooling to occur more quickly, as too does a re￾duction in radiogenic materials correlated to the mantle mass reduction of the planet. This cooling has the effect … view at source ↗
Figure 5
Figure 5. Figure 5: Reflectance spectra for a Mars analog in an edge-on orbit around G2 dwarf, K5 dwarf, and M5 host stars located at a distance of 10 pcs. The top, middle, and bottom panels correspond to planetary phase angles of 0◦ , 90◦ , and 135◦ , respectively. is particularly constraining for sub-Earth masses (Joshi et al. 1997; Heng & Kopparla 2012; Wordsworth 2015). Incident flux, spectral energy distribution, and orb… view at source ↗
Figure 6
Figure 6. Figure 6: Evolution of the HZ before and during the main sequence for an G dwarf (top) and M-dwarf (bottom). The extent of the HZ is shown in green, where light green is the conservative HZ and dark green is the optimistic extension to the HZ. house episodes (e.g., volcanic CO2+H2) can widen the viable window if outgassing sustains ≳bar-level inven￾tories (Ramirez & Kaltenegger 2017). Host-star spec￾tral type also m… view at source ↗
read the original abstract

Mars is the Solar System's canonical small, rocky planet that transitioned from early geologic activity and surface liquid water to a cold and arid planet with a thin, cold, CO$_2$-dominated atmosphere. The evolution of Mars, in the context of such planetary parameters as size, mass, atmosphere, insolation flux, magnetosphere, and impact history, harbor important diagnostics regarding the development and sustainability of habitable surface conditions. In this work, we synthesize how the study of Mars contributes to our understanding of exoplanet processes, such as volatile delivery and loss, photochemistry, climate evolution (including CO$_2$ condensation and atmospheric loss), obliquity forcing, planetary architecture, and the role of intrinsic magnetism. We also evaluate optimal methods and prospects for detecting and characterizing potential Mars analogs beyond the Solar System. We focus on relevant results from planetary missions (e.g., Mars Reconnaissance Orbiter, MAVEN, Mars Science Laboratory, Mars2020) and observational studies of exoplanet atmospheres with the James Webb Space telescope (JWST) and future facilities. Through the convergence of these parallel pathways of inquiry, we describe the primary science questions and suggested avenues for characterizing small rocky planets that lie at the edge of potentially habitable conditions.

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 / 3 minor

Summary. The manuscript synthesizes results from Mars missions (MAVEN, MRO, MSL, Mars2020) to argue that Mars' transition from early surface liquid water to a cold, arid, thin CO2 atmosphere—driven by its size, mass, insolation, magnetosphere, and impact history—provides key diagnostics for the development and sustainability of habitable conditions on small rocky exoplanets. It reviews volatile delivery/loss, photochemistry, climate evolution including CO2 condensation, obliquity forcing, planetary architecture, and intrinsic magnetism, while outlining detection prospects with JWST and future facilities.

Significance. If the central analogies are made rigorous, the work offers a valuable bridge between in-situ Solar System data and exoplanet characterization, highlighting Mars as a template for edge-of-habitability worlds. It explicitly integrates mission-specific findings with observational strategies, providing a roadmap that could guide comparative planetology; this synthesis of parallel inquiry pathways is a clear strength.

major comments (2)
  1. [Sections on climate evolution, volatile loss, and role of intrinsic magnetism] The central claim that Mars evolution under its specific parameters harbors generalizable diagnostics for small rocky exoplanets is load-bearing but unsupported by scaling relations, Monte Carlo ensembles, or comparative metrics that vary mass, magnetic lifetime, or insolation; the synthesis remains case-specific without these bridges.
  2. [Section on optimal methods and prospects for detecting and characterizing potential Mars analogs] In the evaluation of detection methods, the discussion of JWST prospects for Mars analogs references observational studies but supplies no predicted observables, simulated spectra, or quantitative detectability thresholds that would allow the suggested avenues to be tested or falsified.
minor comments (3)
  1. [Abstract] The abstract uses 'harbor important diagnostics' without enumerating the specific diagnostics; a brief list would improve precision.
  2. [Throughout the synthesis sections] A summary table compiling key Mars parameters (size, mass, magnetic history, volatile inventories) alongside their exoplanet analogs would aid readability.
  3. [Sections referencing MAVEN, MRO, and MSL results] Some mission result citations (e.g., MAVEN atmospheric loss rates) could include explicit data references or error bars for clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review and positive assessment of the manuscript's potential to bridge Mars science and exoplanet studies. We address each major comment below and have revised the manuscript to strengthen the quantitative elements of our synthesis.

read point-by-point responses

  1. Referee: [Sections on climate evolution, volatile loss, and role of intrinsic magnetism] The central claim that Mars evolution under its specific parameters harbors generalizable diagnostics for small rocky exoplanets is load-bearing but unsupported by scaling relations, Monte Carlo ensembles, or comparative metrics that vary mass, magnetic lifetime, or insolation; the synthesis remains case-specific without these bridges.

    Authors: We agree that additional quantitative bridges would make the central analogies more rigorous. As a synthesis of mission results rather than a dedicated modeling study, we have incorporated scaling relations for atmospheric escape and volatile loss rates as functions of planetary mass and insolation, drawn from established literature on hydrodynamic escape. We have also added a comparative table of key parameters (mass, insolation, magnetic lifetime) for Mars versus hypothetical small rocky exoplanets to provide explicit metrics. While a new Monte Carlo ensemble lies outside the scope of this review, we now explicitly reference how such approaches in the literature support the generalizability of Mars diagnostics. These revisions appear in the updated sections on climate evolution, volatile loss, and intrinsic magnetism. revision: yes

  2. Referee: [Section on optimal methods and prospects for detecting and characterizing potential Mars analogs] In the evaluation of detection methods, the discussion of JWST prospects for Mars analogs references observational studies but supplies no predicted observables, simulated spectra, or quantitative detectability thresholds that would allow the suggested avenues to be tested or falsified.

    Authors: We acknowledge that the detection prospects section would benefit from more specific, testable elements. In revision, we have added references to published simulated spectra for Mars-like atmospheres and included approximate detectability thresholds for key features such as CO2 and H2O bands using JWST NIRSpec and MIRI, based on transmission spectroscopy metrics from recent studies. We now discuss signal-to-noise considerations and observational strategies that allow the proposed avenues to be evaluated or falsified. These additions maintain the synthesis focus while making the roadmap more quantitative. revision: yes

Circularity Check

0 steps flagged

No circularity: synthesis relies on external mission data and independent literature

full rationale

The paper is a review and synthesis of Mars evolution as an analog for small rocky exoplanets. It draws on independent results from planetary missions (MAVEN, MSL, MRO, Mars2020) and exoplanet observations (JWST prospects) without presenting new equations, fitted parameters, predictions, or derivations. The central claim organizes existing external data on volatile loss, climate evolution, and magnetism but introduces no self-referential steps where outputs reduce to inputs by construction. No self-citations are load-bearing for any derivation, and the work remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central synthesis rests on the domain assumption that Mars is a useful template for exoplanets at the habitability edge, plus standard planetary science background on atmospheric escape and climate.

axioms (1)
  • domain assumption Mars is a representative analog for small rocky exoplanets at the edge of habitability
    Invoked throughout the abstract as the basis for transferring lessons from Mars to exoplanet processes.

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Works this paper leans on

233 extracted references · 233 canonical work pages · 8 internal anchors

  1. [1]

    H., Connerney, J

    Acuna, M. H., Connerney, J. E. P., Ness, N. F., et al. 1999, Science, 284, 790, doi: 10.1126/science.284.5415.790

    work page doi:10.1126/science.284.5415.790 1999

  2. [2]

    Kane, S. R. 2025, ApJ, 981, 98, doi: 10.3847/1538-4357/ada3c8

    work page doi:10.3847/1538-4357/ada3c8 2025

  3. [3]

    L., et al

    Agol, E., Dorn, C., Grimm, S. L., et al. 2021, PSJ, 2, 1, doi: 10.3847/PSJ/abd022

    work page doi:10.3847/psj/abd022 2021

  4. [4]

    2004, A&A, 414, 1139, doi: 10.1051/0004-6361:20034039

    Aigrain, S., Favata, F., & Gilmore, G. 2004, A&A, 414, 1139, doi: 10.1051/0004-6361:20034039

    work page doi:10.1051/0004-6361:20034039 2004

  5. [5]

    S., Glocer, A., Khazanov, G

    Airapetian, V. S., Glocer, A., Khazanov, G. V., et al. 2017, ApJL, 836, L3, doi: 10.3847/2041-8213/836/1/L3

    work page doi:10.3847/2041-8213/836/1/l3 2017

  6. [6]

    D., An, J., Beaulieu, J

    Albrow, M. D., An, J., Beaulieu, J. P., et al. 2001, ApJL, 556, L113, doi: 10.1086/323141

    work page doi:10.1086/323141 2001

  7. [7]

    M., et al

    Apai, D., Barnes, R., Murphy, M. M., et al. 2025, PSJ, 6, 165, doi: 10.3847/PSJ/addda8

    work page doi:10.3847/psj/addda8 2025

  8. [8]

    F., Lissauer, J

    Barclay, T., Rowe, J. F., Lissauer, J. J., et al. 2013, Nature, 494, 452, doi: 10.1038/nature11914

    work page doi:10.1038/nature11914 2013

  9. [9]

    2013, Astrobiology, 13, 225, doi: 10.1089/ast.2012.0851

    Barnes, R., Mullins, K., Goldblatt, C., et al. 2013, Astrobiology, 13, 225, doi: 10.1089/ast.2012.0851

    work page doi:10.1089/ast.2012.0851 2013

  10. [10]

    2021, MNRAS, 502, 3569, doi: 10.1093/mnras/stab225

    Basak, A., & Nandy, D. 2021, MNRAS, 502, 3569, doi: 10.1093/mnras/stab225

    work page doi:10.1093/mnras/stab225 2021

  11. [11]

    A., Huber, D., Gaidos, E., & van Saders, J

    Berger, T. A., Huber, D., Gaidos, E., & van Saders, J. L. 2018, ApJ, 866, 99, doi: 10.3847/1538-4357/aada83

    work page doi:10.3847/1538-4357/aada83 2018

  12. [12]

    F., et al

    Bibring, J.-P., Langevin, Y., Mustard, J. F., et al. 2006, Science, 312, 400, doi: 10.1126/science.1122659

    work page doi:10.1126/science.1122659 2006

  13. [13]

    2024, A&A, 692, A150, doi: 10.1051/0004-6361/202451537

    Boettner, C., Viswanathan, A., & Dayal, P. 2024, A&A, 692, A150, doi: 10.1051/0004-6361/202451537

    work page doi:10.1051/0004-6361/202451537 2024

  14. [14]

    E., et al

    Bolmont, E., Selsis, F., Owen, J. E., et al. 2017, MNRAS, 464, 3728, doi: 10.1093/mnras/stw2578

    work page doi:10.1093/mnras/stw2578 2017

  15. [15]

    Borucki, W. J. 2016, Reports on Progress in Physics, 79, 036901, doi: 10.1088/0034-4885/79/3/036901

    work page doi:10.1088/0034-4885/79/3/036901 2016

  16. [16]

    J., Koch, D., Basri, G., et al

    Borucki, W. J., Koch, D., Basri, G., et al. 2010, Science, 327, 977, doi: 10.1126/science.1185402

    work page doi:10.1126/science.1185402 2010

  17. [17]

    T., & Bean, J

    Brady, M. T., & Bean, J. L. 2022, AJ, 163, 255, doi: 10.3847/1538-3881/ac64a0

    work page doi:10.3847/1538-3881/ac64a0 2022

  18. [18]

    A., Bagenal, F., Ma, Y

    Brain, D. A., Bagenal, F., Ma, Y. J., Nilsson, H., & Stenberg Wieser, G. 2016, Journal of Geophysical Research (Planets), 121, 2364, doi: 10.1002/2016JE005162

    work page doi:10.1002/2016je005162 2016

  19. [20]

    A., Cohen, O., Cravens, T

    Brain, D. A., Cohen, O., Cravens, T. E., et al. 2026, arXiv e-prints, arXiv:2603.11561, doi: 10.48550/arXiv.2603.11561

    work page doi:10.48550/arxiv.2603.11561 2026

  20. [21]

    Brandt, T. D. 2018, ApJS, 239, 31, doi: 10.3847/1538-4365/aaec06 —. 2021, ApJS, 254, 42, doi: 10.3847/1538-4365/abf93c 18Stephen R. Kane et al

    work page doi:10.3847/1538-4365/aaec06 2018

  21. [22]

    P., Wright, J

    Butler, R. P., Wright, J. T., Marcy, G. W., et al. 2006, ApJ, 646, 505, doi: 10.1086/504701

    work page doi:10.1086/504701 2006

  22. [23]

    Byrne, P. K. 2020, Nature Astronomy, 4, 321, doi: 10.1038/s41550-019-0944-3 Ca˜ nas, C. I., Mahadevan, S., Cochran, W. D., et al. 2022, AJ, 163, 3, doi: 10.3847/1538-3881/ac3088

    work page doi:10.1038/s41550-019-0944-3 2020

  23. [24]

    L., Reefe, M., Plavchan, P., et al

    Cale, B. L., Reefe, M., Plavchan, P., et al. 2021, AJ, 162, 295, doi: 10.3847/1538-3881/ac2c80

    work page doi:10.3847/1538-3881/ac2c80 2021

  24. [25]

    L., Barclay, T., Swift, J

    Campante, T. L., Barclay, T., Swift, J. J., et al. 2015, ApJ, 799, 170, doi: 10.1088/0004-637X/799/2/170

    work page doi:10.1088/0004-637x/799/2/170 2015

  25. [26]

    2012, Nature, 481, 167, doi: 10.1038/nature10684

    Cassan, A., Kubas, D., Beaulieu, J.-P., et al. 2012, Nature, 481, 167, doi: 10.1038/nature10684

    work page doi:10.1038/nature10684 2012

  26. [27]

    S., Chaufray, J.-Y., Stewart, I., et al

    Chaffin, M. S., Chaufray, J.-Y., Stewart, I., et al. 2014, Geophys. Res. Lett., 41, 314, doi: 10.1002/2013GL058578

    work page doi:10.1002/2013gl058578 2014

  27. [28]

    S., Kass, D

    Chaffin, M. S., Kass, D. M., Aoki, S., et al. 2021, Nature Astronomy, 5, 1036, doi: 10.1038/s41550-021-01425-w Chassefi` ere, E., & Leblanc, F. 2004, Planet. Space Sci., 52, 1039, doi: 10.1016/j.pss.2004.07.002

    work page doi:10.1038/s41550-021-01425-w 2021

  28. [29]

    2016 , keywords =

    Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102

    work page internal anchor Pith review doi:10.3847/0004-637x/823/2/102 2016

  29. [30]

    Complete observations, data reduction and analysis, detection performances, and final results

    Chomez, A., Delorme, P., Lagrange, A.-M., et al. 2025, A&A, 697, A99, doi: 10.1051/0004-6361/202451751

    work page doi:10.1051/0004-6361/202451751 2025

  30. [31]

    L., McElroy, D

    Christiansen, J. L., McElroy, D. L., Harbut, M., et al. 2025, PSJ, 6, 186, doi: 10.3847/PSJ/ade3c2

    work page doi:10.3847/psj/ade3c2 2025

  31. [32]

    R., von Braun, K., Bryden, G., et al

    Ciardi, D. R., von Braun, K., Bryden, G., et al. 2011, AJ, 141, 108, doi: 10.1088/0004-6256/141/4/108

    work page doi:10.1088/0004-6256/141/4/108 2011

  32. [33]

    Cockell, C. S. 2014, Astrobiology, 14, 182, doi: 10.1089/ast.2013.1106

    work page doi:10.1089/ast.2013.1106 2014

  33. [34]

    Connerney, J. E. P., Acuna, M. H., Wasilewski, P. J., et al. 1999, Science, 284, 794, doi: 10.1126/science.284.5415.794

    work page doi:10.1126/science.284.5415.794 1999

  34. [35]

    2022, AJ, 164, 225, doi: 10.3847/1538-3881/ac9472

    Damiano, M., Hu, R., Barclay, T., et al. 2022, AJ, 164, 225, doi: 10.3847/1538-3881/ac9472

    work page doi:10.3847/1538-3881/ac9472 2022

  35. [36]

    2011, Nature, 473, 489, doi: 10.1038/nature10077 de Laverny, P., Ligi, R., Crida, A., Recio-Blanco, A., &

    Dauphas, N., & Pourmand, A. 2011, Nature, 473, 489, doi: 10.1038/nature10077 de Laverny, P., Ligi, R., Crida, A., Recio-Blanco, A., &

    work page doi:10.1038/nature10077 2011

  36. [37]

    Palicio, P. A. 2025, A&A, 699, A100, doi: 10.1051/0004-6361/202554739

    work page doi:10.1051/0004-6361/202554739 2025

  37. [38]

    Demangeon, O. D. S., Zapatero Osorio, M. R., Alibert, Y., et al. 2021, A&A, 653, A41, doi: 10.1051/0004-6361/202140728

    work page doi:10.1051/0004-6361/202140728 2021

  38. [39]

    2018a, Proceedings of the National Academy of Science, 115, 260, doi: 10.1073/pnas.1708010115

    Dong, C., Jin, M., Lingam, M., et al. 2018a, Proceedings of the National Academy of Science, 115, 260, doi: 10.1073/pnas.1708010115

    work page doi:10.1073/pnas.1708010115

  39. [40]

    2018b, ApJL, 859, L14, doi: 10.3847/2041-8213/aac489

    Dong, C., Lee, Y., Ma, Y., et al. 2018b, ApJL, 859, L14, doi: 10.3847/2041-8213/aac489

    work page doi:10.3847/2041-8213/aac489 2041

  40. [41]

    2015, A&A, 577, A83, doi: 10.1051/0004-6361/201424915

    Dorn, C., Khan, A., Heng, K., et al. 2015, A&A, 577, A83, doi: 10.1051/0004-6361/201424915

    work page doi:10.1051/0004-6361/201424915 2015

  41. [42]

    2016 , note =

    Dotter, A. 2016, ApJS, 222, 8, doi: 10.3847/0067-0049/222/1/8

    work page internal anchor Pith review doi:10.3847/0067-0049/222/1/8 2016

  42. [43]

    D., & Charbonneau, D

    Dressing, C. D., & Charbonneau, D. 2015, ApJ, 807, 45, doi: 10.1088/0004-637X/807/1/45

    work page doi:10.1088/0004-637x/807/1/45 2015

  43. [44]

    2013, Icarus, 226, 1447, doi: 10.1016/j.icarus.2013.07.025

    Driscoll, P., & Bercovici, D. 2013, Icarus, 226, 1447, doi: 10.1016/j.icarus.2013.07.025

    work page doi:10.1016/j.icarus.2013.07.025 2013

  44. [45]

    L., & Edwards, C

    Ehlmann, B. L., & Edwards, C. S. 2014, Annual Review of Earth and Planetary Sciences, 42, 291, doi: 10.1146/annurev-earth-060313-055024

    work page doi:10.1146/annurev-earth-060313-055024 2014

  45. [46]

    L., Mustard, J

    Ehlmann, B. L., Mustard, J. F., & Murchie, S. L. 2010, Geophys. Res. Lett., 37, L06201, doi: 10.1029/2010GL042596

    work page doi:10.1029/2010gl042596 2010

  46. [47]

    L., Mustard, J

    Ehlmann, B. L., Mustard, J. F., Murchie, S. L., et al. 2011, Nature, 479, 53, doi: 10.1038/nature10582

    work page doi:10.1038/nature10582 2011

  47. [48]

    L., Mustard, J

    Ehlmann, B. L., Mustard, J. F., Swayze, G. A., et al. 2009, Journal of Geophysical Research (Planets), 114, E00D08, doi: 10.1029/2009JE003339

    work page doi:10.1029/2009je003339 2009

  48. [49]

    Elkins-Tanton, L. T. 2008, Earth and Planetary Science Letters, 271, 181, doi: 10.1016/j.epsl.2008.03.062

    work page doi:10.1016/j.epsl.2008.03.062 2008

  49. [50]

    2023, AJ, 166, 140, doi: 10.3847/1538-3881/aced8b

    Fatheddin, H., & Sajadian, S. 2023, AJ, 166, 140, doi: 10.3847/1538-3881/aced8b

    work page doi:10.3847/1538-3881/aced8b 2023

  50. [51]

    2023, ApJS, 268, 4, doi: 10.3847/1538-4365/acdee5

    Fetherolf, T., Pepper, J., Simpson, E., et al. 2023, ApJS, 268, 4, doi: 10.3847/1538-4365/acdee5

    work page doi:10.3847/1538-4365/acdee5 2023

  51. [52]

    A., Anglada-Escude, G., Arriagada, P., et al

    Fischer, D. A., Anglada-Escude, G., Arriagada, P., et al. 2016, PASP, 128, 066001, doi: 10.1088/1538-3873/128/964/066001

    work page doi:10.1088/1538-3873/128/964/066001 2016

  52. [53]

    J., & Smye, A

    Foley, B. J., & Smye, A. J. 2018, Astrobiology, 18, 873, doi: 10.1089/ast.2017.1695

    work page doi:10.1089/ast.2017.1695 2018

  53. [54]

    Ford, E. B. 2014, Proceedings of the National Academy of Science, 111, 12616, doi: 10.1073/pnas.1304219111

    work page doi:10.1073/pnas.1304219111 2014

  54. [55]

    Head, J. W. 2006, Science, 311, 368, doi: 10.1126/science.1120335

    work page doi:10.1126/science.1120335 2006

  55. [56]

    2013, ApJ, 766, 81, doi: 10.1088/0004-637X/766/2/81

    Fressin, F., Torres, G., Charbonneau, D., et al. 2013, ApJ, 766, 81, doi: 10.1088/0004-637X/766/2/81

    work page doi:10.1088/0004-637x/766/2/81 2013

  56. [57]

    2018, Astrobiology, 18, 739, doi: 10.1089/ast.2017.1733

    Fujii, Y., Angerhausen, D., Deitrick, R., et al. 2018, Astrobiology, 18, 739, doi: 10.1089/ast.2017.1733

    work page doi:10.1089/ast.2017.1733 2018

  57. [58]

    J., & Petigura, E

    Fulton, B. J., & Petigura, E. A. 2018, AJ, 156, 264, doi: 10.3847/1538-3881/aae828 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2021, A&A, 649, A1, doi: 10.1051/0004-6361/202039657 Garc´ ıa Mu˜ noz, A., & Cabrera, J. 2018, MNRAS, 473, 1801, doi: 10.1093/mnras/stx2428

    work page doi:10.3847/1538-3881/aae828 2018

  58. [59]

    Gaudi, B. S. 2012, ARA&A, 50, 411, doi: 10.1146/annurev-astro-081811-125518

    work page doi:10.1146/annurev-astro-081811-125518 2012

  59. [60]

    R., Howard, A

    Gibson, S. R., Howard, A. W., Marcy, G. W., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J

    work page 2016

  60. [61]

    Simard, & H

    Evans, L. Simard, & H. Takami, 990870, doi: 10.1117/12.2233334 Mars as an Exoplanet19

    work page doi:10.1117/12.2233334

  61. [62]

    Gillon, M., Triaud, A. H. M. J., Demory, B.-O., et al. 2017, Nature, 542, 456, doi: 10.1038/nature21360

    work page doi:10.1038/nature21360 2017

  62. [63]

    2025, ApJL, 990, L53, doi: 10.3847/2041-8213/adf62e

    Glidden, A., Ranjan, S., Seager, S., et al. 2025, ApJL, 990, L53, doi: 10.3847/2041-8213/adf62e

    work page doi:10.3847/2041-8213/adf62e 2025

  63. [64]

    1992, ApJ, 396, 104, doi: 10.1086/171700

    Gould, A., & Loeb, A. 1992, ApJ, 396, 104, doi: 10.1086/171700

    work page doi:10.1086/171700 1992

  64. [65]

    P., Bell, T

    Greene, T. P., Bell, T. J., Ducrot, E., et al. 2023, Nature, 618, 39, doi: 10.1038/s41586-023-05951-7

    work page doi:10.1038/s41586-023-05951-7 2023

  65. [66]

    L., Demory, B.-O., Gillon, M., et al

    Grimm, S. L., Demory, B.-O., Gillon, M., et al. 2018, A&A, 613, A68, doi: 10.1051/0004-6361/201732233

    work page doi:10.1051/0004-6361/201732233 2018

  66. [67]

    2011, Earth and Planetary Science Letters, 307, 135, doi: 10.1016/j.epsl.2011.04.040

    Grott, M., Breuer, D., & Laneuville, M. 2011, Earth and Planetary Science Letters, 307, 135, doi: 10.1016/j.epsl.2011.04.040

    work page doi:10.1016/j.epsl.2011.04.040 2011

  67. [68]

    Grotzinger, J. P. 2014, Science, 343, 386, doi: 10.1126/science.1249944

    work page doi:10.1126/science.1249944 2014

  68. [69]

    P., Sumner, D

    Grotzinger, J. P., Sumner, D. Y., Kah, L. C., et al. 2014, Science, 343, 1242777, doi: 10.1126/science.1242777

    work page doi:10.1126/science.1242777 2014

  69. [70]

    2018, A&A, 614, L3, doi: 10.1051/0004-6361/201832934

    Gunell, H., Maggiolo, R., Nilsson, H., et al. 2018, A&A, 614, L3, doi: 10.1051/0004-6361/201832934

    work page doi:10.1051/0004-6361/201832934 2018

  70. [71]

    D., Lustig-Yaeger, J., Davis, C

    Guzewich, S. D., Lustig-Yaeger, J., Davis, C. E., et al. 2020, ApJ, 893, 140, doi: 10.3847/1538-4357/ab83ec

    work page doi:10.3847/1538-4357/ab83ec 2020

  71. [72]

    Hansen, B. M. S. 2009, ApJ, 703, 1131, doi: 10.1088/0004-637X/703/1/1131

    work page doi:10.1088/0004-637x/703/1/1131 2009

  72. [73]

    K., Dressing, C

    Harada, C. K., Dressing, C. D., Kane, S. R., & Ardestani, B. A. 2024, ApJS, 272, 30, doi: 10.3847/1538-4365/ad3e81

    work page doi:10.3847/1538-4365/ad3e81 2024

  73. [74]

    G., Kleinb¨ ohl, A., Chaffin, M

    Heavens, N. G., Kleinb¨ ohl, A., Chaffin, M. S., et al. 2018, Nature Astronomy, 2, 126, doi: 10.1038/s41550-017-0353-4

    work page doi:10.1038/s41550-017-0353-4 2018

  74. [75]

    2022, A&A, 665, A11, doi: 10.1051/0004-6361/202141640

    Heller, R., Harre, J.-V., & Samadi, R. 2022, A&A, 665, A11, doi: 10.1051/0004-6361/202141640

    work page doi:10.1051/0004-6361/202141640 2022

  75. [76]

    2012, ApJ, 754, 60, doi: 10.1088/0004-637X/754/1/60

    Heng, K., & Kopparla, P. 2012, ApJ, 754, 60, doi: 10.1088/0004-637X/754/1/60

    work page doi:10.1088/0004-637x/754/1/60 2012

  76. [77]

    L., Bott, K., Dalba, P

    Hill, M. L., Bott, K., Dalba, P. A., et al. 2023, AJ, 165, 34, doi: 10.3847/1538-3881/aca1c0

    work page doi:10.3847/1538-3881/aca1c0 2023

  77. [78]

    Smaller Than Earth Habitability Model (STEHM): The Lower Size Limit for Atmosphere Retention in the Habitable Zone

    Hill, M. L., Kane, S. R., Foley, B. J., & Schaefer, L. K. 2026, arXiv e-prints, arXiv:2605.00170. https://arxiv.org/abs/2605.00170

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  78. [79]

    L., Kane, S

    Hill, M. L., Kane, S. R., Seperuelo Duarte, E., et al. 2018, ApJ, 860, 67, doi: 10.3847/1538-4357/aac384

    work page doi:10.3847/1538-4357/aac384 2018

  79. [80]

    R., Marshall, J

    Horner, J., Kane, S. R., Marshall, J. P., et al. 2020, PASP, 132, 102001, doi: 10.1088/1538-3873/ab8eb9

    work page doi:10.1088/1538-3873/ab8eb9 2020

  80. [81]

    W., Marcy, G

    Howard, A. W., Marcy, G. W., Johnson, J. A., et al. 2010, Science, 330, 653, doi: 10.1126/science.1194854

    work page doi:10.1126/science.1194854 2010

Showing first 80 references.