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HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES
Open accessAbstract
Identifying terrestrial planets in the habitable zones (HZs) of other stars is one of the primary goals of ongoing radial velocity (RV) and transit exoplanet surveys and proposed future space missions. Most current estimates of the boundaries of the HZ are based on one-dimensional (1D), cloud-free, climate model calculations by Kasting et al. However, this model used band models that were based on older HITRAN and HITEMP line-by-line databases. The inner edge of the HZ in the Kasting et al. model was determined by loss of water, and the outer edge was determined by the maximum greenhouse provided by a CO 2 atmosphere. A conservative estimate for the width of the HZ from this model in our solar system is 0.95–1.67 AU. Here an updated 1D radiative–convective, cloud-free climate model is used to obtain new estimates for HZ widths around F, G, K, and M stars. New H 2 O and CO 2 absorption coefficients, derived from the HITRAN 2008 and HITEMP 2010 line-by-line databases, are important improvements to the climate model. According to the new model, the water-loss (inner HZ) and maximum greenhouse (outer HZ) limits for our solar system are at 0.99 and 1.70 AU, respectively, suggesting that the present Earth lies near the inner edge. Additional calculations are performed for stars with effective temperatures between 2600 and 7200 K, and the results are presented in parametric form, making them easy to apply to actual stars. The new model indicates that, near the inner edge of the HZ, there is no clear distinction between runaway greenhouse and water-loss limits for stars with T eff ≲ 5000 K, which has implications for ongoing planet searches around K and M stars. To assess the potential habitability of extrasolar terrestrial planets, we propose using stellar flux incident on a planet rather than equilibrium temperature. This removes the dependence on planetary (Bond) albedo, which varies depending on the host star's spectral type. We suggest that conservative estimates of the HZ (water-loss and maximum greenhouse limits) should be used for current RV surveys and Kepler mission to obtain a lower limit on η ⊕ , so that future flagship missions like TPF-C and Darwin are not undersized. Our model does not include the radiative effects of clouds; thus, the actual HZ boundaries may extend further in both directions than the estimates just given.
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“The new Kopparapu et al. (2013) habitable zone model recalculates the classic Kasting et al. (1993) habitable zone with updated model inputs, and its habitable zone extends from 0.99 to 1.70 AU.”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Kopparapu et al. (2013)
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“However, this study did not include the effects of clouds or circulation of moisture, either of which could stabilize a planet at the inner edge of the habitable zone.”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Kopparapu et al. (2013)
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“In this updated conservative estimation, Earth is very near the inner edge of the current habitable zone.”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Kopparapu et al. (2013)
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“The location of the habitable zone depends on how bright the star is (Kopparapu et al., 2013); for brighter stars, the habitable zone is shifted outward because planets must be farther away from these stars to maintain temperatures necessary for liquid water, and for dimmer stars, the habitable zone is shifted inward (Fig. 18).”
From The Astrobiology Primer v2.0 (2016) · cites this paper as Kopparapu et al., 2013
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Cites
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“Rayleigh scattering by water was also considered by Kasting (1988); Kasting et al. (1993), but these authors used the scattering coefficient for air because the coefficient for H2O was not available, or at least not known to them.”
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“As with the inner edge model, a more optimistic empirical limit on the OHZ can be estimated based on the observation that early Mars was warm enough for liquid water to flow on its surface (Pollack et al. 1987; Bibring et al. 2006).”
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Comparative Analysis of Machine Learning Algorithms for Analyzing NASA Kepler Mission Data
Vishwarupe, V., Bedekar, M. V., Pande, M., Bhatkar, V. P., Joshi, P., Zahoor, S., & Kuklani, P. (2022) · Procedia Computer Science · doi:10.1016/j.procs.2022.08.115 · Cited by 11
A New Definition of Exoplanet Habitability: Introducing the Photosynthetic Habitable Zone
Hall, C., Stancil, P. C., Terry, J. P., & Ellison, C. K. (2023) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/acccfb · Cited by 15
EXOPLANETARY DETECTION BY MULTIFRACTAL SPECTRAL ANALYSIS
Agarwal, S., Sordo, F. D., & Wettlaufer, J. (2016) · The Astronomical Journal · doi:10.3847/1538-3881/153/1/12 · Cited by 10
Gómez-Leal, I., Kaltenegger, L., Lucarini, V., & Lunkeit, F. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaea5f · Cited by 13
“The rising temperatures will increase the evaporation and are expected to cause the loss of the water reserves of our planet (e.g. Kasting et al. 1984; Kasting 1988; Kasting et al. 1993; Kopparapu et al. 2013).”
BackgroundMethodResultInfluentialDoes the Evolution of Complex Life Depend on the Stellar Spectral Energy Distribution?
Haqq-Misra, J. (2019) · Astrobiology · doi:10.1089/ast.2018.1946 · Cited by 11
“h range, although the actual lowmass limit does depend upon the choice of scenario. 7 The Earth equivalent distance does not necessarily correspond to the liquid water habitable zone as calculated by Kopparapu et al. (2013). Using the Earth equivalent distance normalizes the Planck functions for other stellar masses t…”
The high-energy radiation environment of the habitable-zone super-Earth LHS 1140b
Spinelli, R., Borsa, F., Ghirlanda, G., Ghisellini, G., Campana, S., Haardt, F., & Poretti, E. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935636 · Cited by 11
“The habitable zone (HZ) is typically defined as the orbital distance at which the steady stellar irradiation leads to a suitable temperature for the presence of liquid water on the planetary surface (e.g., Kasting et al. 1993; Kopparapu et al. 2013).”
BackgroundMultiverse Predictions for Habitability: Number of Potentially Habitable Planets
Sandora, M. (2019) · Universe · doi:10.3390/universe5060157 · Cited by 11
Standard exoplanet yield evaluation for the LUVOIR and HabEx concept studies
Morgan, R. M., Savransky, D., Turmon, M., Mennesson, B. P., Mamajek, E. E., Shaklan, S., Soto, G., Stapelfeldt, K. R., Dula, W., & Keithly, D. (2019) · Techniques and Instrumentation for Detection of Exoplanets · doi:10.1117/12.2530668 · Cited by 11
“Exo-earth candidates are assumed to be on circular orbits and to reside within the conservative HZ, spanning 0.95–1.67 AU for a solar twin (Kopparapu et al., 2013).”
BackgroundInfluentialBiosignatures Search in Habitable Planets
Claudi, R., & Alei, E. (2019) · Galaxies · doi:10.3390/galaxies7040082 · Cited by 14
“The loss of hydrogen and the photochemical induced production of oxygen is driven by the distance from the host star and from the gravitational pull of the planet itself [66,67,83].”
BackgroundInfluentialElectric sails are potentially more effective than light sails near most stars
Lingam, M., & Loeb, A. (2019) · Acta Astronautica · doi:10.1016/j.actaastro.2019.12.013 · Cited by 11
“Lastly, if any exoplanets exist in the habitable zone - which would be situated at distances similar to d? [28; 29; 30; 31] - they are well-suited to serve as “natural” bases for launching these spacecrafts.”
BackgroundThe Dark Planets of the WASP-47 Planetary System
Kane, S. R., Fetherolf, T., & Hill, M. L. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab7818 · Cited by 11
“We adopt the HZ as described by Kopparapu et al. (2013, 2014), including the conservative and optimistic boundaries (Kane et al. 2013, 2016).”
MethodLisse, C. M., Desch, S. J., Unterborn, C. T., Kane, S. R., Young, P. R., Hartnett, H. E., Hinkel, N. R., Shim, S.-H. D., Mamajek, E. E., & Izenberg, N. R. (2020) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab9b91 · Cited by 11
Atmospheric stability and collapse on tidally locked rocky planets
Auclair-Desrotour, P., & Heng, K. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/202037513/pdf · Cited by 12
HADES RV Programme with HARPS-N at TNG
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A brief history of the term ‘habitable zone’ in the 19th century
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Barbato, D., Pinamonti, M., Sozzetti, A., Biazzo, K., Benatti, S., Damasso, M., Desidera, S., Lanza, A. F., Maldonado, J., Mancini, L., et al. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202037954 · Cited by 11
“With these updated stellar parameters, we use the 1D radiative-convective, cloud-free climate model detailed in Kopparapu et al. (2013, 2014) to compute the inner and outer boundaries of the circumstellar habitable zone.”
MethodExploring exomoon atmospheres with an idealized general circulation model
Haqq-Misra, J. D., & Heller, R. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1630 · Cited by 11
“Calculations with other models indicate that atmospheres enter a moist greenhouse and begin to rapidly lose water to space when stratospheric specific humidity exceeds a threshold of qstrat ≈ 10−3 (Kasting 1988; Kopparapu et al. 2013; Wolf & Toon 2014; Kopparapu et al. 2016).”
Feliz, D. L., Blank, D. L., Collins, K. A., White, G. L., Stassun, K. G., Curtis, I. A., Hart, R., Kielkopf, J. F., Nelson, P., Relles, H. M., et al. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab184f · Cited by 11
The Habitable Zone of Inhabited PlanetsPreprint
Zuluaga, J. I., Salazar, J. F., Cuartas-Restrepo, P. A., & Poveda, G. (2014) · doi:10.5194/bgd-11-8443-2014
Inner Habitable Zone Boundary for Eccentric Exoplanets
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The CARMENES search for exoplanets around M dwarfs
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HWO yield sensitivities in the NIR and NUV
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Wogan, N. F., Batalha, N. E., Zahnle, K. J., Krissansen‐Totton, J., Catling, D. C., Wolf, E. T., Robinson, T. D., Meadows, V., Arney, G., & Domagal-Goldman, S. D. (2025) · The Planetary Science Journal · doi:10.3847/psj/ae0e1c · Cited by 16
“Particles have a radius prescribed by the user, and fall according to Stokes’ law (Appendix A.7) until they leave the bottom of the model domain or evaporate.”
Self-citationThree small transiting planets around the M-dwarf host star LP 358-499
Wells, R., Poppenhaeger, K., & Watson, C. A. (2017) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slx171 · Cited by 10
“This is in line with more detailed habitable zone models by Kopparapu et al. (2013), which report the habitable zone for a star with a mass of 0.5 M to range from semi-major axes of ca. 0.15 to 0.3 AU; the three detected planets are closer to their host star than that.”
ResultInfluentialBlank, D. L., Feliz, D. L., Collins, K. A., White, G. L., Stassun, K. G., Curtis, I. A., Hart, R., Kielkopf, J. F., Nelson, P., Relles, H., et al. (2018) · The Astronomical Journal · doi:10.3847/1538-3881/aabded · Cited by 10
“The discovery of Proxima Centauri b (Proxima b, hereafter) claimed by Anglada-Escudé et al. (2016) (A2016, hereafter) in an 11.2 day habitable zone (Kopparapu et al. 2013) orbit of its host star is important because the planet would likely be a rocky (Brugger et al. 2016; Kane et al. 2017; Bixel &…”
BackgroundInfluentialDugaro, A., de Elía, G. C., & Darriba, L. A. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936061 · Cited by 10
“In this sense, Kopparapu et al. (2013) established inner and outer limits for the HZ around stars of different spectral types.”
BackgroundBonati, I., & Ramirez, R. M. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab891 · Cited by 10
Self-citationNext-generation active telescope for space astronomy
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Sánchez, M., de Elía, G. D., & Downes, J. J. (2020) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201937317 · Cited by 1
“…and outer limits of a system with a Sun-like star as central object, considering runaway greenhouse and maximum greenhouse values, respectively (Kopparapu et al. 2013a,b), and ain = 2.7619× 10−5 au K−1, bin = 3.8095 × 10−9 au K−2, aout = 1.3786 × 10−4 au K−1, and bout = 1.4286 × 10−9 au K−2…”
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“Using this “maximum greenhouse limit,” the outer edge of the liquid water habitable zone has been placed at 1.67 astronomical units (au) (Kopparapu et al., 2013) , implying Seff = 11.672 = 0.359, with pCO2≈6-7 bar.”
BackgroundMethodResultInfluentialDirect imaging of exoplanets in the habitable zone with adaptive optics
Males, J. R., Close, L. M., Guyon, O., Morzinski, K., Puglisi, A., Hinz, P., Follette, K. B., Monnier, J. D., Tolls, V., Rodigas, T. J., et al. (2014) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.2057135 · Cited by 28
“Recent estimates for these limits from Kopparapu et al (2013)22 are • Inner edge (H2O loss): 0.99 AU • Outer edge (Max. greenhouse): 1.70 AU Note that there is great deal of ongoing work on this topic, and these values will likely be revised under further study.”
BackgroundInfluentialBarnes, R. (2014) · International Journal of Astrobiology · doi:10.1017/s1473550413000499 · Cited by 10
“…searches for habitable environments begin with the comparison of a planet’s orbit relative to the host star’s habitable zone (HZ), the region around a star for which an Earth-like planet can support water on its surface (Dole 1964; Kasting et al. 1993; Selsis et al. 2007; Kopparapu et al. 2013).”
BackgroundAstrophysical and Cosmological Constraints on Life
Mason, P., & Biermann, P. L. (2018) · Elsevier eBooks · doi:10.1016/b978-0-12-811940-2.00005-8 · Cited by 10
Factors Affecting Exoplanet Habitability
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Self-citationDIRECT IMAGING IN THE HABITABLE ZONE AND THE PROBLEM OF ORBITAL MOTION
Males, J., Skemer, A., & Close, L. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/771/1/10 · Cited by 13
“This is far from simply related to the blackbody equilibrium temperature, as it depends on atmospheric composition and the action of the greenhouse effect (Kasting et al. 1993; Kopparapu et al. 2013), among other factors.”
BackgroundPLATO: the ESA mission for exo-planets discovery
Magrin, D., Roberto Ragazzoni, B., Rauer, H., Pagano, I., Nascimbeni, V., Piotto, G., Piazza, D., Schweitzer, M., Basso, S., Bandy, T., et al. (2018) · Space Telescopes and Instrumentation: Optical, Infrared, and Millimeter Wave · doi:10.1117/12.2313538 · Cited by 10
“rocky planets orbiting at the right distance from their stars to allow liquid water to condense on their surfaces [9], is currently seen by most astronomers as the holy grail of planetary science.”
BackgroundKar, A., Henry, T. J., Couperus, A. A., Vrijmoet, E. H., & Jao, W. (2024) · The Astronomical Journal · doi:10.3847/1538-3881/ad2ddc · Cited by 9
Stellar X-Ray Activity and Habitability Revealed by the ROSAT Sky Survey
Han, H., Wang, S., Zheng, C., Li, X., Xiao, K., & Liu, J. (2024) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ad4b17 · Cited by 10
Exoplanet Geology: What Can We Learn from Current and Future Observations?
Foley, B. J. (2024) · Reviews in Mineralogy and Geochemistry · doi:10.2138/rmg.2024.90.15 · Cited by 11
“Moreover, the cool temperature of M-dwarfs means that the habitable zone is much closer to the star than for a sun-like star, so even habitable zone planets have short period orbits (e.g. Kasting et al. 1993b; Kopparapu et al. 2013).”
BackgroundClimate Regimes across the Habitable Zone: A Comparison of Synchronous Rocky M and K Dwarf Planets
Lobo, A. H., & Shields, A. L. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad58bb · Cited by 9
Absence of a Runaway Greenhouse Limit on Lava Planets
Boer, I. D., Nicholls, H., & Lichtenberg, T. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/add69f · Cited by 17
Exploring the sub-Neptune frontier with JWST
Madhusudhan, N., Holmberg, M., Constantinou, S., & Cooke, G. J. (2025) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.2416194122 · Cited by 9
Design reference missions for the exoplanet starshade (Exo-S) probe-class study
Trabert, R., Shaklan, S., Lisman, P. D., Roberge, A., Turnbull, M., Domagal-Goldman, S. D., & Stark, C. C. (2015) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.2190383 · Cited by 9
Self-citationImproved Analysis of Clarke Exobelt Detectability
Sallmen, S., Korpela, E. J., & Crawford-Taylor, K. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab5300 · Cited by 9
Transmission Spectroscopy of the Earth–Sun System to Inform the Search for Extrasolar Life
Mayorga, L. C., Lustig‐Yaeger, J., May, E., Sotzen, K. S., Gonzalez-Quiles, J., Kilpatrick, B., Martin, E. C., Mandt, K. E., Stevenson, K. B., & Izenberg, N. R. (2021) · The Planetary Science Journal · doi:10.3847/psj/ac0c85 · Cited by 9
EOS: Atmospheric Radiative Transfer in Habitable Worlds with HELIOS
Simonetti, P., Vladilo, G., Silva, L., MARIS, M., Ivanovski, S. L., Biasiotti, L., Malik, M., & von Hardenberg, J. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac32ca · Cited by 9
The Atlas of Mars: Mapping its Geography and Geology
Coles, K. S., Tanaka, K. L., & Christensen, P. R. (2019) · CERN Document Server (European Organization for Nuclear Research) · doi:10.1017/9781139567428 · Cited by 2
Mapping the Skies of Ultracool Worlds: Detecting Storms and Spots with Extremely Large Telescopes
Plummer, M. K., & Wang, J. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/accd5d · Cited by 10
Signs of magnetic star-planet interactions in HD 118203
Castro-González, A., Lillo-Box, J., Correia, A. C. M., Santos, N. C., Barrado, D., Morales‐Calderón, M., & Shkolnik, E. L. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348722 · Cited by 9
Cloutier, R., & Triaud, A. H. M. J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1953 · Cited by 10
Habitability of Planets in Binary Star Systems
Eggl, S. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_61 · Cited by 9
Fiber Mode Scrambler for the Subaru Infrared Doppler Instrument (IRD)
Ishizuka, M., Kotani, T., Nishikawa, J., Kurokawa, T., Mori, T., Kokubo, T., & Tamura, M. (2018) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/aab8d0 · Cited by 9
“Nearly 4000 exoplanets have been discovered, and Earth-like planets in the habitable zone (HZ, Huang 1959, Kopparapu et al. 2013) are drawing increasing interest, though extremely high precision is required to detect such planets.”
BackgroundThe Habitable Zone: The Climatic Limits of Habitability
Kopparapu, R. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_58 · Cited by 10
Self-citationThree Direct Imaging Epochs Could Constrain the Orbit of Earth 2.0 inside the Habitable Zone
Guimond, C. M., & Cowan, N. B. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab0f2e · Cited by 9
Intermittent signals and planetary days in SETI
Gray, R. H. (2020) · International Journal of Astrobiology · doi:10.1017/s1473550420000038 · Cited by 9
“…subsets that might be most relevant for planets with life are: 1484 hours for rocky planets (five cases), 24.2 hours for planets in or near the current solar habitable zone 0.95-1.67 AU (Kopparapu et al. 2013, Kasting et al. 1993) (two cases), and 23.9 hours for the one planet known to have life.”
BackgroundInfluentialStatistical Properties of Habitable Zones in Stellar Binary Systems
Simonetti, P., Vladilo, G., Silva, L., & Sozzetti, A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abc074 · Cited by 9
“In conjunction with the spectral energy distribution (SED) of the central star, the insolation is commonly used to define the spatial extent of the circumstellar habitable zone (HZ; Kopparapu et al. 2013a, 2014).”
BackgroundMethodInfluentialEstimating Planetary Mass with Deep Learning
Tasker, E. J., Laneuville, M., & Guttenberg, N. (2020) · Institutional Repositories DataBase (IRDB) · Cited by 9
Lenardic, A., & Seales, J. (2021) · International Journal of Astrobiology · doi:10.1017/s1473550420000415 · Cited by 9
“Figure 2(a) is based on habitable zone models (Kopparapu et al. 2013).”
BackgroundMilankovitch cycles for a circumstellar Earth-analog within α Centauri-like binaries
Quarles, B., Li, G., & Lissauer, J. J. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3179 · Cited by 9
Sensitivity to habitable planets in the Roman microlensing survey
Sajadian, S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2942 · Cited by 9
TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Vach, S., Quinn, S. N., Vanderburg, A. M., Kane, S. R., Collins, K. A., Kraus, A. L., Zhou, G., Medina, A. A., Schwarz, R. P., Collins, K. I., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac7954 · Cited by 9
Smith, A. M. S., Breton, S., Csizmadia, S., Dai, F., Gandolfi, D., García, R. A., Howard, A. W., Isaacson, H. T., Korth, J., Lam, K. W. F., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3497 · Cited by 9
The Role of Atmospheric Exchange in False‐Positive Biosignature Detection
Felton, R. C., Bastelberger, S., Mandt, K. E., Luspay‐Kuti, A., Fauchez, T. J., & Domagal-Goldman, S. D. (2022) · Journal of Geophysical Research Planets · doi:10.1029/2021je006853 · Cited by 9
Self-citationTidally driven tectonic activity as a parameter in exoplanet habitability
McIntyre, S. R. N. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141112 · Cited by 9
HD 83443c: A Highly Eccentric Giant Planet on a 22 yr Orbit
Errico, A., Wittenmyer, R. A., Horner, J., Li, Z., Brandt, G. M., Kane, S. R., Fetherolf, T., Holt, T. R., Carter, B., Clark, J., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac6589 · Cited by 10
Basant, R., Dietrich, J., & Apai, D. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac6f58 · Cited by 9
Plummer, M. K., & Wang, J. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac75b9 · Cited by 9
Consequences of dynamically unstable moons in extrasolar systems
Hansen, B. M. S. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2847 · Cited by 9
Tuchow, N. W., & Wright, J. T. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb054 · Cited by 9
GRAVITATIONAL MICROLENSING EVENTS AS A TARGET FOR THE SETI PROJECT
Rahvar, S. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/828/1/19 · Cited by 9
Truitt, A., & Young, P. A. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/835/1/87 · Cited by 8
“Tables 6 and 7 show changes in the location of the HZ radius in AU from ZAMS to TAMS for both the Runaway Greenhouse inner boundary (RGH), and the Maximum Greenhouse outer boundary (MaxGH), respectively, which are the conservative HZ limit cases discussed in Kopparapu et al. (2013, 2014).”
MethodThe Effect of Seafloor Weathering on Planetary Habitability
Chambers, J. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab94a4 · Cited by 9
“D radiative-convective climate model with a fully water saturated troposphere generated by Kopparapu et al. (2013, 2014).”
BackgroundMethodA Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Harman, C. E., Kopparapu, R., Stefánsson, G., Lin, A. S. J., Mahadevan, S., Hedges, C., & Batalha, N. E. (2022) · The Planetary Science Journal · doi:10.3847/psj/ac38ac · Cited by 9
Self-citationMadau, P. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acfe0e · Cited by 10
Timmermans, M., Dransfield, G., Gillon, M., Triaud, A. H. M. J., Rackham, B. V., Aganze, C., Barkaoui, K., Briceño, C. A., Burgasser, A. J., Collins, K. A., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347981 · Cited by 8
Potential climates and habitability on Gl 514 b: a super-Earth exoplanet with high eccentricity
Biasiotti, L., Simonetti, P., Vladilo, G., Ivanovski, S. L., Damasso, M., Sozzetti, A., & Monai, S. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1124 · Cited by 8
Konrad, B. S., Quanz, S. P., Alei, E., & Wordsworth, R. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad74f7 · Cited by 8
Harada, C., Dressing, C., Turtelboom, E., Kane, S., Blunt, S., Dietrich, J., Hinkel, N., Li, Z.-X., Mamajek, E. E., Rice, M., et al. (2024) · Astronomical Journal · doi:10.3847/1538-3881/ae0b62 · Cited by 9
Daspute, M., Wandel, A., Kopparapu, R., Perdelwitz, V., Teklu, J. T., & Tal-Or, L. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ad9ba9 · Cited by 9
Self-citationHotnisky, A., Kanodia, S., Libby-Roberts, J., Mahadevan, S., Cañas, C., Gupta, A. F., Han, T., Kobulnicky, H., Larsen, A., Robertson, P., et al. (2025) · Astronomical Journal · doi:10.3847/1538-3881/add2ef · Cited by 9
Self-citationDetailed Architecture of the L 98-59 System and Confirmation of a Fifth Planet in the Habitable Zone
Cadieux, C., L’Heureux, A., Piaulet, C., Doyon, R., Artigau, É., Cook, N. J., Coulombe, L.-P., Roy, P.-A., Lafreniére, D., Lamontagne, P., et al. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/adef59 · Cited by 8
Wickramasinghe, C., & Smith, W. E. (2014) · Hypothesis · doi:10.5779/hypothesis.v12i1.358 · Cited by 8
Bancelin, D., Pilat‐Lohinger, E., Maindl, T. I., Ragossnig, F., & Schäfer, C. M. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa7202 · Cited by 7
“Recently, Küppers et al. (2014) reported water emission from Ceres using Herschel observations.”
BackgroundMethodCloutier, R. (2019) · The Astronomical Journal · doi:10.3847/1538-3881/ab27be · Cited by 8
Blank, D. L., Feliz, D. L., Collins, K. A., White, G. L., Stassun, K. G., Curtis, I. A., Hart, R., Kielkopf, J. F., Nelson, P., Relles, H. M., et al. (2018) · ResearchOnline - JCU (James Cook University) · Cited by 8
The SOPHIE search for northern extrasolar planets XIII. Two planets around M-dwarfs Gl617A and Gl96
Hobson, M. J., Díaz, R. F., Delfosse, X., Astudillo-Defru, N., Boisse, I., Bouchy, F., Bonfils, X., Forveille, T., Hara, N., Arnold, L., et al. (2018) · Open Repository and Bibliography (University of Liège) · doi:10.48550/arxiv.1806.10958 · Cited by 8
Arredondo, A., Hodges, A., Abrahams, J. N. H., Bedford, C. C., Boatwright, B., Buz, J., Cantrall, C. E., Clark, J. V., Erwin, A., Krishnamoorthy, S., et al. (2022) · The Planetary Science Journal · doi:10.3847/psj/ac7324 · Cited by 8
Metadata
- Authors
- Kopparapu, R. K., Ramirez, R., Kasting, J. F., Eymet, V., Robinson, T. D., Mahadevan, S., Terrien, R. C., Domagal-Goldman, S., Meadows, V., & Deshpande, R.
- Affiliations
- Pennsylvania State University (US)
- Laboratoire d'Astrophysique de Bordeaux (FR)
- NASA Astrobiology Institute (US)
- Goddard Space Flight Center (US)
- ORCID
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2013-02-26
- Volume
- 765
- Issue
- 2
- Pages
- 131
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2047751764
- Cited by
- 1,615
- References
- 95
- Citations by year
- 2026: 89 · 2025: 115 · 2024: 119 · 2023: 125 · 2022: 110 · 2021: 112 · 2020: 157 · 2019: 177 · 2018: 149 · 2017: 109 · 2016: 115 · 2015: 83 · 2014: 95 · 2013: 55
- FWCI
- 61.44
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Licence
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- HAL (submittedVersion)
- Oskar-Bordeaux (Universite de Bordeaux) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (1126413, 1006676)
- National Aeronautics and Space Administration (NNH05ZDA001C)
- Pennsylvania Space Grant Consortium
- Oak Ridge Associated Universities
- University of Pennsylvania
- University of Washington
- Pennsylvania State University
- NASA Astrobiology Institute
- NASA Headquarters
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Space Science and Extraterrestrial Life
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Planetary Science and Exploration
- Keywords
- habitable zone, main-sequence stars, terrestrial exoplanets, water loss, runaway greenhouse, stellar effective temperature, stellar flux, M dwarfs, K stars, F and G stars
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