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the claim
A specific minimum planetary mass is required for Earth to retain its atmosphere
the verdict
INSUFFICIENT LEANING
refutedsupported
the weight of evidence
2 sources for · 0 against

The retrieved sources discuss Earth's biosphere and habitable zones, but do not contain information regarding a specific minimum planetary mass required to retain an atmosphere.

Evidence for · 2
2019 · cited by 17
Abstract Environmental conditions have changed in the past of our planet but were not hostile enough to extinguish life. In the future, an aged Earth and a more luminous Sun may lead to harsh or even uninhabitable conditions for life. In order to estimate the life span of the biosphere we built a minimal model of the co-evolution of the geosphere, atmosphere and biosphere of our planet, taking into account temperature boundaries, CO 2 partial pressure lower limits for C3 and C4 plants, and the presence of enough surface water. Our results indicate that the end of the biosphere will happen long before the Sun becomes a red giant, as the biosphere faces increasingly more difficult conditions in the future until its collapse due to high temperatures. The lower limit for CO 2 partial pressure for C3 plants will be reached in 170(+ 320, − 110) Myr, followed by the C4 plants limit in 840(+ 270, − 100) Myr. The mean surface temperature will reach 373 K in 1.63(+ 0.14, − 0.05) Gyr, a point that would mark the extinction of the biosphere. Water loss due to internal geophysical processes will not be dramatic, implying almost no variation in the surface ocean mass and ocean depth for the next 1.5 billion years. Our predictions show qualitative convergence and some quantitative agreement with results found in the literature, but there is considerable scattering in the scale of hundreds of millions of years for all the criteria devised. Even considering these uncertainties, the end of the biosphere will hardly happen sooner than 1.5 Gyr. 2013), the crust may be too hot to be habitable much before that point, certainly marking the end of life on Earth. However, the end of life may come sooner, long before the Sun ’s exit of the main sequence, due to the increase of solar luminosity with time. There are quantitative estimates of the biosphere life span since the 1980s. The work of Lovelock and Whitfield ( 1982) introduced a number of criteria for habitability, for example, a minimum concentration of carbon dioxide in the atmosphere in order to maintain plant photosynthesis, predicting the collapse of the photosynthetic megaflora in about 100 Myr. Basically, this is a ‘follow the liquid water ’ approach, focusing on maintaining liquid water on the planetary surface in a sustainable way. In the inner limit of the CHZ, the increasing solar luminosity introduces more energy into the Earth system and warm up the oceans, increasing vaporization and water vapour content in the atmosphere. Water vapour, being a greenhouse gas, increases the trapping of energy in the atmosphere and the temperatures, promoting more vaporization. Emission increases with increasing temperatures so equilibrium is possible until certain point. For instance, a low mass terrestrial planet like Mars, when compared to a more massive terrestrial planet like Earth or a super-Earth, may not be able to sustain a high heat flux, geo- logical activity and CO 2 flux from volcanoes for billions of years after its formation, making it hard to maintain an intense greenhouse atmosphere and its temperature above 0 °Ce v e ni fi t is inside the classical outer boundary of the CHZ. Another important phenomenon that could influence over a planetary atmosphere is the erosion due to solar wind. Today, Earth ’s strong bipolar magnetic field ensures the maintenance of a dense atmosphere (Stadelmann et al. 2010). This was the case in the past, but may not be certain in the future. The existence of a strong planetary dynamo-created magnetic field is dependent on the existence of a metal liquid core and cor- related with the mass and rotational period of the planet (Zuluaga and Cuartas 2012; Zuluaga et al. 2013). Cerling TE, Dearing MD and Ehleringer JR (2005) A History of Atmospheric CO 2 and its Effects on Plants, Animals, and Ecosystems . New York, NY, USA: Springer. Chamberlain JW (1980) Changes in the planetary heat balance with chemical changes in air. Planetary and Space Science 28, 1011 – 1018. Chamberlain TP and Hunten DM (1990) Theory of Planetary Atmospheres: An Introduction to Their Physics and Chemistry . New York, NY, USA: Academic Press, Inc. Christensen UR (1985) Thermal evolution models for the Earth. Journal of Geophysical Research: Solid Earth 90, 2995 – 3007. Earth and Planetary Science Letters 497, 149 – 160. Labrosse S and Jaupart C (2007) Thermal evolution of the Earth: secular changes and fluctuations of plate characteristics. Earth and Planetary Science Letters 260, 465 – 481. Lammer H, Odert P, Leitzinger M, Khodachenko M, Panchenko M, Kulikov YN, Zhang T, Lichtenegger H, Erkaev N, Wuchterl G, Micela G, Penz T, Biernat HK, Weingrill J, Steller M, Ottacher H, Hasiba J and Hanslmeier A (2009) Determining the mass loss limit for close-in exoplanets: what can we learn from transit observations? Astronomy and Astrophysics 506, 399 – 410. Proceedings of the National Academy of Sciences 109, 4371 – 4376. Rea DK and Ruff LR (1996) Composition and mass flux of sediment entering the world ’s subduction zones: Implications for global sediment budgets, great earthquakes, and volcanism. Earth and Planetary Science Letters 140,1 – 12. Ribas I, Guinan EF, Gudel M and Audard M (2005) Evolution of the solar activity over time and effects on planetary atmospheres I High-energy irra- diances (1 – 1700 Å). The Astrophysical Journal 622, 680 – 694. Richter FM (1984) Regionalized models for the thermal evolution of the Earth. Earth and Planetary Science Letters 68, 471 – 484. Walker JC, Hays P and Kasting JF (1981) A negative feedback mechanism for the long-term stabilization of Earth ’s surface temperature. Journal of Geophysical Research: Oceans 86, 9776 – 9782. Watson AJ and Lovelock JE (1983) Biological homeostasis of the global envir- onment: the parable of Daisyworld. Tellus B: Chemical and Physical Meteorology 35, 284 – 289. Watson AJ, Donahue TM and Walker JC (1981) The dynamics of a rapidly escaping atmosphere: applications to the
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The analysis

rails:sufficiency:partial_only:for=0+2p:against=0+0p | v55:multi_partial_one_side:lean=lean_partial:for:one_sided | v55:coherence_repaired:what=summary

More for · 1
cited by 0
around planets where the atmosphere has carbon dioxide, as by the time a solar-mass star becomes a red giant, planetary-mass bodies would have already In astronomy and astrobiology, the habitable zone (HZ), also known as the circumstellar habitable zone (CHZ), or as the Goldilocks zone, is the range of orbits around a star within which a planetary surface could potentially support liquid water. Liquid water is considered by many scientists as necessary for a planet to be habitable. The range depends upon the brightness of the star interacting wi Conventional habitable zones only require liquid water, a minimum requirement for conventional microbial life. Complex aerobic life is likely to have many additional requirements, including limitations on the concentrations of CO2 and CO in the atmosphere. This has led to the concept of a habitable zone for complex life. The Rare Earth hypothesis argues that complex and intelligent life is uncommon and that the HZ is one of many critical factors. The secondary habitability factors required for multicellular life are both geological (the role of surface water in… Proxima Centauri b, located about 4.2 light-years (1.3 parsecs) from Earth in the constellation of Centaurus, is the nearest known exoplanet, and is orbiting in the habitable zone of its star. The HZ is also of particular interest to the emerging field of habitability of natural satellites because planetary mass moons in the HZ might outnumber planets. The classical habitable zone concept was defined only for planetary surfaces where habitat depends on stellar energy. Deep biospheres are known on Earth, but they would not be detectable on exoplanets. As the name suggests, the continuously habitable zone is a region around a star in which planetary-mass bodies can sustain liquid water for a given period. Like the general circumstellar habitable zone, the continuously habitable zone of a star is divided into a conservative and extended region. In red dwarf systems, gigantic stellar flares which could double a star's brightness in minutes and huge starspots which can cover 20% of the star's surface area, have the potential to strip an otherwise habitable planet of its atmosphere and water. At such stage, Saturn's moon Titan would likely be habitable in Earth's temperature sense. Given that this new equilibrium lasts for about 1 Gyr, and because life on Earth emerged by 0.7 Gyr from the formation of the Solar System at latest, life could conceivably develop on planetary mass objects in the habitable zone of red giants. However, around such a helium-burning star, important life processes like photosynthesis could only happen around planets where the atmosphere has carbon dioxide, as by the time a solar-mass star becomes a red giant, planetary-mass bodies would have already absorbed much of their free carbon dioxide. Moreover, as Ramirez and Kaltenegger (2016) showed, intense stellar winds would completely remove the atmospheres of such smaller planetary bodies, rendering them uninhabitable anyway. Thus, Titan would not be habitable even after the Sun becomes a red giant. Nevertheless, life need not originate during this stage of stellar evolution for it to be detected. Once the star becomes a red giant, and the habitable zone extends outward, the icy surface would melt, forming a temporary atmosphere that can be searched for signs of life that may have been thriving before the start of the red giant stage. Among nearest terrestrial exoplanet candidates, Tau Ceti e is 11.9 light-years away. It is in the inner edge of its planetary system's habitable zone, giving it an estimated average surface temperature of 68 °C (154 °F). === Early findings === The first discoveries of extrasolar planets in the HZ occurred just a few years after the first extrasolar planets were discovered. However, these early detections were all gas giant-sized, and many were in eccentric orbits. Despite this, studies indicate the possibility of large, Earth-like moons around these planets supporting liquid water. Subsequent study has shown they have hydrogen gas atmospheres and they fall into two categories: the larger ones have retain atmospheres but the smaller ones are stipped cores. Models that simulate this bimodal distribution predict that stellar radiation perhaps combined with heat from planetary cooling drive off the atmosphere causing some of these exoplanets to appear smaller. In general, these exoplanets are not in the habitable zone. Moreover, the processes which strip the hydrogen atmosphere from this type of exoplanet is unlikely to operate on planets in the habitable zone. Announced on the 20 April 2017, LHS 1140b is a super-dense super-Earth 39 light years away, 6.6 times Earth's mass and 1.4 times radius, its star 15% the mass of the Sun but with much less observable stellar flare activity than most M dwarfs. The planet is one of few observable by both transit and radial velocity that's mass is confirmed with an atmosphere may be studied. Discovered by radial velocity in June 2017, with approximately three times the mass of Earth, Luyten b orbits within the habitable zone of Luyten's Star just 12.2 light-years away. K2-18b is an exoplanet 124 light-years away, orbiting in the habitable zone of the K2-18, a red dwarf. This planet is significant for water vapor found in its atmosphere; this was announced on September 17, 2019. In September 2020, astronomers identified 24 superhabitable planet The Drake equation, sometimes used to estimate the number of intelligent civilizations in our galaxy, contains the factor or parameter ne, which is the average number of planetary-mass objects orbiting within the HZ of each star. A low value lends support to the Rare Earth hypothesis, which posits that intelligent life is a rarity in the Universe, whereas a high value provides evidence for the Copernican mediocrity principle, the view that habitability—and therefore life—is common throughout the Universe.
Everything we examined (2)
This check searched the claim as stated. It did not run a separate search for evidence against it.
  1. The end of life on Earth is not the end of the world: converging to an estimate of life span of the biosphere?peer-reviewedno side taken
  2. Habitable zonereferenceno side taken
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first checked04 Aug 2026
judged → INSUFFICIENT EVIDENCE · 004 Aug 2026
held for human review07 Aug 2026
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