Habitable Zones Around Main-Sequence Stars: Dependence on Planetary Mass

Kopparapu, R.; Ramirez, Ramses M.; Schottelkotte, J. C.; Kasting, James F.; Domagal-Goldman, Shawn; Eymet, Vincent

doi:10.1088/2041-8205/787/2/l29

Cited by 585 publications

(850 citation statements)

References 45 publications

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“…This result highlights that systems with a Jovian with e 0.4 near the HZ seem unlikely to be able to host a rocky planet within the HZ. This Kopparapu et al (2014), while the orange region indicates the chaotic region as per the equations presented by Giuppone et al (2013). The size of each planet represents the mass ratio, µ = M planet /M , of the system.…”

Section: Resultsmentioning

confidence: 99%

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Stable habitable zones of single Jovian planet systems

Agnew

Maddison

Thilliez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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With continued improvement in telescope sensitivity and observational techniques, the search for rocky planets in stellar habitable zones is entering an exciting era. With so many exoplanetary systems available for follow-up observations to find potentially habitable planets, one needs to prioritise the ever-growing list of candidates. We aim to determine which of the known planetary systems are dynamically capable of hosting rocky planets in their habitable zones, with the goal of helping to focus future planet search programs. We perform an extensive suite of numerical simulations to identify regions in the habitable zones of single Jovian planet systems where Earth mass planets could maintain stable orbits, specifically focusing on the systems in the Catalog of Earth-like Exoplanet Survey Targets (CELESTA). We find that small, Earth-mass planets can maintain stable orbits in cases where the habitable zone is largely, or partially, unperturbed by a nearby Jovian, and that mutual gravitational interactions and resonant mechanisms are capable of producing stable orbits even in habitable zones that are significantly or completely disrupted by a Jovian. Our results yield a list of 13 single Jovian planet systems in CELESTA that are not only capable of supporting an Earth-mass planet on stable orbits in their habitable zone, but for which we are also able to constrain the orbits of the Earth-mass planet such that the induced radial velocity signals would be detectable with next generation instruments.

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Section: Resultsmentioning

confidence: 99%

“…The CELESTA database calculates the HZs of nearby Sun-like stars, calculating the stellar properties needed to determine the HZs from Kopparapu et al (2014), and presents several possible HZ boundaries to choose from. As a large proportion of the exoplanet population is observed around non-Sun-like stars (e.g.…”

Section: Exoplanet Populationmentioning

confidence: 99%

Stable habitable zones of single Jovian planet systems

Agnew

Maddison

Thilliez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…We use here the common definition of a habitable climate that liquid water is stable at the surface (Kasting et al 1993). Important parameters influencing the habitability of a planet are its mass, its atmospheric composition and the intensity and the spectrum of the stellar flux it receives (Kasting et al 1993;Kopparapu et al 2014). Recently, it has been shown that furthermore the rotation period of a planet around its own axis influences its habitability .…”

Section: Introductionmentioning

confidence: 99%

The role of sea-ice albedo in the climate of slowly rotating aquaplanets

2017

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We investigate the influence of the rotation period (Prot) on the mean climate of an aquaplanet, with a focus on the role of sea-ice albedo. We perform aquaplanet simulations with the atmospheric general circulation model ECHAM6 for various rotation periods from one Earth-day to 365 Earth-days in which case the planet is synchronously rotating. The global-mean surface temperature decreases with increasing Prot and sea ice expands equatorwards. The cooling of the mean climate with increasing Prot is caused partly by the high surface albedo of sea ice on the dayside and partly by the high albedo of the deep convective clouds over the substellar region. The cooling caused by these deep convective clouds is weak for non-synchronous rotations compared to synchronous rotation. Sensitivity simulations with the sea-ice model switched off show that the global-mean surface temperature is up to 27 K higher than in our main simulations with sea ice and thus highlight the large influence of sea ice on the climate. We present the first estimates of the influence of the rotation period on the transition of an Earth-like climate to global glaciation. Our results suggest that global glaciation of planets with synchronous rotation occurs at substantially lower incoming solar irradiation than for planets with slow but non-synchronous rotation

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“…Most commonly, this term is applied to individual star systems. Radiative transfer calculations of the atmospheric response of an Earthlike planet to insolation (Kasting, Whitmire & Reynolds, 1993;Kopparapu et al, 2013Kopparapu et al, , 2014 allow the identification of planetary orbits that permit surface liquid water. This is the principal definition of "the habitable zone", and we henceforth refer to it as the stellar habitable zone (SHZ).…”

Section: Introductionmentioning

confidence: 99%

Evaluating galactic habitability using high-resolution cosmological simulations of galaxy formation

Forgan

Dayal

Cockell

et al. 2016

International Journal of Astrobiology

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We present the first model that couples high-resolution simulations of the formation of Local Group galaxies with calculations of the galactic habitable zone (GHZ), a region of space which has sufficient metallicity to form terrestrial planets without being subject to hazardous radiation. These simulations allow us to make substantial progress in mapping out the asymmetric three-dimensional GHZ and its time evolution for the Milky Way (MW) and Triangulum (M33) galaxies, as opposed to works that generally assume an azimuthally symmetric GHZ.Applying typical habitability metrics to MW and M33, we find that while a large number of habitable planets exist as close as a few kiloparsecs from the galactic centre, the probability of individual planetary systems being habitable rises as one approaches the edge of the stellar disc. Tidal streams and satellite galaxies also appear to be fertile grounds for habitable planet formation.In short, we find that both galaxies arrive at similar GHZs by different evolutionary paths, as measured by the first and third quartiles of surviving biospheres. For the Milky Way, this interquartile range begins as a narrow band at large radii, expanding to encompass much of the galaxy at intermediate times before settling at a range of 2-13kpc. In the case of M33, the opposite behaviour occurs -the initial and final interquartile ranges are quite similar, showing gradual evolution. This suggests that galaxy assembly history strongly influences the time evolution of the GHZ, which will affect the relative time lag between biospheres in different galactic locations. We end by noting the caveats involved in such studies and demonstrate that high resolution cosmological simulations will play a vital role in understanding habitability on galactic scales, provided that these simulations accurately resolve chemical evolution.

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Habitable Zones Around Main-Sequence Stars: Dependence on Planetary Mass

Cited by 585 publications

References 45 publications

Stable habitable zones of single Jovian planet systems

Stable habitable zones of single Jovian planet systems

The role of sea-ice albedo in the climate of slowly rotating aquaplanets

Evaluating galactic habitability using high-resolution cosmological simulations of galaxy formation

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