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dc.contributor.authorForgan, Duncan
dc.contributor.authorDayal, Pratika
dc.contributor.authorCockell, Charles
dc.contributor.authorLibeskind, Noam
dc.date.accessioned2016-07-28T23:31:15Z
dc.date.available2016-07-28T23:31:15Z
dc.date.issued2017-01
dc.identifier.citationForgan , D , Dayal , P , Cockell , C & Libeskind , N 2017 , ' Evaluating galactic habitability using high-resolution cosmological simulations of galaxy formation ' , International Journal of Astrobiology , vol. 16 , no. 1 , pp. 60-73 . https://doi.org/10.1017/S1473550415000518en
dc.identifier.issn1473-5504
dc.identifier.otherPURE: 240936178
dc.identifier.otherPURE UUID: 66c3cc6d-4ede-4023-ba58-b27bc2bcc1d1
dc.identifier.otherScopus: 84955587503
dc.identifier.otherWOS: 000390350600007
dc.identifier.urihttp://hdl.handle.net/10023/9224
dc.descriptionD. F. acknowledges support from STFC consolidated grant ST/J001422/1, and the ‘ECOGAL’ ERC Advanced Grant. P. D. acknowledges the support of the Addison Wheeler Fellowship awarded by the Institute of Advanced Study at Durham University. N. I. L. is supported by the Deutsche Forschungs Gemeinschaft (DFG).en
dc.description.abstractWe 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 MW, 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 2–13 kpc. 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.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofInternational Journal of Astrobiologyen
dc.rightsCopyright © Cambridge University Press 2016. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at http://dx.doi.org/10.1017/S1473550415000518en
dc.subjectGalactic habitable zoneen
dc.subjectMilky Wayen
dc.subjectNumerical simulationsen
dc.subjectTriangulumen
dc.subjectQC Physicsen
dc.subjectQB Astronomyen
dc.subjectSpace and Planetary Scienceen
dc.subjectEcology, Evolution, Behavior and Systematicsen
dc.subjectPhysics and Astronomy (miscellaneous)en
dc.subjectEarth and Planetary Sciences (miscellaneous)en
dc.subject3rd-DASen
dc.subject.lccQCen
dc.subject.lccQBen
dc.titleEvaluating galactic habitability using high-resolution cosmological simulations of galaxy formationen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1017/S1473550415000518
dc.description.statusPeer revieweden
dc.date.embargoedUntil2016-07-29


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