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dc.contributor.authorBuchanan, L.E.
dc.contributor.authorSchwamb, M.E.
dc.contributor.authorFraser, W.C.
dc.contributor.authorBannister, M.T.
dc.contributor.authorMarsset, M.
dc.contributor.authorPike, R.E.
dc.contributor.authorNesvorný, D.
dc.contributor.authorKavelaars, J.J.
dc.contributor.authorBenecchi, S.D.
dc.contributor.authorLehner, M.J.
dc.contributor.authorWang, S.-Y.
dc.contributor.authorPeixinho, N.
dc.contributor.authorVolk, K.
dc.contributor.authorAlexandersen, M.
dc.contributor.authorChen, Y.-T.
dc.contributor.authorGladman, B.
dc.contributor.authorGwyn, S.
dc.contributor.authorPetit, J.-M.
dc.date.accessioned2022-03-17T01:57:22Z
dc.date.available2022-03-17T01:57:22Z
dc.date.issued2022
dc.identifier.citationBuchanan, L. E., Schwamb, M. E., Fraser, W. C., Bannister, M. T., Marsset, M., Pike, R. E., Nesvorný, D., Kavelaars, J. J., Benecchi, S. D., Lehner, M. J., Wang, S.-Y., Peixinho, N., Volk, K., Alexandersen, M., Chen, Y.-T., Gladman, B., Gwyn, S., & Petit, J.-M. (2022). Col-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations. Planetary Science Journal.
dc.identifier.issn2632-3338
dc.identifier.doi10.3847/PSJ/ac42c9
dc.identifier.urihttp://hdl.handle.net/10150/663620
dc.description.abstractDynamically excited objects within the Kuiper Belt show a bimodal distribution in their surface colors, and these differing surface colors may be a tracer of where these objects formed. In this work, we explore radial color distributions in the primordial planetesimal disk and implications for the positions of ice line/color transitions within the Kuiper Belt’s progenitor populations. We combine a full dynamical model of the Kuiper Belt’s evolution due to Neptune’s migration with precise surface colors measured by the Colours of the Outer Solar System Origins Survey in order to examine the true color ratios within the Kuiper Belt and the ice lines within the primordial disk. We investigate the position of a dominant, surface color–changing ice line, with two possible surface color layouts within the initial disk: (1) inner neutral surfaces and outer red and (2) inner red surfaces and outer neutral. We performed simulations with a primordial disk that truncates at 30 au. By radially stepping the color transition out through 0.5 au intervals, we show that both disk configurations are consistent with the observed color fraction. For an inner neutral, outer red primordial disk, we find that the color transition can be at 28-+32 au at a 95% confidence level. For an inner red, outer neutral primordial disk, the color transition can be at 27-+33 au at a 95% confidence level. © 2022. The Author(s). Published by the American Astronomical Society.
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.rightsCopyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.titleCol-OSSOS: Probing Ice Line/Color Transitions within the Kuiper Belt’s Progenitor Populations
dc.typeArticle
dc.typetext
dc.contributor.departmentLunar and Planetary Laboratory, University of Arizona
dc.identifier.journalPlanetary Science Journal
dc.description.noteOpen access journal
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
dc.eprint.versionFinal published version
dc.source.journaltitlePlanetary Science Journal
refterms.dateFOA2022-03-17T01:57:22Z


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Copyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
Except where otherwise noted, this item's license is described as Copyright © 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.