Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko
Aims. We provide a detailed quantitative analysis of isolated boulder fields situated in three different regions of comet 67P/Churyumov-Gerasimenko: Imhotep, Hapi, and Hatmehit. This is done to supply a useful method for analyzing the morphology of the boulders and to characterize the regions themse...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Formato: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2019 |
| País: | España |
| Recursos: | Instituto Nacional de Técnica Aeroespacial (INTA) |
| Repositorio: | DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
| OAI Identifier: | oai:digital.inta.es:20.500.12666/353 |
| Acesso em linha: | https://www.aanda.org/articles/aa/full_html/2019/10/aa34775-18/aa34775-18.html http://hdl.handle.net/20.500.12666/353 |
| Access Level: | acceso abierto |
| Palavra-chave: | Comets: general Comets: individual: 67P/Churyumov-Gerasimenko Methods: data analysis |
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| dc.title.none.fl_str_mv |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| title |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| spellingShingle |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko Cambianica, P. Comets: general Comets: individual: 67P/Churyumov-Gerasimenko Methods: data analysis |
| title_short |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| title_full |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| title_fullStr |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| title_full_unstemmed |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| title_sort |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko |
| dc.creator.none.fl_str_mv |
Cambianica, P. Cremonese, G. Naletto, G. Lucchetti, A. Pajola, M. Penasa, L. Simioni, E. Massironi, M. Ferrari, S. Bodewits, D. La Forgia, F. Sierks, H. Lamy, Philippe Rodrigo, Rafael Koschny, D. Davidsson, B. J. R. Barucci, M. A. Bertaux, J. L. Bertini, I. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Fornasier, S. Fulle, M. Gutiérrez, Pedro J. Güttler, C. Ip, W. H. Keller, H. U. Lara, L. M. Lazzarin, M. Lin, Z. Y. López Moreno, J. J. Marzari, F. Mottola, S. Shi, X. Scholten, F. Toth, I. Tubiana, C. Vicent, J. B. |
| author |
Cambianica, P. |
| author_facet |
Cambianica, P. Cremonese, G. Naletto, G. Lucchetti, A. Pajola, M. Penasa, L. Simioni, E. Massironi, M. Ferrari, S. Bodewits, D. La Forgia, F. Sierks, H. Lamy, Philippe Rodrigo, Rafael Koschny, D. Davidsson, B. J. R. Barucci, M. A. Bertaux, J. L. Bertini, I. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Fornasier, S. Fulle, M. Gutiérrez, Pedro J. Güttler, C. Ip, W. H. Keller, H. U. Lara, L. M. Lazzarin, M. Lin, Z. Y. López Moreno, J. J. Marzari, F. Mottola, S. Shi, X. Scholten, F. Toth, I. Tubiana, C. Vicent, J. B. |
| author_role |
author |
| author2 |
Cremonese, G. Naletto, G. Lucchetti, A. Pajola, M. Penasa, L. Simioni, E. Massironi, M. Ferrari, S. Bodewits, D. La Forgia, F. Sierks, H. Lamy, Philippe Rodrigo, Rafael Koschny, D. Davidsson, B. J. R. Barucci, M. A. Bertaux, J. L. Bertini, I. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Fornasier, S. Fulle, M. Gutiérrez, Pedro J. Güttler, C. Ip, W. H. Keller, H. U. Lara, L. M. Lazzarin, M. Lin, Z. Y. López Moreno, J. J. Marzari, F. Mottola, S. Shi, X. Scholten, F. Toth, I. Tubiana, C. Vicent, J. B. |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.contributor.none.fl_str_mv |
Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737 https://orcid.org/0000-0002-8091-4915 |
| dc.subject.none.fl_str_mv |
Comets: general Comets: individual: 67P/Churyumov-Gerasimenko Methods: data analysis |
| topic |
Comets: general Comets: individual: 67P/Churyumov-Gerasimenko Methods: data analysis |
| description |
Aims. We provide a detailed quantitative analysis of isolated boulder fields situated in three different regions of comet 67P/Churyumov-Gerasimenko: Imhotep, Hapi, and Hatmehit. This is done to supply a useful method for analyzing the morphology of the boulders and to characterize the regions themselves. Methods. We used OSIRIS Narrow Angle Camera images with a spatial scale smaller than 2 m px−1 and analyzed the size-frequency distribution and the cumulative fractional area per boulder population. In addition, we correlated shape parameters, such as circularity and solidity, with both the spatial and the size-frequency distribution of the three populations. Results. We identified 11 811 boulders in the Imhotep, Hapi, and Hatmehit regions. We found that the Hatmehit and Imhotep areas show power indices in the range of −2.3/−2.7. These values could represent a transition between gravitational events caused by thermal weathering and sublimation, and material formed during collapses that has undergone sublimation. The Hapi area is characterized by a lower power index (−1.2/−1.7), suggesting that those boulders have a different origin. They can be the result of material formed during gravitational events and collapses that has undergone continuous fragmentation. We calculated the cumulative fractional area (CFA) in order to investigate how the area is covered by boulders as a function of their sizes. The Hatmehit and Imhotep regions show a CFA that is well fit by a power law. In contrast, the Hapi area does not show the same trend. We analyzed the fractal distributions, finding that the populations seem to be fractal at all dimensions, except for the Hapi distribution, which shows a possible fractal behavior for small dimensions only. Finally, the average values of the shape parameters reveal solid and roundish boulders in all populations we studied. |
| publishDate |
2019 |
| dc.date.none.fl_str_mv |
2019 2021 2021 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 |
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article |
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publishedVersion |
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https://www.aanda.org/articles/aa/full_html/2019/10/aa34775-18/aa34775-18.html http://hdl.handle.net/20.500.12666/353 |
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https://www.aanda.org/articles/aa/full_html/2019/10/aa34775-18/aa34775-18.html http://hdl.handle.net/20.500.12666/353 |
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Inglés |
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Inglés |
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Attribution-NonCommercial-NoDerivatives 4.0 International © ESO 2019 https://creativecommons.org/licenses/by-nc-nd/4.0/ info:eu-repo/semantics/openAccess |
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Attribution-NonCommercial-NoDerivatives 4.0 International © ESO 2019 https://creativecommons.org/licenses/by-nc-nd/4.0/ |
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openAccess |
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application/pdf |
| dc.publisher.none.fl_str_mv |
EDP Sciences |
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EDP Sciences |
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reponame:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial instname:Instituto Nacional de Técnica Aeroespacial (INTA) |
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Instituto Nacional de Técnica Aeroespacial (INTA) |
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DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
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DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
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Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-GerasimenkoCambianica, P.Cremonese, G.Naletto, G.Lucchetti, A.Pajola, M.Penasa, L.Simioni, E.Massironi, M.Ferrari, S.Bodewits, D.La Forgia, F.Sierks, H.Lamy, PhilippeRodrigo, RafaelKoschny, D.Davidsson, B. J. R.Barucci, M. A.Bertaux, J. L.Bertini, I.Da Deppo, V.Debei, S.De Cecco, M.Deller, J.Fornasier, S.Fulle, M.Gutiérrez, Pedro J.Güttler, C.Ip, W. H.Keller, H. U.Lara, L. M.Lazzarin, M.Lin, Z. Y.López Moreno, J. J.Marzari, F.Mottola, S.Shi, X.Scholten, F.Toth, I.Tubiana, C.Vicent, J. B.Comets: generalComets: individual: 67P/Churyumov-GerasimenkoMethods: data analysisAims. We provide a detailed quantitative analysis of isolated boulder fields situated in three different regions of comet 67P/Churyumov-Gerasimenko: Imhotep, Hapi, and Hatmehit. This is done to supply a useful method for analyzing the morphology of the boulders and to characterize the regions themselves. Methods. We used OSIRIS Narrow Angle Camera images with a spatial scale smaller than 2 m px−1 and analyzed the size-frequency distribution and the cumulative fractional area per boulder population. In addition, we correlated shape parameters, such as circularity and solidity, with both the spatial and the size-frequency distribution of the three populations. Results. We identified 11 811 boulders in the Imhotep, Hapi, and Hatmehit regions. We found that the Hatmehit and Imhotep areas show power indices in the range of −2.3/−2.7. These values could represent a transition between gravitational events caused by thermal weathering and sublimation, and material formed during collapses that has undergone sublimation. The Hapi area is characterized by a lower power index (−1.2/−1.7), suggesting that those boulders have a different origin. They can be the result of material formed during gravitational events and collapses that has undergone continuous fragmentation. We calculated the cumulative fractional area (CFA) in order to investigate how the area is covered by boulders as a function of their sizes. The Hatmehit and Imhotep regions show a CFA that is well fit by a power law. In contrast, the Hapi area does not show the same trend. We analyzed the fractal distributions, finding that the populations seem to be fractal at all dimensions, except for the Hapi distribution, which shows a possible fractal behavior for small dimensions only. Finally, the average values of the shape parameters reveal solid and roundish boulders in all populations we studied.OSIRIS was built by a consortium of the Max-Planck Institut fur Sonnensystemforschung, in Guttingen, Germany, CISAS University of Padova, Italy, the Laboratoire de Astrophysique de Marseille, France, the Instituto de Astrofisica de Andalucia, CSIC, Granada, Spain, the Research and Scientific Support Department of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Tecnica Aeroespacial, Madrid, Spain, the Universidad Politechnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut fur Datentechnik und Kommunikationsnetze der Technischen Universitat Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. We thank the ESA teams at ESAC, ESOC and ESTEC for their work in support of the Rosetta mission. We made use of Arcgis 10.3.1 software together with the Matlab, Java, and ImageJ software to perform our analysis. I thank Frederic Moisy for sharing the box-count work; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)Peer reviewEDP SciencesUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737https://orcid.org/0000-0002-8091-4915202120212019info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501application/pdfhttps://www.aanda.org/articles/aa/full_html/2019/10/aa34775-18/aa34775-18.htmlhttp://hdl.handle.net/20.500.12666/353reponame:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacialinstname:Instituto Nacional de Técnica Aeroespacial (INTA)InglésAttribution-NonCommercial-NoDerivatives 4.0 International© ESO 2019https://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:digital.inta.es:20.500.12666/3532026-06-23T12:46:37Z |
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15,300719 |