Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-Gerasimenko
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....
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2019 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/204128 |
| Acceso en línea: | http://hdl.handle.net/10261/204128 |
| Access Level: | acceso abierto |
| Palabra clave: | Comets: general Comets: individual: 67P/Churyumov-Gerasimenko Methods: data analysis |
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ES_33cb8428d0b93d3f95bfe0346a77bf2c |
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oai:digital.csic.es:10261/204128 |
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España |
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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, Alice Pajola, M. Penasa, L. Simioni, E. Massironi, M. Ferrari, S. Bodewits, D. La Forgia, F. Sierks, H. Lamy, P.L. Rodrigo Montero, Rafael Koschny, D. Dayidsson, B Barucci, M.A. Bertaux, J.L. Bertini, I. Da Deppo, Vania Debei, S. De Cecco, M. Deller, J. Fornasier, S. Fulle, M. Gutiérrez, Pedro J. Güttler, C. Ip, W. H. Keller, H.U. Lara, Luisa María Lazzarin, M. Lin, Zhong-Yi López-Moreno, José Juan Marzari, F. Mottola, S. Shi, X. Scholten, F. Toth, I. Tubiana, C. Vincent, J.B. |
| author |
Cambianica, P. |
| author_facet |
Cambianica, P. Cremonese, G. Naletto, G. Lucchetti, Alice Pajola, M. Penasa, L. Simioni, E. Massironi, M. Ferrari, S. Bodewits, D. La Forgia, F. Sierks, H. Lamy, P.L. Rodrigo Montero, Rafael Koschny, D. Dayidsson, B Barucci, M.A. Bertaux, J.L. Bertini, I. Da Deppo, Vania Debei, S. De Cecco, M. Deller, J. Fornasier, S. Fulle, M. Gutiérrez, Pedro J. Güttler, C. Ip, W. H. Keller, H.U. Lara, Luisa María Lazzarin, M. Lin, Zhong-Yi López-Moreno, José Juan Marzari, F. Mottola, S. Shi, X. Scholten, F. Toth, I. Tubiana, C. Vincent, J.B. |
| author_role |
author |
| author2 |
Cremonese, G. Naletto, G. Lucchetti, Alice Pajola, M. Penasa, L. Simioni, E. Massironi, M. Ferrari, S. Bodewits, D. La Forgia, F. Sierks, H. Lamy, P.L. Rodrigo Montero, Rafael Koschny, D. Dayidsson, B Barucci, M.A. Bertaux, J.L. Bertini, I. Da Deppo, Vania Debei, S. De Cecco, M. Deller, J. Fornasier, S. Fulle, M. Gutiérrez, Pedro J. Güttler, C. Ip, W. H. Keller, H.U. Lara, Luisa María Lazzarin, M. Lin, Zhong-Yi López-Moreno, José Juan Marzari, F. Mottola, S. Shi, X. Scholten, F. Toth, I. Tubiana, C. Vincent, 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 |
German Centre for Air and Space Travel Centre National D'Etudes Spatiales (France) Agenzia Spaziale Italiana Agencia Estatal de Investigación (España) European Space Agency Swedish National Space Agency Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72] |
| 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 |
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 mpx(-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.© ESO 2019 |
| publishDate |
2019 |
| dc.date.none.fl_str_mv |
2019 2020 2020 2020 |
| dc.type.none.fl_str_mv |
info:eu-repo/semantics/article http://purl.org/coar/resource_type/c_6501 Publisher's version info:eu-repo/semantics/publishedVersion |
| format |
article |
| status_str |
publishedVersion |
| dc.identifier.none.fl_str_mv |
http://hdl.handle.net/10261/204128 |
| url |
http://hdl.handle.net/10261/204128 |
| dc.language.none.fl_str_mv |
Inglés |
| language_invalid_str_mv |
Inglés |
| dc.relation.none.fl_str_mv |
http://dx.doi.org/10.1051/0004-6361/201834775 Sí |
| dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess |
| eu_rights_str_mv |
openAccess |
| dc.publisher.none.fl_str_mv |
EDP Sciences |
| publisher.none.fl_str_mv |
EDP Sciences |
| dc.source.none.fl_str_mv |
reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC instname:Consejo Superior de Investigaciones Científicas (CSIC) |
| instname_str |
Consejo Superior de Investigaciones Científicas (CSIC) |
| reponame_str |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| collection |
DIGITAL.CSIC. Repositorio Institucional del CSIC |
| repository.name.fl_str_mv |
|
| repository.mail.fl_str_mv |
|
| _version_ |
1869405769779118080 |
| spelling |
Quantitative analysis of isolated boulder fields on comet 67P/Churyumov-GerasimenkoCambianica, P.Cremonese, G.Naletto, G.Lucchetti, AlicePajola, M.Penasa, L.Simioni, E.Massironi, M.Ferrari, S.Bodewits, D.La Forgia, F.Sierks, H.Lamy, P.L.Rodrigo Montero, RafaelKoschny, D.Dayidsson, BBarucci, M.A.Bertaux, J.L.Bertini, I.Da Deppo, VaniaDebei, S.De Cecco, M.Deller, J.Fornasier, S.Fulle, M.Gutiérrez, Pedro J.Güttler, C.Ip, W. H.Keller, H.U.Lara, Luisa MaríaLazzarin, M.Lin, Zhong-YiLópez-Moreno, José JuanMarzari, F.Mottola, S.Shi, X.Scholten, F.Toth, I.Tubiana, C.Vincent, J.B.Comets: generalComets: individual: 67P/Churyumov-GerasimenkoMethods: data analysisWe 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 mpx(-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.© ESO 2019OSIRIS 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.EDP SciencesGerman Centre for Air and Space TravelCentre National D'Etudes Spatiales (France)Agenzia Spaziale ItalianaAgencia Estatal de Investigación (España)European Space AgencySwedish National Space AgencyConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2020202020192020info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/204128reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://dx.doi.org/10.1051/0004-6361/201834775Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2041282026-05-22T06:33:51Z |
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15,812429 |