The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta
Remote sensing observations of dust particles ejected from comets provide important hints on the intimate nature of the materials composing these primitive objects. The measurement of dust coma backscattering ratio, BSR, defined as the ratio of the reflectance at phase angle 0° and 30°, helps tuning...
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2019 |
| País: | España |
| Institución: | Instituto Nacional de Técnica Aeroespacial (INTA) |
| Repositorio: | DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
| OAI Identifier: | oai:digital.inta.es:20.500.12666/375 |
| Acceso en línea: | https://academic.oup.com/mnras/article/482/3/2924/5142315 http://hdl.handle.net/20.500.12666/375 |
| Access Level: | acceso abierto |
| Palabra clave: | Scattering Methods: data analysis Techniques: image processing Techniques: photometric Comets: individual: 67P Churyumov–Gerasimenko |
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| dc.title.none.fl_str_mv |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| title |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| spellingShingle |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta Bertini, I. Scattering Methods: data analysis Techniques: image processing Techniques: photometric Comets: individual: 67P Churyumov–Gerasimenko |
| title_short |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| title_full |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| title_fullStr |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| title_full_unstemmed |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| title_sort |
The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard Rosetta |
| dc.creator.none.fl_str_mv |
Bertini, I. La Forgia, F. Fulle, M. Tubiana, C. Güttler, C. Moreno, F. Agarwal, J. Muñoz, O. Mottola, S. Ivanovsky, S. Pajola, M. Lucchetti, A. Petropoulou, V. Lazzarin, M. Rotundi, A. Bodewits, D. Frattin, E. Toth, I. Masoumzadeh, N. Kovács, G. Rinaldi, G. Guirado, D. Sierks, H. Naletto, G. Lamy, Philippe Rodrigo, Rafael Koschny, D. Davidsson, B. J. R. Barbieri, C. Barucci, M. A. Bertaux, J. L. Cambianica, P. Cremonese, G. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Ferrari, S. Ferri, F. Fornasier, S. Gutiérrez, Pedro J. Hasselmann, P. H. Ip, W. H. Keller, H. U. Lara, L. M. López Moreno, J. J. Marzari, F. Massironi, M. Penasa, L. Shi, X. |
| author |
Bertini, I. |
| author_facet |
Bertini, I. La Forgia, F. Fulle, M. Tubiana, C. Güttler, C. Moreno, F. Agarwal, J. Muñoz, O. Mottola, S. Ivanovsky, S. Pajola, M. Lucchetti, A. Petropoulou, V. Lazzarin, M. Rotundi, A. Bodewits, D. Frattin, E. Toth, I. Masoumzadeh, N. Kovács, G. Rinaldi, G. Guirado, D. Sierks, H. Naletto, G. Lamy, Philippe Rodrigo, Rafael Koschny, D. Davidsson, B. J. R. Barbieri, C. Barucci, M. A. Bertaux, J. L. Cambianica, P. Cremonese, G. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Ferrari, S. Ferri, F. Fornasier, S. Gutiérrez, Pedro J. Hasselmann, P. H. Ip, W. H. Keller, H. U. Lara, L. M. López Moreno, J. J. Marzari, F. Massironi, M. Penasa, L. Shi, X. |
| author_role |
author |
| author2 |
La Forgia, F. Fulle, M. Tubiana, C. Güttler, C. Moreno, F. Agarwal, J. Muñoz, O. Mottola, S. Ivanovsky, S. Pajola, M. Lucchetti, A. Petropoulou, V. Lazzarin, M. Rotundi, A. Bodewits, D. Frattin, E. Toth, I. Masoumzadeh, N. Kovács, G. Rinaldi, G. Guirado, D. Sierks, H. Naletto, G. Lamy, Philippe Rodrigo, Rafael Koschny, D. Davidsson, B. J. R. Barbieri, C. Barucci, M. A. Bertaux, J. L. Cambianica, P. Cremonese, G. Da Deppo, V. Debei, S. De Cecco, M. Deller, J. Ferrari, S. Ferri, F. Fornasier, S. Gutiérrez, Pedro J. Hasselmann, P. H. Ip, W. H. Keller, H. U. Lara, L. M. López Moreno, J. J. Marzari, F. Massironi, M. Penasa, L. Shi, X. |
| 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 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 Fulle, M. [0000-0001-8435-5287] Tubiana, C. [0000-0001-8475-9898] Güttler, C. [0000-0003-4277-1738] Pajola, M. [0000-0002-3144-1277] Rinaldi, G. [0000-0002-2968-0455] Naletto, G. [0000-0003-2007-3138] Barucci, M. A. [0000-0002-1345-0890] Bertaux, J. L. [0000-0003-0333-229X] Deller, J. [0000-0001-8341-007X] Fornasier, S. [0000-0001-7678-3310] Penasa, L. [0000-0002-6394-3108] |
| dc.subject.none.fl_str_mv |
Scattering Methods: data analysis Techniques: image processing Techniques: photometric Comets: individual: 67P Churyumov–Gerasimenko |
| topic |
Scattering Methods: data analysis Techniques: image processing Techniques: photometric Comets: individual: 67P Churyumov–Gerasimenko |
| description |
Remote sensing observations of dust particles ejected from comets provide important hints on the intimate nature of the materials composing these primitive objects. The measurement of dust coma backscattering ratio, BSR, defined as the ratio of the reflectance at phase angle 0° and 30°, helps tuning theoretical models aimed at solving the inverse scattering problem deriving information on the nature of the ejected particles. The Rosetta/OSIRIS camera sampled the coma phase function of comet 67P, with four series acquired at low phase angles from 2015 January to 2016 May. We also added previously published data to our analysis to increase the temporal resolution of our findings. We measured a BSR in the range ∼ [1.7–3.6], broader than the range found in literature from ground-based observations of other comets. We found that during the post-perihelion phase, the BSR is systematically larger than the classical cometary dust values only for nucleocentric distances smaller than ∼100 km. We explain this trend in terms of a cloud of chunks orbiting the nucleus at distances <100 km ejected during perihelion and slowly collapsing on the nucleus over a few months because of the coma gas drag. This also implies that the threshold particle size for the dust phase function to become similar to the nucleus phase function is between 2.5 mm and 0.1 m, taking into account previous Rosetta findings. |
| 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 |
| dc.identifier.none.fl_str_mv |
https://academic.oup.com/mnras/article/482/3/2924/5142315 http://hdl.handle.net/20.500.12666/375 |
| url |
https://academic.oup.com/mnras/article/482/3/2924/5142315 http://hdl.handle.net/20.500.12666/375 |
| dc.language.none.fl_str_mv |
Inglés |
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Inglés |
| dc.rights.none.fl_str_mv |
Attribution-NonCommercial-NoDerivatives 4.0 International Copyright © 2018, Oxford University Press https://creativecommons.org/licenses/by-nc-nd/4.0/ info:eu-repo/semantics/openAccess |
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Attribution-NonCommercial-NoDerivatives 4.0 International Copyright © 2018, Oxford University Press https://creativecommons.org/licenses/by-nc-nd/4.0/ |
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openAccess |
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application/pdf |
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Oxford Academics: Oxford University Press |
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Oxford Academics: Oxford University Press |
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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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DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
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1869407852153536512 |
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The backscattering ratio of comet 67P/Churyumov–Gerasimenko dust coma as seen by OSIRIS onboard RosettaBertini, I.La Forgia, F.Fulle, M.Tubiana, C.Güttler, C.Moreno, F.Agarwal, J.Muñoz, O.Mottola, S.Ivanovsky, S.Pajola, M.Lucchetti, A.Petropoulou, V.Lazzarin, M.Rotundi, A.Bodewits, D.Frattin, E.Toth, I.Masoumzadeh, N.Kovács, G.Rinaldi, G.Guirado, D.Sierks, H.Naletto, G.Lamy, PhilippeRodrigo, RafaelKoschny, D.Davidsson, B. J. R.Barbieri, C.Barucci, M. A.Bertaux, J. L.Cambianica, P.Cremonese, G.Da Deppo, V.Debei, S.De Cecco, M.Deller, J.Ferrari, S.Ferri, F.Fornasier, S.Gutiérrez, Pedro J.Hasselmann, P. H.Ip, W. H.Keller, H. U.Lara, L. M.López Moreno, J. J.Marzari, F.Massironi, M.Penasa, L.Shi, X.ScatteringMethods: data analysisTechniques: image processingTechniques: photometricComets: individual: 67PChuryumov–GerasimenkoRemote sensing observations of dust particles ejected from comets provide important hints on the intimate nature of the materials composing these primitive objects. The measurement of dust coma backscattering ratio, BSR, defined as the ratio of the reflectance at phase angle 0° and 30°, helps tuning theoretical models aimed at solving the inverse scattering problem deriving information on the nature of the ejected particles. The Rosetta/OSIRIS camera sampled the coma phase function of comet 67P, with four series acquired at low phase angles from 2015 January to 2016 May. We also added previously published data to our analysis to increase the temporal resolution of our findings. We measured a BSR in the range ∼ [1.7–3.6], broader than the range found in literature from ground-based observations of other comets. We found that during the post-perihelion phase, the BSR is systematically larger than the classical cometary dust values only for nucleocentric distances smaller than ∼100 km. We explain this trend in terms of a cloud of chunks orbiting the nucleus at distances <100 km ejected during perihelion and slowly collapsing on the nucleus over a few months because of the coma gas drag. This also implies that the threshold particle size for the dust phase function to become similar to the nucleus phase function is between 2.5 mm and 0.1 m, taking into account previous Rosetta findings.Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) was built by a consortium of the Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany, Centro di Ateneo di Studi e Attività Spaziali (CISAS) – University of Padova, Italy, the Laboratoire d’ Astrophysique de Marseille, France, the Instituto de Astrofísica de Andalucia, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain, the Research and Scientific Support Department of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Técnica Aeroespacial, Madrid, Spain, the Universidad Politéchnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut für Datentechnik und Kommunikationsnetze der Technischen Universität Braunschweig, Germany. The support of the national funding agencies of Germany (DLR: Deutschen Zentrums für Luft-und Raumfahrt), France (CNES: Centre national d'études spatiales), Italy (ASI: Agenzia Spaziale Italiana), Spain (MEC: Ministry of Education & Science), Sweden (SNSB: Swedish National Space Board), and the European Space Agency (ESA) Technical Directorate is gratefully acknowledged; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737).Peer reviewOxford Academics: Oxford University PressUnidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737Fulle, M. [0000-0001-8435-5287]Tubiana, C. [0000-0001-8475-9898]Güttler, C. [0000-0003-4277-1738]Pajola, M. [0000-0002-3144-1277]Rinaldi, G. [0000-0002-2968-0455]Naletto, G. [0000-0003-2007-3138]Barucci, M. A. [0000-0002-1345-0890]Bertaux, J. L. [0000-0003-0333-229X]Deller, J. [0000-0001-8341-007X]Fornasier, S. [0000-0001-7678-3310]Penasa, L. [0000-0002-6394-3108]202120212019info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501application/pdfhttps://academic.oup.com/mnras/article/482/3/2924/5142315http://hdl.handle.net/20.500.12666/375reponame:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacialinstname:Instituto Nacional de Técnica Aeroespacial (INTA)InglésAttribution-NonCommercial-NoDerivatives 4.0 InternationalCopyright © 2018, Oxford University Presshttps://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:digital.inta.es:20.500.12666/3752026-06-23T12:46:37Z |
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