67P/churyumov-gerasimenko: Activity between March and June 2014 as observed from Rosetta/OSIRIS (Articolo in rivista)

Type
Label
  • 67P/churyumov-gerasimenko: Activity between March and June 2014 as observed from Rosetta/OSIRIS (Articolo in rivista) (literal)
Anno
  • 2015-01-01T00:00:00+01:00 (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#doi
  • 10.1051/0004-6361/201424735 (literal)
Alternative label
  • Tubiana C.; Snodgrass C.; Bertini I.; Mottola S.; Vincent J.-B.; Lara L.; Fornasier S.; Knollenberg J.; Thomas N.; Fulle M.; Agarwal J.; Bodewits D.; Ferri F.; Guttler C.; Gutierrez P.J.; La Forgia F.; Lowry S.; Magrin S.; Oklay N.; Pajola M.; Rodrigo R.; Sierks H.; A'hearn M.F.; Angrilli F.; Barbieri C.; Barucci M.A.; Bertaux J.-L.; Cremonese G.; Da Deppo V.; Davidsson B.; De Cecco M.; Debei S.; Groussin O.; Hviid S.F.; Ip W.; Jorda L.; Keller H.U.; Koschny D.; Kramm R.; Kuhrt E.; Kuppers M.; Lazzarin M.; Lamy P.L.; Lopez Moreno J.J.; Marzari F.; Michalik H.; Naletto G.; Rickman H.; Sabau L.; Wenzel K.-P. (2015)
    67P/churyumov-gerasimenko: Activity between March and June 2014 as observed from Rosetta/OSIRIS
    in Astronomy & astrophysics (Online)
    (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori
  • Tubiana C.; Snodgrass C.; Bertini I.; Mottola S.; Vincent J.-B.; Lara L.; Fornasier S.; Knollenberg J.; Thomas N.; Fulle M.; Agarwal J.; Bodewits D.; Ferri F.; Guttler C.; Gutierrez P.J.; La Forgia F.; Lowry S.; Magrin S.; Oklay N.; Pajola M.; Rodrigo R.; Sierks H.; A'hearn M.F.; Angrilli F.; Barbieri C.; Barucci M.A.; Bertaux J.-L.; Cremonese G.; Da Deppo V.; Davidsson B.; De Cecco M.; Debei S.; Groussin O.; Hviid S.F.; Ip W.; Jorda L.; Keller H.U.; Koschny D.; Kramm R.; Kuhrt E.; Kuppers M.; Lazzarin M.; Lamy P.L.; Lopez Moreno J.J.; Marzari F.; Michalik H.; Naletto G.; Rickman H.; Sabau L.; Wenzel K.-P. (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#url
  • http://www.scopus.com/inward/record.url?eid=2-s2.0-84919633230&partnerID=q2rCbXpz (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#numeroVolume
  • 573 (literal)
Rivista
Note
  • Scopu (literal)
Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#affiliazioni
  • Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, Göttingen, 37077, Germany; Planetary and Space Sciences, Department of Physical Sciences, Open University, Walton Hall, Milton Keynes, MK7 6AA, United Kingdom; Center of Studies and Activities for Space (CISAS) G. Colombo, University of Padova, via Venezia 15, Padova, 35131, Italy; Institute of Planetary Research, DLR, Rutherfordstrasse 2, Berlin, 12489, Germany; Instituto de Astrofísica de Andalucía - CSIC, Granada, 18080, Spain; LESIA, Obs. de Paris, Univ Paris 06, 5 Place J. Janssen, Meudon, 92195, France; Physikalisches Institut, University of Bern, Sidlerstrasse 5, Bern, 3012, Switzerland; INAF - Osservatorio Astronomico di Trieste, via Tiepolo 11, Trieste, 34143, Italy; Department for Astronomy, University of Maryland, College Park, MD, 20742-2421, United States; Department of Physics and Astronomy G. Galilei, University of Padova, Vic. Osservatorio 3, Padova, 35122, Italy; Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, CT2 7NH, United Kingdom; Centro de Astrobiología, CSIC-INTA, Torrejón de Ardoz, Madrid, 28850, Spain; International Space Science Institute, Hallerstrasse 6, Bern, 3012, Switzerland; University of Padova, Department of Physics and Astronomy, vicolo dell'Osservatorio 3, Padova, 35122, Italy; LATMOS, CNRS/UVSQ/IPSL, 11 Boulevard d'Alembert, Guyancourt, 78280, France; INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, 35122, Italy; CNR-IFN UOS Padova LUXOR, via Trasea 7, Padova, 35131, Italy; Department of Physics and Astronomy, Uppsala University, Uppsala, 75120, Sweden; UNITN, Universitá di Trento, via Mesiano 77, Trento, 38100, Italy; Department of Mechanical Engineering, University of Padova, via Venezia 1, Padova, 35131, Italy; Aix Marseille Université, CNRS, LAM (Laboratoire d'Astro-physique de Marseille) UMR 7326, Marseille, 13388, France; Institute for Space Science, National Central University, Chung-Li, 32054, Taiwan; Institute for Geophysics and Extraterrestrial Physics, TU Braunschweig, Braunschweig, 38106, Germany; Research and Scientific Support Department, European Space Agency, Noordwijk, 2201, Netherlands; ESA/ESAC, PO Box 78, Villanueva de la Cañada, 28691, Spain; Dept. Physics, University of Padova, 35122 Padova, Italy; Institut für Datentechnik und Kommunikationsnetze, Braunschweig, 38106, Germany; Department of Information Engineering - University of Padova, via Gradenigo 6, Padova, 35131, Italy; PAS Space Reserch Center, Bartycka 18A, Warszawa, 00716, Poland; Instituto Nacional de Técnica Aeroespacial, Torrejon de Ardoz, 28850, Spain (literal)
Titolo
  • 67P/churyumov-gerasimenko: Activity between March and June 2014 as observed from Rosetta/OSIRIS (literal)
Abstract
  • Aims. 67P/Churyumov-Gerasimenko is the target comet of the ESA's Rosetta mission. After commissioning at the end of March 2014, the Optical, Spectroscopic, and Infrared Remote Imaging System (OSIRIS) onboard Rosetta, started imaging the comet and its dust environment to investigate how they change and evolve while approaching the Sun.,Methods. We focused our work on Narrow Angle Camera (NAC) orange images and Wide Angle Camera (WAC) red and visible-610 images acquired between 2014 March 23 and June 24 when the nucleus of 67P was unresolved and moving from approximately 4.3 AU to 3.8 AU inbound. During this period the 67P - Rosetta distance decreased from 5 million to 120 thousand km.,Results. Through aperture photometry, we investigated how the comet brightness varies with heliocentric distance. 67P was likely already weakly active at the end of March 2014, with excess flux above that expected for the nucleus. The comet's brightness was mostly constant during the three months of approach observations, apart from one outburst that occurred around April 30 and a second increase in flux after June 20. Coma was resolved in the profiles from mid-April. Analysis of the coma morphology suggests that most of the activity comes from a source towards the celestial north pole of the comet, but the outburst that occurred on April 30 released material in a different direction. (literal)
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