The origin of the rubber duck
The origin of the rubber duck
It seems that scientists have resolved to what is the curious form of the most mediatic comet of recent times. And that form that some have compared with that of a rubber duck offers Comet 67P / Churyumov-Gerasimenko a unique aspect that has given many headaches to the scientific community.
Image 1: Aspect of Comet 67P / Churyumov-Gerasimenko where the rubber duck is sensed. Credits: ESA / Rosetta / Navcam.
Thanks to the high resolution images that the Rosetta probe (ESA) used to study the layers of material seen in the nucleus, has been found with the solution that explains the curious morphology of the comet. "The images show that both lobes have an external envelope of materials organized in different layers", says Matteo Massironi, a scientist associated with the team of OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) in the University of Padua (Italy) and author of one of the articles announcing the discovery.
Two training assumptions
Massironi and his colleagues used a 3D model to determine the directions of inclination in the layers and to visualize how they extend along the subsoil. Knowing that the layers must form a right angle with respect to the direction of the force of gravity at that point, these two cases represented:
1) that the comet consists of a single body with a center of mass near the neck.
2) that the comet is composed of two separate bodies, each with its own center of mass.
One or two?
When observing the two lobes, remarkable structural similarities can be seen, which would point to a single body that, due to erosive effects, has formed a neck and with the passage of time would have given rise to the two large structures that make up the nucleus.
However, there was a key clue that unequivocally points out that the two lobes are independent when they observed that the layers were leaning in opposite directions near the comet's neck. "This suggests that the surface layers of the two lobes were formed independently before the two objects merged, and it must have been a low-speed collision because the ordering of the strata has been preserved," Massironi concludes.
Image 2: 3D view of the nucleus and strata of Comet 67P / Churyumov-Gerasimenko. On the left side there are four different 3D views of the comet nucleus with the best adjusted planes derived from the stratification. On the right side, the planes that best fit individually are shown. Each plane indicates the orientation of the strata at that specific location of the comet, which corresponds to the center of the drawn plane. You can see how the two lobes show independent envelopes. The color scale indicates the angular deviation between the vector of the plane and the local gravity vector, calculated for the whole body assuming a uniform density. Credits: doi: 10.1038 / nature15511 / M. Massironi et al.
Therefore, the famous rubber duck that some claim to appreciate in the form of the comet has been produced by the impact of two comets at low speed, merging into a single body and adopting that curious shape.
The results of this research were presented in two presentations during the EPSC (European Planetary Science Congress) that is being held in Nantes (France), as well as in the journal Science, under the title "The shape and structure of cometary nuclei as a result of low velocity accretion ", by M. Jutzi et al. and in the journal Nature, under the title "Two independent and primitive envelopes of the bilobate nucleus of comet 67P", by M. Massironi et al.
The team that has carried out the research published in the journal Science is formed by M. Jutzi (Center for Space and Habitability / University of Bern, Switzerland) and E. Asphaug (School of Earth and Space Exploration / Arizona State University, United States) , while the one published in the journal Nature is formed by M. Massironi (Dipartimento di Geoscienze / University of Padova, Italy; CISAS / University of Padova, Italy), E. Simioni (CNR-IFN UOS Padova LUXOR, Italy), F Marzari (University of Padova / Department of Physics and Astronomy, Italy), G. Cremonese (INAF / Osservatorio Astronomico di Padova, Italy), L. Giacomini (Dipartimento di Geoscienze / University of Padova, Italy), M. Pajola (CISAS / University of Padova, Italy), L. Jorda (Aix Marseille Université / CNRS / LAM, France), G. Naletto (CISAS / University of Padova, Italy, CNR-IFN UOS Padova LUXOR, Italy, Department of Information Engineering / University of Padova, Italy), S. Lowry (The University of Kent / School of Physics al Sciences, United Kingdom), M.R. El-Maarry (Physikalisches Institut der Universität Bern, Switzerland), F. Preusker (DLR / Institut für Planetenforschung, Germany), F. Scholten (DLR / Institut für Planetenforschung, Germany), H. Sierks (Max-Planck-Institut für Sonnensystemforschung , Germany), C. Barbieri (University of Padova / Department of Physics and Astronomy, Italy), P. Lamy (Aix Marseille Université / CNRS / LAM, France), R. Rodrigo (Center for Astrobiology / CSIC-INTA, Spain; International Space Science Institute, Switzerland), D. Koschny (Scientific Support Office / European Space Research and Technology Center / ESA, The Netherlands), H. Rickman (Department of Physics and Astronomy / Uppsala University, Sweden, PAS Space Research Center, Poland ), HU Keller (IGEP / Technische Universität Braunschweig, Germany), M.F. A'Hearn (University of Maryland / Department of Astronomy, United States, Akademie der Wissenschaften zu Göttingen and Max-Planck-Institut für Sonnensystemforschung, Germany), J. Agarwal (Max-Planck-Institut für Sonnensystemforschung, Germany), A.T. Auger (Aix Marseille Université / CNRS / LAM, France), M.A. Barucci (LESIA-Observatoire de Paris / CNRS / Université Pierre et Marie Curie, France), J.L. Bertaux (LATMOS / CNRS / UVSQ / IPSL, France), I. Bertini (CISAS / University of Padova, Italy), S. Besse (Scientific Support Office / European Space Research and Technology Center / ESA, The Netherlands), D. Bodewits (University of Maryland / Department of Astronomy, United States), C. Capanna (Aix Marseille University / CNRS / LAM, France), V. da Deppo (CNR-IFN UOS Padova LUXOR, Italy), B. Davidsson (Department of Physics and Astronomy / Uppsala University, Sweden), S. Debei (Department of Industrial Engineering / University of Padova, Italy), M. de Cecco (University of Trento, Italy), F. Ferri (CISAS / University of Padova, Italy), S. Fornasier (LESIA-Observatoire de Paris / CNRS / Université Pierre et Marie Curie, France), M. Fulle (INAF / Osservatorio Astronomico, Italy), R. Gaskell (Planetary Science Institute, United States), O. Groussin (Aix) Marseille University / CNRS / LAM, France), PJ Gutiérrez (Institute of Astrophysics of Andalucia / CSIC, Spain), C. Güttler (Max-Planck-Institut für Sonnensystemforschung, Germany), S.F. Hviid (DLR / Institut für Planetenforschung, Germany, Max-Planck-Institut für Sonnensystemforschung, Germany), W.H. Ip (National Central University / Graduate Institute of Astronomy, Taiwan), J. Knollenberg (DLR / Institut für Planetenforschung, Germany), G. Kovacs (Max-Planck-Institut für Sonnensystemforschung, Germany), R. Kramm (Max-Planck- Institut für Sonnensystemforschung, Germany), E. Kührt (DLR / Institut für Planetenforschung, Germany), M. Küppers (Operations Department / European Space Astronomy Center / ESA, Spain), F. la Forgia (University of Padova / Department of Physics and Astronomy, Italy), LM Lara (Institute of Astrophysics of Andalucia / CSIC, Spain), M. Lazzarin (University of Padova / Department of Physics and Astronomy, Italy), Z.Y. Lin (National Central University / Graduate Institute of Astronomy, Taiwan), J.J. Lopez Moreno (Institute of Astrophysics of Andalucia / CSIC, Spain), S. Magrin (University of Padova / Department of Physics and Astronomy, Italy), H. Michalik (Institut für Datentechnik und Kommunikationsnetze der TU Braunschweig, Germany), S. Mottola (DLR / Institut für Planetenforschung, Germany), N. Oklay (Max-Planck-Institut für Sonnensystemforschung, Germany), A. Pommerol (Physikalisches Institut der Universität Bern, Switzerland), N. Thomas (Physikalisches Institut der Universität Bern, Switzerland) , C. Tubiana (Max-Planck-Institut für Sonnensystemforschung, Germany) and JB Vincent (Max-Planck-Institut für Sonnensystemforschung, Germany).
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