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8 results on '"MIGLIORINI, Alessandra"'

1. The Comet Interceptor Mission

Author

Jones, Geraint H., Snodgrass, Colin, Tubiana, Cecilia, Küppers, Michael, Kawakita, Hideyo, Lara, Luisa M., Agarwal, Jessica, André, Nicolas, Attree, Nicholas, Auster, Uli, Bagnulo, Stefano, Bannister, Michele, Beth, Arnaud, Bowles, Neil, Coates, Andrew, Colangeli, Luigi, Corral van Damme, Carlos, Da Deppo, Vania, De Keyser, Johan, Della Corte, Vincenzo, Edberg, Niklas, El-Maarry, Mohamed Ramy, Faggi, Sara, Fulle, Marco, Funase, Ryu, Galand, Marina, Goetz, Charlotte, Groussin, Olivier, Guilbert-Lepoutre, Aurélie, Henri, Pierre, Kasahara, Satoshi, Kereszturi, Akos, Kidger, Mark, Knight, Matthew, Kokotanekova, Rosita, Kolmasova, Ivana, Kossacki, Konrad, Kührt, Ekkehard, Kwon, Yuna, La Forgia, Fiorangela, Levasseur-Regourd, Anny-Chantal, Lippi, Manuela, Longobardo, Andrea, Marschall, Raphael, Morawski, Marek, Muñoz, Olga, Näsilä, Antti, Nilsson, Hans, Opitom, Cyrielle, Pajusalu, Mihkel, Pommerol, Antoine, Prech, Lubomir, Rando, Nicola, Ratti, Francesco, Rothkaehl, Hanna, Rotundi, Alessandra, Rubin, Martin, Sakatani, Naoya, Sánchez, Joan Pau, Simon Wedlund, Cyril, Stankov, Anamarija, Thomas, Nicolas, Toth, Imre, Villanueva, Geronimo, Vincent, Jean-Baptiste, Volwerk, Martin, Wurz, Peter, Wielders, Arno, Yoshioka, Kazuo, Aleksiejuk, Konrad, Alvarez, Fernando, Amoros, Carine, Aslam, Shahid, Atamaniuk, Barbara, Baran, Jędrzej, Barciński, Tomasz, Beck, Thomas, Behnke, Thomas, Berglund, Martin, Bertini, Ivano, Bieda, Marcin, Binczyk, Piotr, Busch, Martin-Diego, Cacovean, Andrei, Capria, Maria Teresa, Carr, Chris, Castro Marín, José María, Ceriotti, Matteo, Chioetto, Paolo, Chuchra-Konrad, Agata, Cocola, Lorenzo, Colin, Fabrice, Crews, Chiaki, Cripps, Victoria, Cupido, Emanuele, Dassatti, Alberto, Davidsson, Björn J. R., De Roche, Thierry, Deca, Jan, Del Togno, Simone, Dhooghe, Frederik, Donaldson Hanna, Kerri, Eriksson, Anders, Fedorov, Andrey, Fernández-Valenzuela, Estela, Ferretti, Stefano, Floriot, Johan, Frassetto, Fabio, Fredriksson, Jesper, Garnier, Philippe, Gaweł, Dorota, Génot, Vincent, Gerber, Thomas, Glassmeier, Karl-Heinz, Granvik, Mikael, Grison, Benjamin, Gunell, Herbert, Hachemi, Tedjani, Hagen, Christian, Hajra, Rajkumar, Harada, Yuki, Hasiba, Johann, Haslebacher, Nico, Herranz De La Revilla, Miguel Luis, Hestroffer, Daniel, Hewagama, Tilak, Holt, Carrie, Hviid, Stubbe, Iakubivskyi, Iaroslav, Inno, Laura, Irwin, Patrick, Ivanovski, Stavro, Jansky, Jiri, Jernej, Irmgard, Jeszenszky, Harald, Jimenéz, Jaime, Jorda, Laurent, Kama, Mihkel, Kameda, Shingo, Kelley, Michael S. P., Klepacki, Kamil, Kohout, Tomáš, Kojima, Hirotsugu, Kowalski, Tomasz, Kuwabara, Masaki, Ladno, Michal, Laky, Gunter, Lammer, Helmut, Lan, Radek, Lavraud, Benoit, Lazzarin, Monica, Le Duff, Olivier, Lee, Qiu-Mei, Lesniak, Cezary, Lewis, Zoe, Lin, Zhong-Yi, Lister, Tim, Lowry, Stephen, Magnes, Werner, Markkanen, Johannes, Martinez Navajas, Ignacio, Martins, Zita, Matsuoka, Ayako, Matyjasiak, Barbara, Mazelle, Christian, Mazzotta Epifani, Elena, Meier, Mirko, Michaelis, Harald, Micheli, Marco, Migliorini, Alessandra, Millet, Aude-Lyse, Moreno, Fernando, Mottola, Stefano, Moutounaick, Bruno, Muinonen, Karri, Müller, Daniel R., Murakami, Go, Murata, Naofumi, Myszka, Kamil, Nakajima, Shintaro, Nemeth, Zoltan, Nikolajev, Artiom, Nordera, Simone, Ohlsson, Dan, Olesk, Aire, Ottacher, Harald, Ozaki, Naoya, Oziol, Christophe, Patel, Manish, Savio Paul, Aditya, Penttilä, Antti, Pernechele, Claudio, Peterson, Joakim, Petraglio, Enrico, Piccirillo, Alice Maria, Plaschke, Ferdinand, Polak, Szymon, Postberg, Frank, Proosa, Herman, Protopapa, Silvia, Puccio, Walter, Ranvier, Sylvain, Raymond, Sean, Richter, Ingo, Rieder, Martin, Rigamonti, Roberto, Ruiz Rodriguez, Irene, Santolik, Ondrej, Sasaki, Takahiro, Schrödter, Rolf, Shirley, Katherine, Slavinskis, Andris, Sodor, Balint, Soucek, Jan, Stephenson, Peter, Stöckli, Linus, Szewczyk, Paweł, Troznai, Gabor, Uhlir, Ludek, Usami, Naoto, Valavanoglou, Aris, Vaverka, Jakub, Wang, Wei, Wang, Xiao-Dong, Wattieaux, Gaëtan, Wieser, Martin, Wolf, Sebastian, Yano, Hajime, Yoshikawa, Ichiro, Zakharov, Vladimir, Zawistowski, Tomasz, Zuppella, Paola, Rinaldi, Giovanna, and Ji, Hantao

Published
2024
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2. The CUBES science case

Author

Evans, Chris, Cristiani, Stefano, Opitom, Cyrielle, Cescutti, Gabriele, D’Odorico, Valentina, Alcalá, Juan Manuel, Alencar, Silvia H. P., Balashev, Sergei, Barbuy, Beatriz, Bastian, Nate, Battino, Umberto, Cambianica, Pamela, Carini, Roberta, Carter, Brad, Cassisi, Santi, Vaz Castilho, Bruno, Christlieb, Norbert, Cooke, Ryan, Covino, Stefano, Cremonese, Gabriele, Cunha, Katia, da Silva, André R., D’Elia, Valerio, De Cia, Annalisa, De Silva, Gayandhi, Diaz, Marcos, Di Marcantonio, Paolo, Ernandes, Heitor, Fitzsimmons, Alan, Franchini, Mariagrazia, Gänsicke, Boris T., Genoni, Matteo, Giribaldi, Riano E., Grazian, Andrea, Hansen, Camilla Juul, La Forgia, Fiorangela, Lazzarin, Monica, Marcolino, Wagner, Marconi, Marcella, Migliorini, Alessandra, Noterdaeme, Pasquier, Pereira, Claudio, Pilecki, Bogumil, Quirrenbach, Andreas, Randich, Sofia, Rossi, Silvia, Smiljanic, Rodolfo, Snodgrass, Colin, Stürmer, Julian, Trost, Andrea, Vanzella, Eros, Ventura, Paolo, Wright, Duncan, and Zafar, Tayyaba

Published
2023
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3. Cometary science with CUBES

Author

Opitom, Cyrielle, Snodgrass, Colin, Forgia, Fiorangela La, Evans, Chris, Cambianica, Pamela, Cremonese, Gabriele, Fitzsimmons, Alan, Lazzarin, Monica, and Migliorini, Alessandra

Published
2023
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5. Water and Carbon Dioxide Ices-Rich Areas on Comet 67P/CG Nucleus Surface

Author

Filacchione, Gianrico, Capaccioni, Fabrizio, Raponi, Andrea, de Sanctis, Maria Cristina, Ciarniello, Mauro, Barucci, Maria Antonella, Tosi, Federico, Migliorini, Alessandra, Capria, Maria Teresa, Erard, Stéphane, Bockelée-Morvan, Dominique, Leyrat, Cédric, Arnold, Gabriele, Kappel, David, Mccord, Thomas B., ITA, USA, FRA, DEU, Istituto di Astrofisica e Planetologia Spaziali, INAF (IAPS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Bear Fight Institute, and Henry, Florence

Subjects
Asteroiden und Kometen, 67P, Leitungsbereich PF, Rosetta, comets, VIRTIS, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], water ice, carbon dioxide ice
Abstract

International audience; So far, only two ice species have been identified by Rosetta/VIRTIS-M [1] on the surface of 67P/Churyumov-Gerasimenko during the pre-perihelion time: crystalline water and carbon dioxide ice. Water ice has been spectroscopically identified in three distinct modalities: 1) On the active areas of Hapi region where water ice changes its abundance with local time and illumination conditions, condensing during the night hours and sublimating during daytime [2]; 2) On recent debris fields collapsed from two elevated structures in the Imhotep region where more fresh and pristine material is exposed [3]; 3) On eight bright areas located in Khonsu, Imhotep, Anhur, Atum and Khepry regions [4] where single or multiple grouped icy patches with sizes ranging between few meters to about 60 m are observed. Carbon dioxide ice has been detected only in a 60-80 m area in Anhur region while it was exiting from a four year-long winter-night season [5]. This ice deposit underwent a rapid sublimation, disappearing in about one month after its initial detection. While water and carbon dioxide ice appear always mixed with the ubiquitous dark material [6,7], there are no evidences of the presence of water and carbon dioxide ices mixed together in the same area. If observed, ices always account for very small fraction (few percent) with respect to the dark material. Moreover, the surface ice deposits are preferentially located on the large lobe and the neck while they are absent on the small lobe. Apart from these differences in the spatial distribution of ices on the surface, a large variability is observed the mixing modalities and in the grain size distributions, as retrieved from spectral modeling [8]: 1) very small Îm-sized water ice grains in intimate mixing with the dark terrain are detected on Hapi active regions [2]; 2) two monodispersed distributions with maxima at 56 Îm and at 2 mm, corresponding to the intimate and areal mixing classes, are observedon the Imhotep debris fields ice grains [3]; 3) different combinations of water ice and dark terrain in intimate mixing with small grains (tens of microns) or in areal mixing with large grains (mm- sized) are seen on the eight bright areas discussed in [4]; 4) the CO2 ice in the Anhur region appears grouped in areal patches made of 50 mum sized grains [5]. While the spectroscopic identification of water and carbon dioxide ices is made by means of diagnostic infrared absorption features, their presence cause significant effects also at visible wavelengths, including the increase of the albedo and the reduction of the spectral slope which results in a more blue color [9,10]. In summary, thermodynamic conditions prevailing on the 67P/CG nucleus surface allow the presence of only H2O and CO2 ices. Similar properties are probably common among other Jupiter family comets.

Published
2017

6. VIRTIS observations of the nucleus of 67P/Churyumov=Gerasimenko at low phase angle

Author

Ciarniello, Mauro, Filacchione, Gianrico, Capaccioni, Fabrizio, Raponi, Andrea, de Sanctis, Maria Cristina, Tosi, Federico, Piccioni, Giuseppe, Migliorini, Alessandra, Cerroni, Priscilla, Capria, Maria Teresa, Erard, Stéphane, Bockelée-Morvan, Dominique, Leyrat, Cédric, Arnold, Gabriele, Barucci, Maria Antonella, Schmitt, Bernard, Quirico, Éric, Taylor, Frederic W., Kappel, David, Longobardo, Andrea, Henry, Florence, ITA, GBR, FRA, DEU, Istituto di Astrofisica e Planetologia Spaziali, INAF (IAPS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR) Berlin, Germany, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Oxford University

Subjects
67P, Rosetta, spectrophotometry, comets, VIRTIS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; On 9-10 of April 2016, the Rosetta orbiter completed a close flyby around the nucleus of 67P/Churyumov-Gerasimenko, when the comet was at heliocentric distance of 2.76 AU, along the outbound leg of its orbit around the Sun. This allowed the VIRTIS-M imaging spectrometer to observe the surface of 67P at visible wavelengths (0.2-1 mum) in the 0.93°-89.7° phase angle range with a spatial resolution ranging from 7 to 46 m/pix, resulting in a total of 105 hyperspectral images. Previous observations of the comet at low phase angle were acquired by VIRTIS-M during the approach phase on July 2014 (3.7 AU), with pixel resolution varying from 450 to 3200 m/pix, preventing disk-resolved imaging. The April 2016 observations fill this gap, allowing us to constrain the spectrophotometric properties of the surface at higher spatial resolution in the opposition surge geometry, therefore investigating both the 'shadow hiding' and 'coherent backscattering' opposition effect. Extrapolation to 0° phase angle of the reflectance measured during the flyby at latitude between -10° and 30° indicates a surface normal albedo of 0.06 at 0.55 mum. This result is close to the previous average value derived by Ciarniello et al. (2015) from a full-disk analysis giving 0.062 /-0.002 (3.7 AU, inbound orbit). Subsequent measurements by Filacchione et al. (2016) and Ciarniello et al. (submitted), derived from pre-perihelion observations at lower heliocentric distances, revealed a progressive enrichment of water ice abundance on the nucleus, in northern hemisphere regions, with a consequent brightening of the surface. The measured normal albedo derived from the 9-10 April 2016 dataset seems to indicate that during the post-perihelion phase the northern hemisphere has returned to albedo values compatible to the ones measured during the inbound part of the orbit, when the comet was at 3.7 AU from the Sun. This could be an indication that the northern hemisphere has been either covered by dust emitted by the southern hemisphere during the very active perihelion phase, or that dehydration of the upper surface layers has taken place.

Published
2016

7. The SSDC contribution to the improvement of knowledge by means of 3D data projections of minor bodies.

Author

Zinzi, Angelo, Ciarniello, Mauro, Della Corte, Vincenzo, Ivanovski, Stavro, Longobardo, Andrea, Migliorini, Alessandra, Capria, Maria Teresa, Palomba, Ernesto, and Rotundi, Alessandra

Subjects
*PLANETARY exploration, *SPACE sciences, *SPACE exploration, *SOLAR system
Abstract

Abstract The latest developments of planetary exploration missions devoted to minor bodies required new solutions to correctly visualize and analyze data acquired over irregularly shaped bodies. ASI Space Science Data Center (SSDC – ASI, formerly ASDC – ASI Science Data Center) worked on this task since early 2013, when started developing the web tool MATISSE (Multi-purpose Advanced Tool for the Instruments of the Solar System Exploration) mainly focused on the Rosetta/ESA space mission data. In order to visualize very high-resolution shape models, MATISSE uses a Python module (vtpMaker), which can also be launched as a stand-alone command-line software. MATISSE and vtpMaker are part of the SSDC contribution to the new challenges imposed by the "orbital exploration" of minor bodies: (1) MATISSE allows to search for specific observations inside datasets and then analyze them in parallel, providing high-level outputs; (2) the 3D capabilities of both tools are critical in inferring information otherwise difficult to retrieve for non-spherical targets and, as in the case for the GIADA instrument onboard Rosetta, to visualize data related to the coma. New tasks and features adding valuable capabilities to the minor bodies SSDC tools are planned for the near future thanks to new collaborations. [ABSTRACT FROM AUTHOR]

Published
2018
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8. Investigation into the disparate origin of CO2 and H2O outgassing for Comet 67/P.

Author

Fink, Uwe, Doose, Lyn, Rinaldi, Giovanna, Bieler, André, Capaccioni, Fabrizio, Bockelée-Morvan, Dominique, Filacchione, Gianrico, Erard, Stephane, Leyrat, Cedric, Blecka, Maria, Capria, Maria Teresa, Combi, Michael, Crovisier, Jacques, De Sanctis, Maria Cristina, Fougere, Nicolas, Taylor, Fred, Migliorini, Alessandra, and Piccioni, Giuseppe

Subjects
*CARBON dioxide, *SPECTROMETERS, *OUTGASSING, *VAPOR pressure, *CHURYUMOV-Gerasimenko comet
Abstract

We present an investigation of the emission intensity of CO 2 and H 2 O and their distribution in the coma of 67P/ Churyumov–Gerasimenko obtained by the VIRTIS-M imaging spectrometer on the Rosetta mission. We analyze 4 data cubes from Feb. 28, and 7 data cubes from April 27, 2015. For both data sets the spacecraft was at a sufficiently large distance from the comet to allow images of the whole nucleus and the surrounding coma. We find that unlike water which has a reasonably predictable behavior and correlates well with the solar illumination, CO 2 outgasses mostly in local regions or spots. Furthermore for the data on April 27, the CO 2 evolves almost exclusively from the southern hemisphere, a region of the comet that has not received solar illumination since the comet's last perihelion passage. Because CO 2 and H 2 O have such disparate origins, deriving mixing ratios from local column density measurements cannot provide a meaningful measurement of the CO 2 /H 2 O ratio in the coma of the comet. We obtain total production rates of H 2 O and CO 2 by integrating the band intensity in an annulus surrounding the nucleus and obtain pro-forma production rate CO 2 /H 2 O mixing ratios of ∼5.0% and ∼2.5% for Feb. 28 and April 27, respectively. Because of the highly variable nature of the CO 2 evolution from the surface we do not believe that these numbers are diagnostic of the comet's bulk CO 2 /H 2 O composition. We believe that our investigation provides an explanation for the large observed variations reported in the literature for the CO 2 /H 2 O production rate ratios. Our mixing ratio maps indicate that, besides the difference in vapor pressure of the two gases, this ratio depends on the comet's rotational orientation combined with its complex geometric shape which can result in quite variable rates of erosion for different surface areas such as the northern and southern hemisphere. Our annulus measurement for the total water production for Feb. 28 at 2.21AU from the Sun is 2.5 × 10 26 molecules/s while for April 27 at 1.76 AU it is 4.65 × 10 26 . We find that about 83% of the H 2 O resides in the illuminated portion of our annulus and about 17% on the night side. We also make an attempt to obtain the fraction of the H 2 O production coming from the highly active neck of the comet versus the rest of the illuminated surface from the pole-on view of Feb. 28 and estimate that about 60% of the H 2 O derives from the neck area. A rough estimate of the water surface evaporation rate of the illuminated nucleus for April 27 yields about 5 × 10 19 molecules/s/m 2 . Spatial radial profiles of H 2 O on April 27 on the illuminated side of the comet, extending from 1.78 to 6.47 km from the nucleus center, show that water follows model predictions quite well, with the gas accelerating as it expands into the coma. Our dayside radial profile allows us to make an empirical determination of the expansion velocity of water. On the night side the spatial profile of water follows 1/ ρ . The CO 2 profiles do not exhibit any acceleration into the coma but are closely matched by a 1/ ρ profile. [ABSTRACT FROM AUTHOR]

Published
2016
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