Academic Journal
GRAVITY chromatic imaging of η Car’s core. Milliarcsecond resolution imaging of the wind-wind collision zone (Brγ, He I) ; Imagerie spectro-interférométrique du noyau de η Car avec l'instrument GRAVITY : images de la zone de collision de vent dans les raies Br γ et He I avec une résolution de la milli-seconde d'arc
| العنوان: | GRAVITY chromatic imaging of η Car’s core. Milliarcsecond resolution imaging of the wind-wind collision zone (Brγ, He I) ; Imagerie spectro-interférométrique du noyau de η Car avec l'instrument GRAVITY : images de la zone de collision de vent dans les raies Br γ et He I avec une résolution de la milli-seconde d'arc |
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| المؤلفون: | Sanchez-Bermudez, Joel, Weigelt, Gerd, Bestenlehner, Joachim M., Kervella, Pierre, Brandner, Wolfgang, Henning, Thomas, Müller, André, Perrin, Guy, Pott, Jorg-Uwe, Schöller, Markus, van Boekel, Roy, Abuter, Roberto, Accardo, Matteo, Amorim, Antonio, Anugu, Narsireddy, Avila, Gerardo, Benisty, Myriam, Berger, Jean-Philippe, Blind, Nicolas, Bonnet, Henri, Bourget, Pierre, Brast, Roland, Buron, Alexander, Cantalloube, Faustine, Caratti O Garatti, Alessio, Cassaing, Frederic, Chapron, Frédéric, Choquet, Élodie, Clenet, Yann, Collin, Claude, Coude Du Foresto, Vincent, de Wit, Willem-Jan, de Zeeuw, Tim, Deen, Casey, Delplancke-Ströbele, Françoise, Dembet, Roderick, Derie, Frédéric, Dexter, Jason, Duvert, Gilles, Ebert, Monica, Eckart, Andreas, Eisenhauer, Frank, Esselborn, Michael, Fédou, Pierre, Garcia, Paulo J. V., Garcia-Dabo, Cesar Enrique, Garcia Lopez, Rebeca, Gao, Feng, Gendron, Eric, Genzel, Reinhard, Gillessen, Stefan, Haubois, Xavier, Haug, Marcus, Haussmann, Frank, Hippler, Stefan, Horrobin, Matthew, Huber, Armin, Huber, Zoltan, Hubin, Norbert, Hummel, Christian A., Jakob, Gerd, Jochum, Lieselotte, Jocou, Laurent, Karl, Martina, Kaufer, Andreas, Kellner, Stefan, Kendrew, Sarah, Kern, Lothar, Kiekebusch, Mario, Klein, Ralf, Kolb, Johann, Kulas, Martin, Lacour, Sylvestre, Lapeyrère, Vincent, Lazareff, Bernard, Le Bouquin, Jean-Baptiste, Léna, Pierre, Lenzen, Rainer, Lévêque, Samuel, Lippa, Magdalena, Magnard, Yves, Mehrgan, Leander, Mellein, Marcus, Mérand, Antoine, Moreno-Ventas, Javier, Moulin, Thibaut, Muller, Ewald, Muller, Friedrich, Neumann, Udo, Oberti, Sylvain, Ott, Thomas, Pallanca, Laurent, Panduro, Johana, Pasquini, Luca, Paumard, Thibaut, Percheron, Isabelle, Perraut, Karine, Petrucci, Pierre-Olivier, Pflüger, Andreas, Pfuhl, Oliver, Duc, Thanh Phan, Plewa, Philipp M., Popovic, Dan, Rabien, Sebastian, Ramirez, Andres, Ramos, Jose Ricardo, Rau, Christian, Riquelme, Miguel, Rodríguez-Coira, Gustavo, Rohloff, Ralf-Rainer, Rosales, Alejandra, Rousset, Gérard, Scheithauer, Silvia, Schuhler, Nicolas, Spyromilio, Jason, Straub, Odele, Straubmeier, Christian, Sturm, Eckhard, Suarez, Marco, Tristram, Konrad R. W., Ventura, Noel, Vincent, Frédéric, Waisberg, Idel, Wank, Imke, Widmann, Felix, Wieprecht, Ekkehard, Wiest, Michael, Wiezorrek, Erich, Wittkowski, Markus, Woillez, Julien, Wolff, Burkhard, Yazici, Senol, Ziegler, Denis, Zins, Gerard |
| المساهمون: | Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, European Southern Observatory Santiago (ESO), European Southern Observatory (ESO), Max-Planck-Institut für Radioastronomie (MPIFR), University of Sheffield Sheffield, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Santiago de Chile Santiago (USACH), Centro de Astrofísica e Gravitação Instituto Superior Técnico, Lisboa = Center for Astrophysics and Gravitation Lisbon (CENTRA), Instituto Superior Técnico (IST / Técnico Lisboa)-Universidade de Lisboa = University of Lisbon = Université de Lisbonne (ULISBOA), Universidade de Lisboa = University of Lisbon = Université de Lisbonne (ULISBOA), University of Exeter, 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 ), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Max Planck Institute for Extraterrestrial Physics (MPE), Dublin Institute for Advanced Studies (DIAS), DOTA, ONERA, Université Paris Saclay (COmUE) Châtillon, ONERA-Université Paris Saclay (COmUE), Universiteit Leiden = Leiden University, Physikalisches Institut Köln, Universität zu Köln = University of Cologne, Max Planck Institute for Radio Astronomy, Universidade do Porto = University of Porto, Instituto Superior Técnico, Technical University of Lisbon, Lawrence Berkeley National Laboratory Berkeley (LBNL), Space Telescope Science Institute (STSci), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté COMUE (UBFC)-Université Bourgogne Franche-Comté COMUE (UBFC) |
| المصدر: | ISSN: 0004-6361. |
| بيانات النشر: | HAL CCSD EDP Sciences |
| سنة النشر: | 2018 |
| المجموعة: | Université Savoie Mont Blanc: HAL |
| مصطلحات موضوعية: | MASS LOSS, INTERFEROMETER, MASSIVE STAR, BINARY STAR, HIGH ANGULAR RESOLUTION, STAR IMAGING, IMAGERIE STELLAIRE, ETOILES BINAIRES, ETOILES MASSIVES, INSTRUMENTATION: HAUTE RESOLUTION ANGULAIRE, ETOILE: PERTE DE MASSE, INSTRUMENTATION: INTERFEROMETRES, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic |
| الوصف: | International audience ; Context. η Car is one of the most intriguing luminous blue variables in the Galaxy. Observations and models of the X-ray, ultraviolet, optical, and infrared emission suggest a central binary in a highly eccentric orbit with a 5.54 yr period residing in its core. 2D and 3D radiative transfer and hydrodynamic simulations predict a primary with a dense and slow stellar wind that interacts with the faster and lower density wind of the secondary. The wind-wind collision scenario suggests that the secondary’s wind penetrates the primary’s wind creating a low-density cavity in it, with dense walls where the two winds interact. However, the morphology of the cavity and its physical properties are not yet fully constrained.Aims. We aim to trace the inner ∼5–50 au structure of η Car’s wind-wind interaction, as seen through Brγ and, for the first time, through the He I 2s-2p line.Methods. We have used spectro-interferometric observations with the K-band beam-combiner GRAVITY at the VLTI. The analyses of the data include (i) parametrical model-fitting to the interferometric observables, (ii) a CMFGEN model of the source’s spectrum, and (iii) interferometric image reconstruction.Results. Our geometrical modeling of the continuum data allows us to estimate its FWHM angular size close to 2 mas and an elongation ratio ϵ = 1.06 ± 0.05 over a PA = 130° ± 20°. Our CMFGEN modeling of the spectrum helped us to confirm that the role of the secondary should be taken into account to properly reproduce the observed Brγ and He I lines. Chromatic images across the Brγ line reveal a southeast arc-like feature, possibly associated to the hot post-shocked winds flowing along the cavity wall. The images of the He I 2s-2p line served to constrain the 20 mas (∼50 au) structure of the line-emitting region. The observed morphology of He I suggests that the secondary is responsible for the ionized material that produces the line profile. Both the Brγ and the He I 2s-2p maps are consistent with previous hydrodynamical ... |
| نوع الوثيقة: | article in journal/newspaper |
| اللغة: | English |
| Relation: | info:eu-repo/semantics/altIdentifier/arxiv/1808.02141; ARXIV: 1808.02141; BIBCODE: 2018A&A.618A.125G |
| DOI: | 10.1051/0004-6361/201832977 |
| الاتاحة: | https://hal.science/hal-02055583 https://hal.science/hal-02055583v1/document https://hal.science/hal-02055583v1/file/DOTA18263.1544447453_postprint.pdf https://doi.org/10.1051/0004-6361/201832977 |
| Rights: | info:eu-repo/semantics/OpenAccess |
| رقم الانضمام: | edsbas.C7E68C6B |
| قاعدة البيانات: | BASE |
| DOI: | 10.1051/0004-6361/201832977 |
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