The Asymmetric Inner Disk of the Herbig Ae Star HD 163296 in the Eyes of VLTI/MATISSE: Evidence for a Vortex?
Context.A complex environment exists in the inner few astronomical units of planet-forming disks. High-angular-resolution observa-tions play a key role in our understanding of the disk structure and the dynamical processes at work.Aims.In this study we aim to characterize the mid-infrared brightness...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2021-03, Vol.647, p.A56 |
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| creator | Varga, J Hogerheijde, M Boekel, R van Klarmann, L Petrov, R Waters, L B F M Lagarde, S Berio, Ph Weigelt, G Robbe-Dubois, S Lopez, B Millour, F Augereau, J-C Meheut, H Meilland, A Henning, Th Jaffe, W Bettonvil, F Bristow, P Hofmann, K-H Matter, A Allouche, F Donnan, F Heininger, M Cruzalebes, P Glindermann, A Meisenheimer, K Paladini, C Scholler, M Woillez, J Venema, L Kokoulina, E Yoffe, G Abadie, S Abuter, R Accardo, M Adler, T Antonelli, P Bohm, A Bailet, C Bazin, G Beltran, J Boland, W Bourget, P Brast, R Bresson, Y Chelli, A Cid, C Clausse, J-M Conzelmann, R D Danchi, W-C Hann, M De Delbo, M Ebert, M Fantei, Y Gallenne, A Garces, E Herrera, J C Gonzalez Guitton, F Hron, J Hubin, N Huerta, R Ives, D Jakob, G Jasko, A Jochum, L Kragt, J Kroes, G Kuindersma, S Laun, W Leinert, C Lizon, J-L Lopez, M Merand, A Mauclert, N Maurer, T Meisner, J Meixner, K Mohr, L Morel, S Mosoni, L Navarro, R Pallanca, L Pasquini, L Percheron, I Ridinger, A Rigal, F Riquelme, M Rivinius, Th Roelfsema, R Schuhler, N Schuil, M Stee, P Stephan, C Horst, R ter Tromp, N Vakili, F Duin, A van Wittkowski, M Wrhel, F |
| description | Context.A complex environment exists in the inner few astronomical units of planet-forming disks. High-angular-resolution observa-tions play a key role in our understanding of the disk structure and the dynamical processes at work.Aims.In this study we aim to characterize the mid-infrared brightness distribution of the inner disk of the young intermediate-massstar HD 163296 from early VLTI/MATISSE observations taken in theL- andN-bands. We put special emphasis on the detection ofpotential disk asymmetries.Methods.We use simple geometric models to fit the interferometric visibilities and closure phases. Our models include a smoothedring, a flat disk with an inner cavity, and a 2D Gaussian. The models can account for disk inclination and for azimuthal asymmetriesas well. We also perform numerical hydrodynamical simulations of the inner edge of the disk.Results.Our modeling reveals a significant brightness asymmetry in theL-band disk emission. The brightness maximum of the asym-metry is located at the NW part of the disk image, nearly at the position angle of the semimajor axis. The surface brightness ratio inthe azimuthal variation is3.5±0.2. Comparing our result on the location of the asymmetry with other interferometric measurements,we confirm that the morphology of ther |
| doi_str_mv | 10.1051/0004-6361/202039400 |
| format | Article |
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High-angular-resolution observa-tions play a key role in our understanding of the disk structure and the dynamical processes at work.Aims.In this study we aim to characterize the mid-infrared brightness distribution of the inner disk of the young intermediate-massstar HD 163296 from early VLTI/MATISSE observations taken in theL- andN-bands. We put special emphasis on the detection ofpotential disk asymmetries.Methods.We use simple geometric models to fit the interferometric visibilities and closure phases. Our models include a smoothedring, a flat disk with an inner cavity, and a 2D Gaussian. The models can account for disk inclination and for azimuthal asymmetriesas well. We also perform numerical hydrodynamical simulations of the inner edge of the disk.Results.Our modeling reveals a significant brightness asymmetry in theL-band disk emission. The brightness maximum of the asym-metry is located at the NW part of the disk image, nearly at the position angle of the semimajor axis. The surface brightness ratio inthe azimuthal variation is3.5±0.2. Comparing our result on the location of the asymmetry with other interferometric measurements,we confirm that the morphology of ther<0.3au disk region is time-variable. We propose that this asymmetric structure, located in ornear the inner rim of the dusty disk, orbits the star. To find the physical origin of the asymmetry, we tested a hypothesis where a vortexis created by Rossby wave instability, and we find that a unique large-scale vortex may be compatible with our data. The half-lightradius of theL-band-emitting region is0.33±0.01au, the inclination is52◦+5◦−7◦, and the position angle is143◦±3◦. Our models predictthat a non-negligible fraction of theL-band disk emission originates inside the dust sublimation radius forμm-sized grains. Refractorygrains or large (&10μm-sized) grains could be the origin of this emission.N-band observations may also support a lack of smallsilicate grains in the innermost disk (r.0.6au), in agreement with our findings fromL-band data.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/202039400</identifier><language>eng</language><publisher>Goddard Space Flight Center: EDP Sciences</publisher><subject>Accretion disks ; Astronomy ; Asymmetric structures ; Asymmetry ; Brightness distribution ; Celestial bodies ; Emission ; Inclination ; Interferometry ; Mathematical analysis ; Planet formation ; Planetary waves ; Sciences of the Universe ; Sublimation ; Surface brightness ; Two dimensional models ; Vortices</subject><ispartof>Astronomy and astrophysics (Berlin), 2021-03, Vol.647, p.A56</ispartof><rights>Copyright Determination: MAY_INCLUDE_COPYRIGHT_MATERIAL</rights><rights>Copyright EDP Sciences Mar 2021</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c443t-3025ccd556e5f230159275e8013b10a3dc923be8426e196b2b930f326a4519e73</citedby><cites>FETCH-LOGICAL-c443t-3025ccd556e5f230159275e8013b10a3dc923be8426e196b2b930f326a4519e73</cites><orcidid>0000-0002-2725-6415 ; 0000-0003-4989-575X ; 0000-0002-9765-7783 ; 0000-0001-6015-646X ; 0000-0002-2958-4738 ; 0000-0001-8220-0636 ; 0000-0001-8400-687X ; 0000-0001-7517-8274 ; 0000-0001-9332-3308 ; 0000-0002-3393-2459 ; 0000-0001-5217-537X ; 0000-0001-7853-4094 ; 0000-0002-8963-2404 ; 0000-0002-1493-300X ; 0000-0001-9754-2233</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,3714,27901,27902</link.rule.ids><backlink>$$Uhttps://hal.science/hal-03383364$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Varga, J</creatorcontrib><creatorcontrib>Hogerheijde, M</creatorcontrib><creatorcontrib>Boekel, R van</creatorcontrib><creatorcontrib>Klarmann, L</creatorcontrib><creatorcontrib>Petrov, R</creatorcontrib><creatorcontrib>Waters, L B F M</creatorcontrib><creatorcontrib>Lagarde, S</creatorcontrib><creatorcontrib>Berio, Ph</creatorcontrib><creatorcontrib>Weigelt, G</creatorcontrib><creatorcontrib>Robbe-Dubois, S</creatorcontrib><creatorcontrib>Lopez, B</creatorcontrib><creatorcontrib>Millour, F</creatorcontrib><creatorcontrib>Augereau, J-C</creatorcontrib><creatorcontrib>Meheut, H</creatorcontrib><creatorcontrib>Meilland, A</creatorcontrib><creatorcontrib>Henning, Th</creatorcontrib><creatorcontrib>Jaffe, W</creatorcontrib><creatorcontrib>Bettonvil, F</creatorcontrib><creatorcontrib>Bristow, P</creatorcontrib><creatorcontrib>Hofmann, K-H</creatorcontrib><creatorcontrib>Matter, A</creatorcontrib><creatorcontrib>Allouche, F</creatorcontrib><creatorcontrib>Donnan, F</creatorcontrib><creatorcontrib>Heininger, M</creatorcontrib><creatorcontrib>Cruzalebes, P</creatorcontrib><creatorcontrib>Glindermann, A</creatorcontrib><creatorcontrib>Meisenheimer, K</creatorcontrib><creatorcontrib>Paladini, C</creatorcontrib><creatorcontrib>Scholler, M</creatorcontrib><creatorcontrib>Woillez, J</creatorcontrib><creatorcontrib>Venema, L</creatorcontrib><creatorcontrib>Kokoulina, E</creatorcontrib><creatorcontrib>Yoffe, G</creatorcontrib><creatorcontrib>Abadie, S</creatorcontrib><creatorcontrib>Abuter, R</creatorcontrib><creatorcontrib>Accardo, M</creatorcontrib><creatorcontrib>Adler, T</creatorcontrib><creatorcontrib>Antonelli, P</creatorcontrib><creatorcontrib>Bohm, A</creatorcontrib><creatorcontrib>Bailet, C</creatorcontrib><creatorcontrib>Bazin, G</creatorcontrib><creatorcontrib>Beltran, J</creatorcontrib><creatorcontrib>Boland, W</creatorcontrib><creatorcontrib>Bourget, P</creatorcontrib><creatorcontrib>Brast, R</creatorcontrib><creatorcontrib>Bresson, Y</creatorcontrib><creatorcontrib>Chelli, A</creatorcontrib><creatorcontrib>Cid, C</creatorcontrib><creatorcontrib>Clausse, J-M</creatorcontrib><creatorcontrib>Conzelmann, R D</creatorcontrib><creatorcontrib>Danchi, W-C</creatorcontrib><creatorcontrib>Hann, M De</creatorcontrib><creatorcontrib>Delbo, M</creatorcontrib><creatorcontrib>Ebert, M</creatorcontrib><creatorcontrib>Fantei, Y</creatorcontrib><creatorcontrib>Gallenne, A</creatorcontrib><creatorcontrib>Garces, E</creatorcontrib><creatorcontrib>Herrera, J C Gonzalez</creatorcontrib><creatorcontrib>Guitton, F</creatorcontrib><creatorcontrib>Hron, J</creatorcontrib><creatorcontrib>Hubin, N</creatorcontrib><creatorcontrib>Huerta, R</creatorcontrib><creatorcontrib>Ives, D</creatorcontrib><creatorcontrib>Jakob, G</creatorcontrib><creatorcontrib>Jasko, A</creatorcontrib><creatorcontrib>Jochum, L</creatorcontrib><creatorcontrib>Kragt, J</creatorcontrib><creatorcontrib>Kroes, G</creatorcontrib><creatorcontrib>Kuindersma, S</creatorcontrib><creatorcontrib>Laun, W</creatorcontrib><creatorcontrib>Leinert, C</creatorcontrib><creatorcontrib>Lizon, J-L</creatorcontrib><creatorcontrib>Lopez, M</creatorcontrib><creatorcontrib>Merand, A</creatorcontrib><creatorcontrib>Mauclert, N</creatorcontrib><creatorcontrib>Maurer, T</creatorcontrib><creatorcontrib>Meisner, J</creatorcontrib><creatorcontrib>Meixner, K</creatorcontrib><creatorcontrib>Mohr, L</creatorcontrib><creatorcontrib>Morel, S</creatorcontrib><creatorcontrib>Mosoni, L</creatorcontrib><creatorcontrib>Navarro, R</creatorcontrib><creatorcontrib>Pallanca, L</creatorcontrib><creatorcontrib>Pasquini, L</creatorcontrib><creatorcontrib>Percheron, I</creatorcontrib><creatorcontrib>Ridinger, A</creatorcontrib><creatorcontrib>Rigal, F</creatorcontrib><creatorcontrib>Riquelme, M</creatorcontrib><creatorcontrib>Rivinius, Th</creatorcontrib><creatorcontrib>Roelfsema, R</creatorcontrib><creatorcontrib>Schuhler, N</creatorcontrib><creatorcontrib>Schuil, M</creatorcontrib><creatorcontrib>Stee, P</creatorcontrib><creatorcontrib>Stephan, C</creatorcontrib><creatorcontrib>Horst, R ter</creatorcontrib><creatorcontrib>Tromp, N</creatorcontrib><creatorcontrib>Vakili, F</creatorcontrib><creatorcontrib>Duin, A van</creatorcontrib><creatorcontrib>Wittkowski, M</creatorcontrib><creatorcontrib>Wrhel, F</creatorcontrib><title>The Asymmetric Inner Disk of the Herbig Ae Star HD 163296 in the Eyes of VLTI/MATISSE: Evidence for a Vortex?</title><title>Astronomy and astrophysics (Berlin)</title><description>Context.A complex environment exists in the inner few astronomical units of planet-forming disks. High-angular-resolution observa-tions play a key role in our understanding of the disk structure and the dynamical processes at work.Aims.In this study we aim to characterize the mid-infrared brightness distribution of the inner disk of the young intermediate-massstar HD 163296 from early VLTI/MATISSE observations taken in theL- andN-bands. We put special emphasis on the detection ofpotential disk asymmetries.Methods.We use simple geometric models to fit the interferometric visibilities and closure phases. Our models include a smoothedring, a flat disk with an inner cavity, and a 2D Gaussian. The models can account for disk inclination and for azimuthal asymmetriesas well. We also perform numerical hydrodynamical simulations of the inner edge of the disk.Results.Our modeling reveals a significant brightness asymmetry in theL-band disk emission. The brightness maximum of the asym-metry is located at the NW part of the disk image, nearly at the position angle of the semimajor axis. The surface brightness ratio inthe azimuthal variation is3.5±0.2. Comparing our result on the location of the asymmetry with other interferometric measurements,we confirm that the morphology of ther<0.3au disk region is time-variable. We propose that this asymmetric structure, located in ornear the inner rim of the dusty disk, orbits the star. To find the physical origin of the asymmetry, we tested a hypothesis where a vortexis created by Rossby wave instability, and we find that a unique large-scale vortex may be compatible with our data. The half-lightradius of theL-band-emitting region is0.33±0.01au, the inclination is52◦+5◦−7◦, and the position angle is143◦±3◦. Our models predictthat a non-negligible fraction of theL-band disk emission originates inside the dust sublimation radius forμm-sized grains. Refractorygrains or large (&10μm-sized) grains could be the origin of this emission.N-band observations may also support a lack of smallsilicate grains in the innermost disk (r.0.6au), in agreement with our findings fromL-band data.</description><subject>Accretion disks</subject><subject>Astronomy</subject><subject>Asymmetric structures</subject><subject>Asymmetry</subject><subject>Brightness distribution</subject><subject>Celestial bodies</subject><subject>Emission</subject><subject>Inclination</subject><subject>Interferometry</subject><subject>Mathematical analysis</subject><subject>Planet formation</subject><subject>Planetary waves</subject><subject>Sciences of the Universe</subject><subject>Sublimation</subject><subject>Surface brightness</subject><subject>Two dimensional 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Sciences</general><scope>CYE</scope><scope>CYI</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0002-2725-6415</orcidid><orcidid>https://orcid.org/0000-0003-4989-575X</orcidid><orcidid>https://orcid.org/0000-0002-9765-7783</orcidid><orcidid>https://orcid.org/0000-0001-6015-646X</orcidid><orcidid>https://orcid.org/0000-0002-2958-4738</orcidid><orcidid>https://orcid.org/0000-0001-8220-0636</orcidid><orcidid>https://orcid.org/0000-0001-8400-687X</orcidid><orcidid>https://orcid.org/0000-0001-7517-8274</orcidid><orcidid>https://orcid.org/0000-0001-9332-3308</orcidid><orcidid>https://orcid.org/0000-0002-3393-2459</orcidid><orcidid>https://orcid.org/0000-0001-5217-537X</orcidid><orcidid>https://orcid.org/0000-0001-7853-4094</orcidid><orcidid>https://orcid.org/0000-0002-8963-2404</orcidid><orcidid>https://orcid.org/0000-0002-1493-300X</orcidid><orcidid>https://orcid.org/0000-0001-9754-2233</orcidid></search><sort><creationdate>20210301</creationdate><title>The Asymmetric Inner Disk of the Herbig Ae Star HD 163296 in the Eyes of VLTI/MATISSE: Evidence for a Vortex?</title><author>Varga, J ; Hogerheijde, M ; Boekel, R van ; Klarmann, L ; Petrov, R ; Waters, L B F M ; Lagarde, S ; Berio, Ph ; Weigelt, G ; Robbe-Dubois, S ; Lopez, B ; Millour, F ; Augereau, J-C ; Meheut, H ; Meilland, A ; Henning, Th ; Jaffe, W ; Bettonvil, F ; Bristow, P ; Hofmann, K-H ; Matter, A ; Allouche, F ; Donnan, F ; Heininger, M ; Cruzalebes, P ; Glindermann, A ; Meisenheimer, K ; Paladini, C ; Scholler, M ; Woillez, J ; Venema, L ; Kokoulina, E ; Yoffe, G ; Abadie, S ; Abuter, R ; Accardo, M ; Adler, T ; Antonelli, P ; Bohm, A ; Bailet, C ; Bazin, G ; Beltran, J ; Boland, W ; Bourget, P ; Brast, R ; Bresson, Y ; Chelli, A ; Cid, C ; Clausse, J-M ; Conzelmann, R D ; Danchi, W-C ; Hann, M De ; Delbo, M ; Ebert, M ; Fantei, Y ; Gallenne, A ; Garces, E ; Herrera, J C Gonzalez ; Guitton, F ; Hron, J ; Hubin, N ; Huerta, R ; Ives, D ; Jakob, G ; Jasko, A ; Jochum, L ; Kragt, J ; Kroes, G ; Kuindersma, S ; Laun, W ; Leinert, C ; Lizon, J-L ; Lopez, M ; Merand, A ; Mauclert, N ; Maurer, T ; Meisner, J ; Meixner, K ; Mohr, L ; Morel, S ; Mosoni, L ; Navarro, R ; Pallanca, L ; Pasquini, L ; Percheron, I ; Ridinger, A ; Rigal, F ; Riquelme, M ; Rivinius, Th ; Roelfsema, R ; Schuhler, N ; Schuil, M ; Stee, P ; Stephan, C ; Horst, R ter ; Tromp, N ; Vakili, F ; Duin, A van ; Wittkowski, M ; Wrhel, F</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c443t-3025ccd556e5f230159275e8013b10a3dc923be8426e196b2b930f326a4519e73</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Accretion disks</topic><topic>Astronomy</topic><topic>Asymmetric structures</topic><topic>Asymmetry</topic><topic>Brightness distribution</topic><topic>Celestial bodies</topic><topic>Emission</topic><topic>Inclination</topic><topic>Interferometry</topic><topic>Mathematical analysis</topic><topic>Planet formation</topic><topic>Planetary waves</topic><topic>Sciences of the Universe</topic><topic>Sublimation</topic><topic>Surface brightness</topic><topic>Two dimensional models</topic><topic>Vortices</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Varga, J</creatorcontrib><creatorcontrib>Hogerheijde, M</creatorcontrib><creatorcontrib>Boekel, R van</creatorcontrib><creatorcontrib>Klarmann, L</creatorcontrib><creatorcontrib>Petrov, R</creatorcontrib><creatorcontrib>Waters, L B F M</creatorcontrib><creatorcontrib>Lagarde, S</creatorcontrib><creatorcontrib>Berio, Ph</creatorcontrib><creatorcontrib>Weigelt, G</creatorcontrib><creatorcontrib>Robbe-Dubois, S</creatorcontrib><creatorcontrib>Lopez, B</creatorcontrib><creatorcontrib>Millour, F</creatorcontrib><creatorcontrib>Augereau, J-C</creatorcontrib><creatorcontrib>Meheut, H</creatorcontrib><creatorcontrib>Meilland, A</creatorcontrib><creatorcontrib>Henning, 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R</creatorcontrib><creatorcontrib>Ives, D</creatorcontrib><creatorcontrib>Jakob, G</creatorcontrib><creatorcontrib>Jasko, A</creatorcontrib><creatorcontrib>Jochum, L</creatorcontrib><creatorcontrib>Kragt, J</creatorcontrib><creatorcontrib>Kroes, G</creatorcontrib><creatorcontrib>Kuindersma, S</creatorcontrib><creatorcontrib>Laun, W</creatorcontrib><creatorcontrib>Leinert, C</creatorcontrib><creatorcontrib>Lizon, J-L</creatorcontrib><creatorcontrib>Lopez, M</creatorcontrib><creatorcontrib>Merand, A</creatorcontrib><creatorcontrib>Mauclert, N</creatorcontrib><creatorcontrib>Maurer, T</creatorcontrib><creatorcontrib>Meisner, J</creatorcontrib><creatorcontrib>Meixner, K</creatorcontrib><creatorcontrib>Mohr, L</creatorcontrib><creatorcontrib>Morel, S</creatorcontrib><creatorcontrib>Mosoni, L</creatorcontrib><creatorcontrib>Navarro, R</creatorcontrib><creatorcontrib>Pallanca, L</creatorcontrib><creatorcontrib>Pasquini, L</creatorcontrib><creatorcontrib>Percheron, I</creatorcontrib><creatorcontrib>Ridinger, A</creatorcontrib><creatorcontrib>Rigal, F</creatorcontrib><creatorcontrib>Riquelme, M</creatorcontrib><creatorcontrib>Rivinius, Th</creatorcontrib><creatorcontrib>Roelfsema, R</creatorcontrib><creatorcontrib>Schuhler, N</creatorcontrib><creatorcontrib>Schuil, M</creatorcontrib><creatorcontrib>Stee, P</creatorcontrib><creatorcontrib>Stephan, C</creatorcontrib><creatorcontrib>Horst, R ter</creatorcontrib><creatorcontrib>Tromp, N</creatorcontrib><creatorcontrib>Vakili, F</creatorcontrib><creatorcontrib>Duin, A van</creatorcontrib><creatorcontrib>Wittkowski, M</creatorcontrib><creatorcontrib>Wrhel, F</creatorcontrib><collection>NASA Scientific and Technical Information</collection><collection>NASA Technical Reports Server</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Varga, J</au><au>Hogerheijde, M</au><au>Boekel, R van</au><au>Klarmann, L</au><au>Petrov, R</au><au>Waters, L B F M</au><au>Lagarde, S</au><au>Berio, Ph</au><au>Weigelt, G</au><au>Robbe-Dubois, S</au><au>Lopez, B</au><au>Millour, F</au><au>Augereau, J-C</au><au>Meheut, H</au><au>Meilland, A</au><au>Henning, Th</au><au>Jaffe, W</au><au>Bettonvil, F</au><au>Bristow, P</au><au>Hofmann, K-H</au><au>Matter, A</au><au>Allouche, F</au><au>Donnan, F</au><au>Heininger, M</au><au>Cruzalebes, P</au><au>Glindermann, A</au><au>Meisenheimer, K</au><au>Paladini, C</au><au>Scholler, M</au><au>Woillez, J</au><au>Venema, L</au><au>Kokoulina, E</au><au>Yoffe, G</au><au>Abadie, S</au><au>Abuter, R</au><au>Accardo, M</au><au>Adler, T</au><au>Antonelli, P</au><au>Bohm, A</au><au>Bailet, C</au><au>Bazin, G</au><au>Beltran, J</au><au>Boland, W</au><au>Bourget, P</au><au>Brast, R</au><au>Bresson, Y</au><au>Chelli, A</au><au>Cid, C</au><au>Clausse, J-M</au><au>Conzelmann, R D</au><au>Danchi, W-C</au><au>Hann, M De</au><au>Delbo, M</au><au>Ebert, M</au><au>Fantei, Y</au><au>Gallenne, A</au><au>Garces, E</au><au>Herrera, J C Gonzalez</au><au>Guitton, F</au><au>Hron, J</au><au>Hubin, N</au><au>Huerta, R</au><au>Ives, D</au><au>Jakob, G</au><au>Jasko, A</au><au>Jochum, L</au><au>Kragt, J</au><au>Kroes, G</au><au>Kuindersma, S</au><au>Laun, W</au><au>Leinert, C</au><au>Lizon, J-L</au><au>Lopez, M</au><au>Merand, A</au><au>Mauclert, N</au><au>Maurer, T</au><au>Meisner, J</au><au>Meixner, K</au><au>Mohr, L</au><au>Morel, S</au><au>Mosoni, L</au><au>Navarro, R</au><au>Pallanca, L</au><au>Pasquini, L</au><au>Percheron, I</au><au>Ridinger, A</au><au>Rigal, F</au><au>Riquelme, M</au><au>Rivinius, Th</au><au>Roelfsema, R</au><au>Schuhler, N</au><au>Schuil, M</au><au>Stee, P</au><au>Stephan, C</au><au>Horst, R ter</au><au>Tromp, N</au><au>Vakili, F</au><au>Duin, A van</au><au>Wittkowski, M</au><au>Wrhel, F</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Asymmetric Inner Disk of the Herbig Ae Star HD 163296 in the Eyes of VLTI/MATISSE: Evidence for a Vortex?</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2021-03-01</date><risdate>2021</risdate><volume>647</volume><spage>A56</spage><pages>A56-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><eissn>1432-0756</eissn><abstract>Context.A complex environment exists in the inner few astronomical units of planet-forming disks. High-angular-resolution observa-tions play a key role in our understanding of the disk structure and the dynamical processes at work.Aims.In this study we aim to characterize the mid-infrared brightness distribution of the inner disk of the young intermediate-massstar HD 163296 from early VLTI/MATISSE observations taken in theL- andN-bands. We put special emphasis on the detection ofpotential disk asymmetries.Methods.We use simple geometric models to fit the interferometric visibilities and closure phases. Our models include a smoothedring, a flat disk with an inner cavity, and a 2D Gaussian. The models can account for disk inclination and for azimuthal asymmetriesas well. We also perform numerical hydrodynamical simulations of the inner edge of the disk.Results.Our modeling reveals a significant brightness asymmetry in theL-band disk emission. The brightness maximum of the asym-metry is located at the NW part of the disk image, nearly at the position angle of the semimajor axis. The surface brightness ratio inthe azimuthal variation is3.5±0.2. Comparing our result on the location of the asymmetry with other interferometric measurements,we confirm that the morphology of ther<0.3au disk region is time-variable. We propose that this asymmetric structure, located in ornear the inner rim of the dusty disk, orbits the star. To find the physical origin of the asymmetry, we tested a hypothesis where a vortexis created by Rossby wave instability, and we find that a unique large-scale vortex may be compatible with our data. The half-lightradius of theL-band-emitting region is0.33±0.01au, the inclination is52◦+5◦−7◦, and the position angle is143◦±3◦. Our models predictthat a non-negligible fraction of theL-band disk emission originates inside the dust sublimation radius forμm-sized grains. Refractorygrains or large (&10μm-sized) grains could be the origin of this emission.N-band observations may also support a lack of smallsilicate grains in the innermost disk (r.0.6au), in agreement with our findings fromL-band data.</abstract><cop>Goddard Space Flight Center</cop><pub>EDP Sciences</pub><doi>10.1051/0004-6361/202039400</doi><orcidid>https://orcid.org/0000-0002-2725-6415</orcidid><orcidid>https://orcid.org/0000-0003-4989-575X</orcidid><orcidid>https://orcid.org/0000-0002-9765-7783</orcidid><orcidid>https://orcid.org/0000-0001-6015-646X</orcidid><orcidid>https://orcid.org/0000-0002-2958-4738</orcidid><orcidid>https://orcid.org/0000-0001-8220-0636</orcidid><orcidid>https://orcid.org/0000-0001-8400-687X</orcidid><orcidid>https://orcid.org/0000-0001-7517-8274</orcidid><orcidid>https://orcid.org/0000-0001-9332-3308</orcidid><orcidid>https://orcid.org/0000-0002-3393-2459</orcidid><orcidid>https://orcid.org/0000-0001-5217-537X</orcidid><orcidid>https://orcid.org/0000-0001-7853-4094</orcidid><orcidid>https://orcid.org/0000-0002-8963-2404</orcidid><orcidid>https://orcid.org/0000-0002-1493-300X</orcidid><orcidid>https://orcid.org/0000-0001-9754-2233</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0004-6361 |
| ispartof | Astronomy and astrophysics (Berlin), 2021-03, Vol.647, p.A56 |
| issn | 0004-6361 1432-0746 1432-0756 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_hal_03383364v1 |
| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; EDP Sciences; NASA Technical Reports Server; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals |
| subjects | Accretion disks Astronomy Asymmetric structures Asymmetry Brightness distribution Celestial bodies Emission Inclination Interferometry Mathematical analysis Planet formation Planetary waves Sciences of the Universe Sublimation Surface brightness Two dimensional models Vortices |
| title | The Asymmetric Inner Disk of the Herbig Ae Star HD 163296 in the Eyes of VLTI/MATISSE: Evidence for a Vortex? |
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