Binary-induced spiral arms inside the disc cavity of AB Aurigae
ABSTRACT In this work we demonstrate that the inner spiral structure observed in AB Aurigae can be created by a binary star orbiting inside the dust cavity. We find that a companion with a mass-ratio of 0.25, semimajor axis of 40 au, eccentricity of 0.5, and inclination of 90° produces gaseous spira...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2020-08, Vol.496 (2), p.2362-2371 |
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| container_title | Monthly notices of the Royal Astronomical Society |
| container_volume | 496 |
| creator | Poblete, Pedro P Calcino, Josh Cuello, Nicolás Macías, Enrique Ribas, Álvaro Price, Daniel J Cuadra, Jorge Pinte, Christophe |
| description | ABSTRACT
In this work we demonstrate that the inner spiral structure observed in AB Aurigae can be created by a binary star orbiting inside the dust cavity. We find that a companion with a mass-ratio of 0.25, semimajor axis of 40 au, eccentricity of 0.5, and inclination of 90° produces gaseous spirals closely matching the ones observed in 12CO (2-1) line emission. Based on dust dynamics in circumbinary discs (Poblete, Cuello & Cuadra 2019), we constrain the inclination of the binary with respect to the circumbinary disc to range between 60° and 90°. We predict that the stellar companion is located roughly 0.18 arcsec from the central star towards the east-southeast, above the plane of the disc. Should this companion be detected in the near future, our model indicates that it should be moving away from the primary star at a rate of 6 mas yr−1 on the plane of the sky. Since our companion is inclined, we also predict that the spiral structure will appear to change with time, and not simply corotate with the companion. |
| doi_str_mv | 10.1093/mnras/staa1655 |
| format | Article |
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In this work we demonstrate that the inner spiral structure observed in AB Aurigae can be created by a binary star orbiting inside the dust cavity. We find that a companion with a mass-ratio of 0.25, semimajor axis of 40 au, eccentricity of 0.5, and inclination of 90° produces gaseous spirals closely matching the ones observed in 12CO (2-1) line emission. Based on dust dynamics in circumbinary discs (Poblete, Cuello & Cuadra 2019), we constrain the inclination of the binary with respect to the circumbinary disc to range between 60° and 90°. We predict that the stellar companion is located roughly 0.18 arcsec from the central star towards the east-southeast, above the plane of the disc. Should this companion be detected in the near future, our model indicates that it should be moving away from the primary star at a rate of 6 mas yr−1 on the plane of the sky. Since our companion is inclined, we also predict that the spiral structure will appear to change with time, and not simply corotate with the companion.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/staa1655</identifier><language>eng</language><publisher>Oxford University Press</publisher><subject>Astrophysics ; Earth and Planetary Astrophysics ; Physics ; Solar and Stellar Astrophysics</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2020-08, Vol.496 (2), p.2362-2371</ispartof><rights>2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2020</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-c347t-3b175c985815fcf2262156da946d0d3203c90b37c6bbe892b02808c9e6556b7b3</citedby><cites>FETCH-LOGICAL-c347t-3b175c985815fcf2262156da946d0d3203c90b37c6bbe892b02808c9e6556b7b3</cites><orcidid>0000-0003-3713-8073 ; 0000-0003-1283-6262 ; 0000-0002-4716-4235 ; 0000-0001-5907-5179</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,780,784,885,1604,27924,27925</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/staa1655$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc><backlink>$$Uhttps://hal.science/hal-02898006$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Poblete, Pedro P</creatorcontrib><creatorcontrib>Calcino, Josh</creatorcontrib><creatorcontrib>Cuello, Nicolás</creatorcontrib><creatorcontrib>Macías, Enrique</creatorcontrib><creatorcontrib>Ribas, Álvaro</creatorcontrib><creatorcontrib>Price, Daniel J</creatorcontrib><creatorcontrib>Cuadra, Jorge</creatorcontrib><creatorcontrib>Pinte, Christophe</creatorcontrib><title>Binary-induced spiral arms inside the disc cavity of AB Aurigae</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
In this work we demonstrate that the inner spiral structure observed in AB Aurigae can be created by a binary star orbiting inside the dust cavity. We find that a companion with a mass-ratio of 0.25, semimajor axis of 40 au, eccentricity of 0.5, and inclination of 90° produces gaseous spirals closely matching the ones observed in 12CO (2-1) line emission. Based on dust dynamics in circumbinary discs (Poblete, Cuello & Cuadra 2019), we constrain the inclination of the binary with respect to the circumbinary disc to range between 60° and 90°. We predict that the stellar companion is located roughly 0.18 arcsec from the central star towards the east-southeast, above the plane of the disc. Should this companion be detected in the near future, our model indicates that it should be moving away from the primary star at a rate of 6 mas yr−1 on the plane of the sky. Since our companion is inclined, we also predict that the spiral structure will appear to change with time, and not simply corotate with the companion.</description><subject>Astrophysics</subject><subject>Earth and Planetary Astrophysics</subject><subject>Physics</subject><subject>Solar and Stellar Astrophysics</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNqFkLtOAzEQRS0EEiHQUrul2GRsx167YxMBQYpEA7Xl1xKjZDeyN5HyN3wLX8aG8CipRhqdezVzELomMCKg2HjdJJPHuTOGCM5P0IAwwQuqhDhFAwDGC1kSco4ucn4DgAmjYoBup7ExaV_Exm9d8DhvYjIrbNI649jk6APulgH7mB12Zhe7PW5rXE0_3qttiq8mXKKz2qxyuPqeQ_Ryf_c8mxeLp4fHWbUoHJuUXcEsKblTkkvCa1dTKijhwhs1ER48o8CcAstKJ6wNUlELVIJ0KvSvCFtaNkQ3x96lWelNiuv-at2aqOfVQh92fUBJALEjPTs6si61OadQ_wYI6IMr_eVK_7j6K2-3m__YT67Ra9w</recordid><startdate>20200801</startdate><enddate>20200801</enddate><creator>Poblete, Pedro P</creator><creator>Calcino, Josh</creator><creator>Cuello, Nicolás</creator><creator>Macías, Enrique</creator><creator>Ribas, Álvaro</creator><creator>Price, Daniel J</creator><creator>Cuadra, Jorge</creator><creator>Pinte, Christophe</creator><general>Oxford University Press</general><general>Oxford University Press (OUP): Policy P - Oxford Open Option A</general><scope>AAYXX</scope><scope>CITATION</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0003-3713-8073</orcidid><orcidid>https://orcid.org/0000-0003-1283-6262</orcidid><orcidid>https://orcid.org/0000-0002-4716-4235</orcidid><orcidid>https://orcid.org/0000-0001-5907-5179</orcidid></search><sort><creationdate>20200801</creationdate><title>Binary-induced spiral arms inside the disc cavity of AB Aurigae</title><author>Poblete, Pedro P ; Calcino, Josh ; Cuello, Nicolás ; Macías, Enrique ; Ribas, Álvaro ; Price, Daniel J ; Cuadra, Jorge ; Pinte, Christophe</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c347t-3b175c985815fcf2262156da946d0d3203c90b37c6bbe892b02808c9e6556b7b3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>Astrophysics</topic><topic>Earth and Planetary Astrophysics</topic><topic>Physics</topic><topic>Solar and Stellar Astrophysics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Poblete, Pedro P</creatorcontrib><creatorcontrib>Calcino, Josh</creatorcontrib><creatorcontrib>Cuello, Nicolás</creatorcontrib><creatorcontrib>Macías, Enrique</creatorcontrib><creatorcontrib>Ribas, Álvaro</creatorcontrib><creatorcontrib>Price, Daniel J</creatorcontrib><creatorcontrib>Cuadra, Jorge</creatorcontrib><creatorcontrib>Pinte, Christophe</creatorcontrib><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Poblete, Pedro P</au><au>Calcino, Josh</au><au>Cuello, Nicolás</au><au>Macías, Enrique</au><au>Ribas, Álvaro</au><au>Price, Daniel J</au><au>Cuadra, Jorge</au><au>Pinte, Christophe</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Binary-induced spiral arms inside the disc cavity of AB Aurigae</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2020-08-01</date><risdate>2020</risdate><volume>496</volume><issue>2</issue><spage>2362</spage><epage>2371</epage><pages>2362-2371</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
In this work we demonstrate that the inner spiral structure observed in AB Aurigae can be created by a binary star orbiting inside the dust cavity. We find that a companion with a mass-ratio of 0.25, semimajor axis of 40 au, eccentricity of 0.5, and inclination of 90° produces gaseous spirals closely matching the ones observed in 12CO (2-1) line emission. Based on dust dynamics in circumbinary discs (Poblete, Cuello & Cuadra 2019), we constrain the inclination of the binary with respect to the circumbinary disc to range between 60° and 90°. We predict that the stellar companion is located roughly 0.18 arcsec from the central star towards the east-southeast, above the plane of the disc. Should this companion be detected in the near future, our model indicates that it should be moving away from the primary star at a rate of 6 mas yr−1 on the plane of the sky. Since our companion is inclined, we also predict that the spiral structure will appear to change with time, and not simply corotate with the companion.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/staa1655</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0003-3713-8073</orcidid><orcidid>https://orcid.org/0000-0003-1283-6262</orcidid><orcidid>https://orcid.org/0000-0002-4716-4235</orcidid><orcidid>https://orcid.org/0000-0001-5907-5179</orcidid><oa>free_for_read</oa></addata></record> |
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| title | Binary-induced spiral arms inside the disc cavity of AB Aurigae |
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