A possible misaligned orbit for the young planet AU Mic c
The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously wi...
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| creator | H Yu Garai, Z Cretignier, M Szabó, Gy M Aigrain, S Gandolfi, D Bryant, E M Correia, A C M Klein, B Brandeker, A Owen, J E Günther, M N Winn, J N Heitzmann, A Cegla, H M Wilson, T G Gill, S Kriskovics, L Barragán, O Boldog, A Nielsen, L D Billot, N Lafarga, M Meech, A Alibert, Y Alonso, R Bárczy, T Barrado, D Barros, S C C Baumjohann, W Bayliss, D Benz, W Bergomi, M Borsato, L Broeg, C A Collier Cameron Csizmadia, Sz Cubillos, P E Davies, M B Deleuil, M Deline, A Demangeon, O D S Demory, B O Derekas, A Doyle, L Edwards, B Egger, J A Ehrenreich, D Erikson, A tier, A Fossati, L Fridlund, M Gazeas, K Gillon, M Güdel, M Isaak, K G Kiss, L L Korth, J Lam, K W F Laskar, J A Lecavelier des Etangs Lendl, M Magrin, D Maxted, P F L McCormac, J Merín, B Mordasini, C Nascimbeni, V O'Brien, S M Olofsson, G Ottensamer, R Pagano, I Pallé, E Peter, G Piazza, D Piotto, G Pollacco, D Queloz, D Ragazzoni, R Rando, N Rauer, H Ribas, I Santos, N C Scandariato, G Ségransan, D Simon, A E Smith, A M S Sousa, S G Southworth, R Stalport, M Steinberger, M Sulis, S Udry, S Ulmer, B Ulmer-Moll, S V Van Grootel Venturini, J Villaver, E Walton, N A Wheatley, P J |
| description | The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range \(\lambda_c=67.8_{-49.0}^{+31.7}\)\,degrees (1-\(\sigma\)). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b (\(\lambda_b=-2.96_{-10.30}^{+10.44}\)\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely. |
| doi_str_mv | 10.48550/arxiv.2411.16958 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_arxiv</sourceid><recordid>TN_cdi_proquest_journals_3133540117</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>3133540117</sourcerecordid><originalsourceid>FETCH-LOGICAL-a527-3e4e22ce296dcf47ffe7d77652b2bd9542c08524f9b205d4929ae8661adb63b83</originalsourceid><addsrcrecordid>eNotj01LwzAch4MgOOY-gCcDnluTf96PY_gymHiZ55K06czompq04r69c_P0uzz8eB6E7igpuRaCPNr0E75L4JSWVBqhr9AMGKOF5gA3aJHznhACUoEQbIbMEg8x5-A6jw8h2y7set_gmFwYcRsTHj89Psap3-Ghs70f8fIDv4Ua17fourVd9ov_naPt89N29Vps3l_Wq-WmsAJUwTz3ALUHI5u65aptvWqUkgIcuMYIDjXRAnhrHBDRcAPGei0ltY2TzGk2R_eX23NXNaRwsOlY_fVV574T8XAhhhS_Jp_Hah-n1J-cKkYZE5xQqtgvkcZRJQ</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>3133540117</pqid></control><display><type>article</type><title>A possible misaligned orbit for the young planet AU Mic c</title><source>arXiv.org</source><source>Free E- Journals</source><creator>H Yu ; Garai, Z ; Cretignier, M ; Szabó, Gy M ; Aigrain, S ; Gandolfi, D ; Bryant, E M ; Correia, A C M ; Klein, B ; Brandeker, A ; Owen, J E ; Günther, M N ; Winn, J N ; Heitzmann, A ; Cegla, H M ; Wilson, T G ; Gill, S ; Kriskovics, L ; Barragán, O ; Boldog, A ; Nielsen, L D ; Billot, N ; Lafarga, M ; Meech, A ; Alibert, Y ; Alonso, R ; Bárczy, T ; Barrado, D ; Barros, S C C ; Baumjohann, W ; Bayliss, D ; Benz, W ; Bergomi, M ; Borsato, L ; Broeg, C ; A Collier Cameron ; Csizmadia, Sz ; Cubillos, P E ; Davies, M B ; Deleuil, M ; Deline, A ; Demangeon, O D S ; Demory, B O ; Derekas, A ; Doyle, L ; Edwards, B ; Egger, J A ; Ehrenreich, D ; Erikson, A ; tier, A ; Fossati, L ; Fridlund, M ; Gazeas, K ; Gillon, M ; Güdel, M ; Isaak, K G ; Kiss, L L ; Korth, J ; Lam, K W F ; Laskar, J ; A Lecavelier des Etangs ; Lendl, M ; Magrin, D ; Maxted, P F L ; McCormac, J ; Merín, B ; Mordasini, C ; Nascimbeni, V ; O'Brien, S M ; Olofsson, G ; Ottensamer, R ; Pagano, I ; Pallé, E ; Peter, G ; Piazza, D ; Piotto, G ; Pollacco, D ; Queloz, D ; Ragazzoni, R ; Rando, N ; Rauer, H ; Ribas, I ; Santos, N C ; Scandariato, G ; Ségransan, D ; Simon, A E ; Smith, A M S ; Sousa, S G ; Southworth, R ; Stalport, M ; Steinberger, M ; Sulis, S ; Udry, S ; Ulmer, B ; Ulmer-Moll, S ; V Van Grootel ; Venturini, J ; Villaver, E ; Walton, N A ; Wheatley, P J</creator><creatorcontrib>H Yu ; Garai, Z ; Cretignier, M ; Szabó, Gy M ; Aigrain, S ; Gandolfi, D ; Bryant, E M ; Correia, A C M ; Klein, B ; Brandeker, A ; Owen, J E ; Günther, M N ; Winn, J N ; Heitzmann, A ; Cegla, H M ; Wilson, T G ; Gill, S ; Kriskovics, L ; Barragán, O ; Boldog, A ; Nielsen, L D ; Billot, N ; Lafarga, M ; Meech, A ; Alibert, Y ; Alonso, R ; Bárczy, T ; Barrado, D ; Barros, S C C ; Baumjohann, W ; Bayliss, D ; Benz, W ; Bergomi, M ; Borsato, L ; Broeg, C ; A Collier Cameron ; Csizmadia, Sz ; Cubillos, P E ; Davies, M B ; Deleuil, M ; Deline, A ; Demangeon, O D S ; Demory, B O ; Derekas, A ; Doyle, L ; Edwards, B ; Egger, J A ; Ehrenreich, D ; Erikson, A ; tier, A ; Fossati, L ; Fridlund, M ; Gazeas, K ; Gillon, M ; Güdel, M ; Isaak, K G ; Kiss, L L ; Korth, J ; Lam, K W F ; Laskar, J ; A Lecavelier des Etangs ; Lendl, M ; Magrin, D ; Maxted, P F L ; McCormac, J ; Merín, B ; Mordasini, C ; Nascimbeni, V ; O'Brien, S M ; Olofsson, G ; Ottensamer, R ; Pagano, I ; Pallé, E ; Peter, G ; Piazza, D ; Piotto, G ; Pollacco, D ; Queloz, D ; Ragazzoni, R ; Rando, N ; Rauer, H ; Ribas, I ; Santos, N C ; Scandariato, G ; Ségransan, D ; Simon, A E ; Smith, A M S ; Sousa, S G ; Southworth, R ; Stalport, M ; Steinberger, M ; Sulis, S ; Udry, S ; Ulmer, B ; Ulmer-Moll, S ; V Van Grootel ; Venturini, J ; Villaver, E ; Walton, N A ; Wheatley, P J</creatorcontrib><description>The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range \(\lambda_c=67.8_{-49.0}^{+31.7}\)\,degrees (1-\(\sigma\)). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b (\(\lambda_b=-2.96_{-10.30}^{+10.44}\)\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2411.16958</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Orbital stability ; Physics - Earth and Planetary Astrophysics ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics ; Planetary orbits ; Planetary systems ; Systems stability</subject><ispartof>arXiv.org, 2024-12</ispartof><rights>2024. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27925</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2411.16958$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1093/mnras/stae2655$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>H Yu</creatorcontrib><creatorcontrib>Garai, Z</creatorcontrib><creatorcontrib>Cretignier, M</creatorcontrib><creatorcontrib>Szabó, Gy M</creatorcontrib><creatorcontrib>Aigrain, S</creatorcontrib><creatorcontrib>Gandolfi, D</creatorcontrib><creatorcontrib>Bryant, E M</creatorcontrib><creatorcontrib>Correia, A C M</creatorcontrib><creatorcontrib>Klein, B</creatorcontrib><creatorcontrib>Brandeker, A</creatorcontrib><creatorcontrib>Owen, J E</creatorcontrib><creatorcontrib>Günther, M N</creatorcontrib><creatorcontrib>Winn, J N</creatorcontrib><creatorcontrib>Heitzmann, A</creatorcontrib><creatorcontrib>Cegla, H M</creatorcontrib><creatorcontrib>Wilson, T G</creatorcontrib><creatorcontrib>Gill, S</creatorcontrib><creatorcontrib>Kriskovics, L</creatorcontrib><creatorcontrib>Barragán, O</creatorcontrib><creatorcontrib>Boldog, A</creatorcontrib><creatorcontrib>Nielsen, L D</creatorcontrib><creatorcontrib>Billot, N</creatorcontrib><creatorcontrib>Lafarga, M</creatorcontrib><creatorcontrib>Meech, A</creatorcontrib><creatorcontrib>Alibert, Y</creatorcontrib><creatorcontrib>Alonso, R</creatorcontrib><creatorcontrib>Bárczy, T</creatorcontrib><creatorcontrib>Barrado, D</creatorcontrib><creatorcontrib>Barros, S C C</creatorcontrib><creatorcontrib>Baumjohann, W</creatorcontrib><creatorcontrib>Bayliss, D</creatorcontrib><creatorcontrib>Benz, W</creatorcontrib><creatorcontrib>Bergomi, M</creatorcontrib><creatorcontrib>Borsato, L</creatorcontrib><creatorcontrib>Broeg, C</creatorcontrib><creatorcontrib>A Collier Cameron</creatorcontrib><creatorcontrib>Csizmadia, Sz</creatorcontrib><creatorcontrib>Cubillos, P E</creatorcontrib><creatorcontrib>Davies, M B</creatorcontrib><creatorcontrib>Deleuil, M</creatorcontrib><creatorcontrib>Deline, A</creatorcontrib><creatorcontrib>Demangeon, O D S</creatorcontrib><creatorcontrib>Demory, B O</creatorcontrib><creatorcontrib>Derekas, A</creatorcontrib><creatorcontrib>Doyle, L</creatorcontrib><creatorcontrib>Edwards, B</creatorcontrib><creatorcontrib>Egger, J A</creatorcontrib><creatorcontrib>Ehrenreich, D</creatorcontrib><creatorcontrib>Erikson, A</creatorcontrib><creatorcontrib>tier, A</creatorcontrib><creatorcontrib>Fossati, L</creatorcontrib><creatorcontrib>Fridlund, M</creatorcontrib><creatorcontrib>Gazeas, K</creatorcontrib><creatorcontrib>Gillon, M</creatorcontrib><creatorcontrib>Güdel, M</creatorcontrib><creatorcontrib>Isaak, K G</creatorcontrib><creatorcontrib>Kiss, L L</creatorcontrib><creatorcontrib>Korth, J</creatorcontrib><creatorcontrib>Lam, K W F</creatorcontrib><creatorcontrib>Laskar, J</creatorcontrib><creatorcontrib>A Lecavelier des Etangs</creatorcontrib><creatorcontrib>Lendl, M</creatorcontrib><creatorcontrib>Magrin, D</creatorcontrib><creatorcontrib>Maxted, P F L</creatorcontrib><creatorcontrib>McCormac, J</creatorcontrib><creatorcontrib>Merín, B</creatorcontrib><creatorcontrib>Mordasini, C</creatorcontrib><creatorcontrib>Nascimbeni, V</creatorcontrib><creatorcontrib>O'Brien, S M</creatorcontrib><creatorcontrib>Olofsson, G</creatorcontrib><creatorcontrib>Ottensamer, R</creatorcontrib><creatorcontrib>Pagano, I</creatorcontrib><creatorcontrib>Pallé, E</creatorcontrib><creatorcontrib>Peter, G</creatorcontrib><creatorcontrib>Piazza, D</creatorcontrib><creatorcontrib>Piotto, G</creatorcontrib><creatorcontrib>Pollacco, D</creatorcontrib><creatorcontrib>Queloz, D</creatorcontrib><creatorcontrib>Ragazzoni, R</creatorcontrib><creatorcontrib>Rando, N</creatorcontrib><creatorcontrib>Rauer, H</creatorcontrib><creatorcontrib>Ribas, I</creatorcontrib><creatorcontrib>Santos, N C</creatorcontrib><creatorcontrib>Scandariato, G</creatorcontrib><creatorcontrib>Ségransan, D</creatorcontrib><creatorcontrib>Simon, A E</creatorcontrib><creatorcontrib>Smith, A M S</creatorcontrib><creatorcontrib>Sousa, S G</creatorcontrib><creatorcontrib>Southworth, R</creatorcontrib><creatorcontrib>Stalport, M</creatorcontrib><creatorcontrib>Steinberger, M</creatorcontrib><creatorcontrib>Sulis, S</creatorcontrib><creatorcontrib>Udry, S</creatorcontrib><creatorcontrib>Ulmer, B</creatorcontrib><creatorcontrib>Ulmer-Moll, S</creatorcontrib><creatorcontrib>V Van Grootel</creatorcontrib><creatorcontrib>Venturini, J</creatorcontrib><creatorcontrib>Villaver, E</creatorcontrib><creatorcontrib>Walton, N A</creatorcontrib><creatorcontrib>Wheatley, P J</creatorcontrib><title>A possible misaligned orbit for the young planet AU Mic c</title><title>arXiv.org</title><description>The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range \(\lambda_c=67.8_{-49.0}^{+31.7}\)\,degrees (1-\(\sigma\)). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b (\(\lambda_b=-2.96_{-10.30}^{+10.44}\)\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely.</description><subject>Orbital stability</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Planetary orbits</subject><subject>Planetary systems</subject><subject>Systems stability</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotj01LwzAch4MgOOY-gCcDnluTf96PY_gymHiZ55K06czompq04r69c_P0uzz8eB6E7igpuRaCPNr0E75L4JSWVBqhr9AMGKOF5gA3aJHznhACUoEQbIbMEg8x5-A6jw8h2y7set_gmFwYcRsTHj89Psap3-Ghs70f8fIDv4Ua17fourVd9ov_naPt89N29Vps3l_Wq-WmsAJUwTz3ALUHI5u65aptvWqUkgIcuMYIDjXRAnhrHBDRcAPGei0ltY2TzGk2R_eX23NXNaRwsOlY_fVV574T8XAhhhS_Jp_Hah-n1J-cKkYZE5xQqtgvkcZRJQ</recordid><startdate>20241220</startdate><enddate>20241220</enddate><creator>H Yu</creator><creator>Garai, Z</creator><creator>Cretignier, M</creator><creator>Szabó, Gy M</creator><creator>Aigrain, S</creator><creator>Gandolfi, D</creator><creator>Bryant, E M</creator><creator>Correia, A C M</creator><creator>Klein, 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arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20241220</creationdate><title>A possible misaligned orbit for the young planet AU Mic c</title><author>H Yu ; Garai, Z ; Cretignier, M ; Szabó, Gy M ; Aigrain, S ; Gandolfi, D ; Bryant, E M ; Correia, A C M ; Klein, B ; Brandeker, A ; Owen, J E ; Günther, M N ; Winn, J N ; Heitzmann, A ; Cegla, H M ; Wilson, T G ; Gill, S ; Kriskovics, L ; Barragán, O ; Boldog, A ; Nielsen, L D ; Billot, N ; Lafarga, M ; Meech, A ; Alibert, Y ; Alonso, R ; Bárczy, T ; Barrado, D ; Barros, S C C ; Baumjohann, W ; Bayliss, D ; Benz, W ; Bergomi, M ; Borsato, L ; Broeg, C ; A Collier Cameron ; Csizmadia, Sz ; Cubillos, P E ; Davies, M B ; Deleuil, M ; Deline, A ; Demangeon, O D S ; Demory, B O ; Derekas, A ; Doyle, L ; Edwards, B ; Egger, J A ; Ehrenreich, D ; Erikson, A ; tier, A ; Fossati, L ; Fridlund, M ; Gazeas, K ; Gillon, M ; Güdel, M ; Isaak, K G ; Kiss, L L ; Korth, J ; Lam, K W F ; Laskar, J ; A Lecavelier des Etangs ; Lendl, M ; Magrin, D ; Maxted, P F L ; McCormac, J ; Merín, B ; Mordasini, C ; Nascimbeni, V ; O'Brien, S M ; Olofsson, G ; Ottensamer, R ; Pagano, I ; Pallé, E ; Peter, G ; Piazza, D ; Piotto, G ; Pollacco, D ; Queloz, D ; Ragazzoni, R ; Rando, N ; Rauer, H ; Ribas, I ; Santos, N C ; Scandariato, G ; Ségransan, D ; Simon, A E ; Smith, A M S ; Sousa, S G ; Southworth, R ; Stalport, M ; Steinberger, M ; Sulis, S ; Udry, S ; Ulmer, B ; Ulmer-Moll, S ; V Van Grootel ; Venturini, J ; Villaver, E ; Walton, N A ; Wheatley, P J</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a527-3e4e22ce296dcf47ffe7d77652b2bd9542c08524f9b205d4929ae8661adb63b83</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Orbital stability</topic><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Instrumentation and Methods for Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Planetary orbits</topic><topic>Planetary systems</topic><topic>Systems stability</topic><toplevel>online_resources</toplevel><creatorcontrib>H Yu</creatorcontrib><creatorcontrib>Garai, Z</creatorcontrib><creatorcontrib>Cretignier, M</creatorcontrib><creatorcontrib>Szabó, Gy M</creatorcontrib><creatorcontrib>Aigrain, S</creatorcontrib><creatorcontrib>Gandolfi, D</creatorcontrib><creatorcontrib>Bryant, E M</creatorcontrib><creatorcontrib>Correia, A C M</creatorcontrib><creatorcontrib>Klein, B</creatorcontrib><creatorcontrib>Brandeker, A</creatorcontrib><creatorcontrib>Owen, J E</creatorcontrib><creatorcontrib>Günther, M N</creatorcontrib><creatorcontrib>Winn, J N</creatorcontrib><creatorcontrib>Heitzmann, A</creatorcontrib><creatorcontrib>Cegla, H M</creatorcontrib><creatorcontrib>Wilson, T G</creatorcontrib><creatorcontrib>Gill, S</creatorcontrib><creatorcontrib>Kriskovics, L</creatorcontrib><creatorcontrib>Barragán, O</creatorcontrib><creatorcontrib>Boldog, A</creatorcontrib><creatorcontrib>Nielsen, L D</creatorcontrib><creatorcontrib>Billot, N</creatorcontrib><creatorcontrib>Lafarga, M</creatorcontrib><creatorcontrib>Meech, A</creatorcontrib><creatorcontrib>Alibert, Y</creatorcontrib><creatorcontrib>Alonso, R</creatorcontrib><creatorcontrib>Bárczy, T</creatorcontrib><creatorcontrib>Barrado, D</creatorcontrib><creatorcontrib>Barros, S C C</creatorcontrib><creatorcontrib>Baumjohann, W</creatorcontrib><creatorcontrib>Bayliss, D</creatorcontrib><creatorcontrib>Benz, W</creatorcontrib><creatorcontrib>Bergomi, M</creatorcontrib><creatorcontrib>Borsato, L</creatorcontrib><creatorcontrib>Broeg, C</creatorcontrib><creatorcontrib>A Collier Cameron</creatorcontrib><creatorcontrib>Csizmadia, Sz</creatorcontrib><creatorcontrib>Cubillos, P E</creatorcontrib><creatorcontrib>Davies, M B</creatorcontrib><creatorcontrib>Deleuil, M</creatorcontrib><creatorcontrib>Deline, A</creatorcontrib><creatorcontrib>Demangeon, O D S</creatorcontrib><creatorcontrib>Demory, B O</creatorcontrib><creatorcontrib>Derekas, A</creatorcontrib><creatorcontrib>Doyle, L</creatorcontrib><creatorcontrib>Edwards, B</creatorcontrib><creatorcontrib>Egger, J A</creatorcontrib><creatorcontrib>Ehrenreich, D</creatorcontrib><creatorcontrib>Erikson, A</creatorcontrib><creatorcontrib>tier, A</creatorcontrib><creatorcontrib>Fossati, L</creatorcontrib><creatorcontrib>Fridlund, M</creatorcontrib><creatorcontrib>Gazeas, K</creatorcontrib><creatorcontrib>Gillon, M</creatorcontrib><creatorcontrib>Güdel, M</creatorcontrib><creatorcontrib>Isaak, K G</creatorcontrib><creatorcontrib>Kiss, L L</creatorcontrib><creatorcontrib>Korth, J</creatorcontrib><creatorcontrib>Lam, K W F</creatorcontrib><creatorcontrib>Laskar, J</creatorcontrib><creatorcontrib>A Lecavelier des Etangs</creatorcontrib><creatorcontrib>Lendl, M</creatorcontrib><creatorcontrib>Magrin, D</creatorcontrib><creatorcontrib>Maxted, P F L</creatorcontrib><creatorcontrib>McCormac, J</creatorcontrib><creatorcontrib>Merín, B</creatorcontrib><creatorcontrib>Mordasini, C</creatorcontrib><creatorcontrib>Nascimbeni, V</creatorcontrib><creatorcontrib>O'Brien, S M</creatorcontrib><creatorcontrib>Olofsson, G</creatorcontrib><creatorcontrib>Ottensamer, R</creatorcontrib><creatorcontrib>Pagano, I</creatorcontrib><creatorcontrib>Pallé, E</creatorcontrib><creatorcontrib>Peter, G</creatorcontrib><creatorcontrib>Piazza, D</creatorcontrib><creatorcontrib>Piotto, G</creatorcontrib><creatorcontrib>Pollacco, D</creatorcontrib><creatorcontrib>Queloz, D</creatorcontrib><creatorcontrib>Ragazzoni, R</creatorcontrib><creatorcontrib>Rando, N</creatorcontrib><creatorcontrib>Rauer, H</creatorcontrib><creatorcontrib>Ribas, I</creatorcontrib><creatorcontrib>Santos, N C</creatorcontrib><creatorcontrib>Scandariato, G</creatorcontrib><creatorcontrib>Ségransan, D</creatorcontrib><creatorcontrib>Simon, A E</creatorcontrib><creatorcontrib>Smith, A M S</creatorcontrib><creatorcontrib>Sousa, S G</creatorcontrib><creatorcontrib>Southworth, R</creatorcontrib><creatorcontrib>Stalport, M</creatorcontrib><creatorcontrib>Steinberger, M</creatorcontrib><creatorcontrib>Sulis, S</creatorcontrib><creatorcontrib>Udry, S</creatorcontrib><creatorcontrib>Ulmer, B</creatorcontrib><creatorcontrib>Ulmer-Moll, S</creatorcontrib><creatorcontrib>V Van Grootel</creatorcontrib><creatorcontrib>Venturini, J</creatorcontrib><creatorcontrib>Villaver, E</creatorcontrib><creatorcontrib>Walton, N A</creatorcontrib><creatorcontrib>Wheatley, P J</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Access via ProQuest (Open Access)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>H Yu</au><au>Garai, Z</au><au>Cretignier, M</au><au>Szabó, Gy M</au><au>Aigrain, S</au><au>Gandolfi, D</au><au>Bryant, E M</au><au>Correia, A C M</au><au>Klein, B</au><au>Brandeker, A</au><au>Owen, J E</au><au>Günther, M N</au><au>Winn, J N</au><au>Heitzmann, A</au><au>Cegla, H M</au><au>Wilson, T G</au><au>Gill, S</au><au>Kriskovics, L</au><au>Barragán, O</au><au>Boldog, A</au><au>Nielsen, L D</au><au>Billot, N</au><au>Lafarga, M</au><au>Meech, A</au><au>Alibert, Y</au><au>Alonso, R</au><au>Bárczy, T</au><au>Barrado, D</au><au>Barros, S C C</au><au>Baumjohann, W</au><au>Bayliss, D</au><au>Benz, W</au><au>Bergomi, M</au><au>Borsato, L</au><au>Broeg, C</au><au>A Collier Cameron</au><au>Csizmadia, Sz</au><au>Cubillos, P E</au><au>Davies, M B</au><au>Deleuil, M</au><au>Deline, A</au><au>Demangeon, O D S</au><au>Demory, B O</au><au>Derekas, A</au><au>Doyle, L</au><au>Edwards, B</au><au>Egger, J A</au><au>Ehrenreich, D</au><au>Erikson, A</au><au>tier, A</au><au>Fossati, L</au><au>Fridlund, M</au><au>Gazeas, K</au><au>Gillon, M</au><au>Güdel, M</au><au>Isaak, K G</au><au>Kiss, L L</au><au>Korth, J</au><au>Lam, K W F</au><au>Laskar, J</au><au>A Lecavelier des Etangs</au><au>Lendl, M</au><au>Magrin, D</au><au>Maxted, P F L</au><au>McCormac, J</au><au>Merín, B</au><au>Mordasini, C</au><au>Nascimbeni, V</au><au>O'Brien, S M</au><au>Olofsson, G</au><au>Ottensamer, R</au><au>Pagano, I</au><au>Pallé, E</au><au>Peter, G</au><au>Piazza, D</au><au>Piotto, G</au><au>Pollacco, D</au><au>Queloz, D</au><au>Ragazzoni, R</au><au>Rando, N</au><au>Rauer, H</au><au>Ribas, I</au><au>Santos, N C</au><au>Scandariato, G</au><au>Ségransan, D</au><au>Simon, A E</au><au>Smith, A M S</au><au>Sousa, S G</au><au>Southworth, R</au><au>Stalport, M</au><au>Steinberger, M</au><au>Sulis, S</au><au>Udry, S</au><au>Ulmer, B</au><au>Ulmer-Moll, S</au><au>V Van Grootel</au><au>Venturini, J</au><au>Villaver, E</au><au>Walton, N A</au><au>Wheatley, P J</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A possible misaligned orbit for the young planet AU Mic c</atitle><jtitle>arXiv.org</jtitle><date>2024-12-20</date><risdate>2024</risdate><eissn>2331-8422</eissn><abstract>The AU Microscopii planetary system is only 24 Myr old, and its geometry may provide clues about the early dynamical history of planetary systems. Here, we present the first measurement of the Rossiter-McLaughlin effect for the warm sub-Neptune AU Mic c, using two transits observed simultaneously with the European Southern Observatory's (ESO's) Very Large Telescope (VLT)/Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO), CHaracterising ExOPlanet Satellite (CHEOPS), and Next-Generation Transit Survey (NGTS). After correcting for flares and for the magnetic activity of the host star, and accounting for transit-timing variations, we find the sky-projected spin-orbit angle of planet c to be in the range \(\lambda_c=67.8_{-49.0}^{+31.7}\)\,degrees (1-\(\sigma\)). We examine the possibility that planet c is misaligned with respect to the orbit of the inner planet b (\(\lambda_b=-2.96_{-10.30}^{+10.44}\)\,degrees), and the equatorial plane of the host star, and discuss scenarios that could explain both this and the planet's high density, including secular interactions with other bodies in the system or a giant impact. We note that a significantly misaligned orbit for planet c is in some degree of tension with the dynamical stability of the system, and with the fact that we see both planets in transit, though these arguments alone do not preclude such an orbit. Further observations would be highly desirable to constrain the spin-orbit angle of planet c more precisely.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2411.16958</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2024-12 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_proquest_journals_3133540117 |
| source | arXiv.org; Free E- Journals |
| subjects | Orbital stability Physics - Earth and Planetary Astrophysics Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics Planetary orbits Planetary systems Systems stability |
| title | A possible misaligned orbit for the young planet AU Mic c |
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