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The changing face of AU Mic b : stellar spots, spin-orbit commensurability, and transit timing variations as seen by CHEOPS and TESS
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dc.contributor.author | Szabo, Gy M | |
dc.contributor.author | Gandolfi, D | |
dc.contributor.author | Brandeker, A | |
dc.contributor.author | Csizmadia, S | |
dc.contributor.author | Garai, Z | |
dc.contributor.author | Billot, N | |
dc.contributor.author | Broeg, C | |
dc.contributor.author | Ehrenreich, D | |
dc.contributor.author | Fortier, A | |
dc.contributor.author | Fossati, L | |
dc.contributor.author | Hoyer, S | |
dc.contributor.author | Kiss, L | |
dc.contributor.author | Lecavelier des Etangs, A | |
dc.contributor.author | Maxted, PFL | |
dc.contributor.author | Ribas, I | |
dc.contributor.author | Alibert, Y | |
dc.contributor.author | Alonso, R | |
dc.contributor.author | Escude, GA | |
dc.contributor.author | Barczy, T | |
dc.contributor.author | Barros, SCC | |
dc.contributor.author | Barrado, D | |
dc.contributor.author | Baumjohann, W | |
dc.contributor.author | Beck, M | |
dc.contributor.author | Beck, T | |
dc.contributor.author | Bekkelien, A | |
dc.contributor.author | Bonfils, X | |
dc.contributor.author | Benz, W | |
dc.contributor.author | Borsato, L | |
dc.contributor.author | Busch, MD | |
dc.contributor.author | Cabrera, J | |
dc.contributor.author | Charnoz, S | |
dc.contributor.author | Cameron, AC | |
dc.contributor.author | Van Damme, CC | |
dc.contributor.author | Davies, MB | |
dc.contributor.author | Delrez, L | |
dc.contributor.author | Deleuil, M | |
dc.contributor.author | Demangeon, ODS | |
dc.contributor.author | Demory, BO | |
dc.contributor.author | Erikson, A | |
dc.contributor.author | Fridlund, M | |
dc.contributor.author | Futyan, D | |
dc.contributor.author | Muñoz, A García | |
dc.contributor.author | Gillon, M | |
dc.contributor.author | Guedel, M | |
dc.contributor.author | Guterman, P | |
dc.contributor.author | Heng, K | |
dc.contributor.author | Isaak, KG | |
dc.contributor.author | Lacedelli, G | |
dc.contributor.author | Laskar, J | |
dc.contributor.author | Lendl, M | |
dc.contributor.author | Lovis, C | |
dc.contributor.author | Luntzer, A | |
dc.contributor.author | Magrin, D | |
dc.contributor.author | Nascimbeni, V | |
dc.contributor.author | Olofsson, G | |
dc.contributor.author | Osborn, HP | |
dc.contributor.author | Ottensamer, R | |
dc.contributor.author | Pagano, I | |
dc.contributor.author | Palle, E | |
dc.contributor.author | Peter, G | |
dc.contributor.author | Piazza, D | |
dc.contributor.author | Piotto, G | |
dc.contributor.author | Pollacco, D | |
dc.contributor.author | Queloz, D | |
dc.contributor.author | Ragazzoni, R | |
dc.contributor.author | Rando, N | |
dc.contributor.author | Rauer, H | |
dc.contributor.author | Santos, NC | |
dc.contributor.author | Scandariato, G | |
dc.contributor.author | Segransan, D | |
dc.contributor.author | Serrano, LM | |
dc.contributor.author | Sicilia, D | |
dc.contributor.author | Simon, AE | |
dc.contributor.author | Smith, AMS | |
dc.contributor.author | Sousa, SG | |
dc.contributor.author | Steller, M | |
dc.contributor.author | Thomas, N | |
dc.contributor.author | Udry, S | |
dc.contributor.author | Van Grootel, V | |
dc.contributor.author | Walton, NA | |
dc.contributor.author | Wilson, TG | |
dc.date.accessioned | 2021-11-12T15:30:02Z | |
dc.date.available | 2021-11-12T15:30:02Z | |
dc.date.issued | 2021-10 | |
dc.identifier | 276677716 | |
dc.identifier | 7aa91fc0-8cc8-42cf-aa68-d4db19fd2077 | |
dc.identifier | 000711136600002 | |
dc.identifier | 85118444840 | |
dc.identifier.citation | Szabo , G M , Gandolfi , D , Brandeker , A , Csizmadia , S , Garai , Z , Billot , N , Broeg , C , Ehrenreich , D , Fortier , A , Fossati , L , Hoyer , S , Kiss , L , Lecavelier des Etangs , A , Maxted , PFL , Ribas , I , Alibert , Y , Alonso , R , Escude , GA , Barczy , T , Barros , SCC , Barrado , D , Baumjohann , W , Beck , M , Beck , T , Bekkelien , A , Bonfils , X , Benz , W , Borsato , L , Busch , MD , Cabrera , J , Charnoz , S , Cameron , AC , Van Damme , CC , Davies , MB , Delrez , L , Deleuil , M , Demangeon , ODS , Demory , BO , Erikson , A , Fridlund , M , Futyan , D , Muñoz , A G , Gillon , M , Guedel , M , Guterman , P , Heng , K , Isaak , KG , Lacedelli , G , Laskar , J , Lendl , M , Lovis , C , Luntzer , A , Magrin , D , Nascimbeni , V , Olofsson , G , Osborn , HP , Ottensamer , R , Pagano , I , Palle , E , Peter , G , Piazza , D , Piotto , G , Pollacco , D , Queloz , D , Ragazzoni , R , Rando , N , Rauer , H , Santos , NC , Scandariato , G , Segransan , D , Serrano , LM , Sicilia , D , Simon , AE , Smith , AMS , Sousa , SG , Steller , M , Thomas , N , Udry , S , Van Grootel , V , Walton , NA & Wilson , TG 2021 , ' The changing face of AU Mic b : stellar spots, spin-orbit commensurability, and transit timing variations as seen by CHEOPS and TESS ' , Astronomy & Astrophysics , vol. 654 , A159 . https://doi.org/10.1051/0004-6361/202140345 | en |
dc.identifier.issn | 0004-6361 | |
dc.identifier.other | RIS: urn:503052C3FB4955E5825C413417C90636 | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/103137349 | |
dc.identifier.other | ORCID: /0000-0001-8749-1962/work/103138164 | |
dc.identifier.uri | https://hdl.handle.net/10023/24330 | |
dc.description | A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/M001296/1. | en |
dc.description.abstract | AU Mic is a young planetary system with a resolved debris disc showing signs of planet formation and two transiting warm Neptunes near mean-motion resonances. Here we analyse three transits of AU Mic b observed with the CHaracterising ExOPlanet Satellite (CHEOPS), supplemented with sector 1 and 27 Transiting Exoplanet Survey Satellite (TESS) photometry, and the All-Sky Automated Survey from the ground. The refined orbital period of AU Mic b is 8.462995 ± 0.000003 d, whereas the stellar rotational period is P-rot = 4.8367 ± 0.0006 d. The two periods indicate a 7:4 spin-orbit commensurability at a precision of 0.1%. Therefore, all transits are observed in front of one of the four possible stellar central longitudes. This is strongly supported by the observation that the same complex star-spot pattern is seen in the second and third CHEOPS visits that were separated by four orbits (and seven stellar rotations). Using a bootstrap analysis we find that flares and star spots reduce the accuracy of transit parameters by up to 10% in the planet-to-star radius ratio and the accuracy on transit time by 3-4 min. Nevertheless, occulted stellar spot features independently confirm the presence of transit timing variations (TTVs) with an amplitude of at least 4 min. We find that the outer companion, AU Mic c, may cause the observed TTVs. | |
dc.format.extent | 15 | |
dc.format.extent | 7326484 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomy & Astrophysics | en |
dc.subject | Planetary systems | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | The changing face of AU Mic b : stellar spots, spin-orbit commensurability, and transit timing variations as seen by CHEOPS and TESS | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | 10.1051/0004-6361/202140345 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | https://arxiv.org/abs/2108.02149 | en |
dc.identifier.grantnumber | ST/R00824/1 | en |
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