{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,1,6]],"date-time":"2026-01-06T13:05:45Z","timestamp":1767704745223},"reference-count":11,"publisher":"Cambridge University Press (CUP)","issue":"S273","license":[{"start":{"date-parts":[[2011,8,26]],"date-time":"2011-08-26T00:00:00Z","timestamp":1314316800000},"content-version":"unspecified","delay-in-days":390,"URL":"https:\/\/www.cambridge.org\/core\/terms"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Proc. IAU"],"published-print":{"date-parts":[[2010,8]]},"abstract":"<jats:title>Abstract<\/jats:title><jats:p>Photospheric stellar activity (i.e. dark spots or bright plages) might be an important source of noise and confusion in the radial-velocity (RV) measurements. Radial-velocimetry planet search surveys as well as follow-up of photometric transit surveys require a deeper understanding and characterization of the effects of stellar activities to disentangle it from planetary signals.<\/jats:p><jats:p>We simulate dark spots on a rotating stellar photosphere. The variations of the RV are characterized and analyzed according to the stellar inclination, the latitude and the number of spots. The Lomb-Scargle periodograms of the RV variations induced by activity present power at the rotational period <jats:italic>P<\/jats:italic><jats:sub><jats:italic>rot<\/jats:italic><\/jats:sub> of the star and its two-first harmonics <jats:italic>P<\/jats:italic><jats:sub><jats:italic>rot<\/jats:italic><\/jats:sub>\/2 and <jats:italic>P<\/jats:italic><jats:sub><jats:italic>rot<\/jats:italic><\/jats:sub>\/3. Three adjusted sinusoids fixed at the fundamental period and its two-first harmonics allow to remove about 90% of the RV jitter amplitude. We apply and validate our approach on four known active planet-host stars: HD 189733, GJ 674, CoRoT-7 and \u03b9 Hor. We succeed in fitting simultaneously activity and planetary signals on GJ674 and CoRoT-7. We excluded short-period low-mass exoplanets around \u03b9 Hor. Our approach is efficient to disentangle reflex-motion due to a planetary companion and stellar-activity induced-RV variations provided that 1) the planetary orbital period is not close to that of the stellar rotation or one of its two-first harmonics, 2) the rotational period of the star is accurately known, 3) the data cover more than one stellar rotational period.<\/jats:p>","DOI":"10.1017\/s1743921311015389","type":"journal-article","created":{"date-parts":[[2011,8,26]],"date-time":"2011-08-26T14:15:55Z","timestamp":1314368155000},"page":"281-285","source":"Crossref","is-referenced-by-count":4,"title":["Disentangling between stellar activity and planetary signals"],"prefix":"10.1017","volume":"6","author":[{"given":"Isabelle","family":"Boisse","sequence":"first","affiliation":[]},{"given":"Fran\u00e7ois","family":"Bouchy","sequence":"additional","affiliation":[]},{"given":"Guillaume","family":"H\u00e9brard","sequence":"additional","affiliation":[]},{"given":"Xavier","family":"Bonfils","sequence":"additional","affiliation":[]},{"given":"Nuno","family":"Santos","sequence":"additional","affiliation":[]},{"given":"Sylvie","family":"Vauclair","sequence":"additional","affiliation":[]}],"member":"56","published-online":{"date-parts":[[2011,8,26]]},"reference":[{"key":"S1743921311015389_ref10","doi-asserted-by":"publisher","DOI":"10.1086\/304392"},{"key":"S1743921311015389_ref7","first-page":"287","volume":"506","author":"L\u00e9ger","year":"2009","journal-title":"AandA"},{"key":"S1743921311015389_ref2","first-page":"293","volume":"474","author":"Bonfils","year":"2007","journal-title":"AandA"},{"key":"S1743921311015389_ref1","first-page":"959","volume":"495","author":"Boisse","year":"2009","journal-title":"AandA"},{"key":"S1743921311015389_ref4","first-page":"259","volume":"185","author":"Hatzes","year":"1999","journal-title":"ASPC"},{"key":"S1743921311015389_ref5","first-page":"L9","volume":"489","author":"Hu\u00e9lamo","year":"2008","journal-title":"AandA"},{"key":"S1743921311015389_ref9","first-page":"303","volume":"506","author":"Queloz","year":"2009","journal-title":"AandA"},{"key":"S1743921311015389_ref8","first-page":"279","volume":"379","author":"Queloz","year":"2001","journal-title":"AandA"},{"key":"S1743921311015389_ref3","first-page":"983","volume":"473","author":"Desort","year":"2007","journal-title":"AandA"},{"key":"S1743921311015389_ref11","first-page":"5","volume":"428","author":"Vauclair","year":"2008","journal-title":"AandA"},{"key":"S1743921311015389_ref6","first-page":"33","volume":"353","author":"K\u00fcrster","year":"2000","journal-title":"AandA"}],"container-title":["Proceedings of the International Astronomical Union"],"original-title":[],"language":"en","link":[{"URL":"https:\/\/www.cambridge.org\/core\/services\/aop-cambridge-core\/content\/view\/S1743921311015389","content-type":"unspecified","content-version":"vor","intended-application":"similarity-checking"}],"deposited":{"date-parts":[[2019,4,28]],"date-time":"2019-04-28T19:17:14Z","timestamp":1556479034000},"score":1,"resource":{"primary":{"URL":"https:\/\/www.cambridge.org\/core\/product\/identifier\/S1743921311015389\/type\/journal_article"}},"subtitle":[],"short-title":[],"issued":{"date-parts":[[2010,8]]},"references-count":11,"journal-issue":{"issue":"S273","published-print":{"date-parts":[[2010,8]]}},"alternative-id":["S1743921311015389"],"URL":"https:\/\/doi.org\/10.1017\/s1743921311015389","relation":{},"ISSN":["1743-9213","1743-9221"],"issn-type":[{"value":"1743-9213","type":"print"},{"value":"1743-9221","type":"electronic"}],"subject":[],"published":{"date-parts":[[2010,8]]}}}