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Titolo:
No planet for HD 166435
Autore:
Queloz, D; Henry, GW; Sivan, JP; Baliunas, SL; Beuzit, JL; Donahue, RA; Mayor, M; Naef, D; Perrier, C; Udry, S;
Indirizzi:
Observ Geneva, CH-1290 Sauverny, Switzerland Observ Geneva Sauverny Switzerland CH-1290 CH-1290 Sauverny, Switzerland Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37203 USA Tennessee State Univ Nashville TN USA 37203 Syst, Nashville, TN 37203 USA Observ Haute Provence, F-04870 St Michel, France Observ Haute Provence StMichel France F-04870 F-04870 St Michel, France Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA Harvard Smithsonian Ctr Astrophys Cambridge MA USA 02138 ge, MA 02138 USA Mt Wilson Observ, Pasadena, CA 91106 USA Mt Wilson Observ Pasadena CA USA91106 son Observ, Pasadena, CA 91106 USA Observ Grenoble, F-38041 Grenoble, France Observ Grenoble Grenoble France F-38041 enoble, F-38041 Grenoble, France
Titolo Testata:
ASTRONOMY & ASTROPHYSICS
fascicolo: 1, volume: 379, anno: 2001,
pagine: 279 - 287
SICI:
1432-0746(200111)379:1<279:NPFH1>2.0.ZU;2-H
Fonte:
ISI
Lingua:
ENG
Soggetto:
MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; LITHIUM ABUNDANCES; ROTATION; SEARCH; EVOLUTION; VELOCITY; PLEIADES; PRAESEPE; CLUSTER;
Keywords:
stars : activity; individual : HD 166435; planetary systems;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
28
Recensione:
Indirizzi per estratti:
Indirizzo: Queloz, D Observ Geneva, 51 Ch Maillettes, CH-1290 Sauverny, Switzerland Observ Geneva 51 Ch Maillettes Sauverny Switzerland CH-1290 and
Citazione:
D. Queloz et al., "No planet for HD 166435", ASTRON ASTR, 379(1), 2001, pp. 279-287

Abstract

The G0 V star HD 166435 has been observed by the fiber-fed spectrograph ELODIE as one of the targets in the large extra-solar planet survey that we are conducting at the Observatory of Haute-Provence. We detected coherent, low-amplitude, radial-velocity variations with a period of 3.7987 days, suggesting a possible close-in planetary companion. Subsequently, we initiated a series of high-precision photometric observations to search for possible planetary transits and an additional series of Ca II H and K observations to measure the level of surface magnetic activity and to look for possible rotational modulation. Surprisingly, we found the star to be photometricallyvariable and magnetically active. A detailed study of the phase stability of the radial-velocity signal revealed that the radial-velocity variabilityremains coherent only for durations of about 30 days. Analysis of the timevariation of the spectroscopic line profiles using line bisectors revealeda correlation between radial velocity and line-bisector orientation. All of these observations, along with a one-quarter cycle phase shift between the photometric and the radial-velocity variations, are well explained by thepresence of dark photospheric spots on HD 166435. We conclude that the radial-velocity variations are not due to gravitational interaction with an orbiting planet but, instead, originate from line-profile changes stemming from star spots on the surface of the star. The quasi-coherence of the radial-velocity signal over more than two years, which allowed a fair fit with a binary model, makes the stability of this star unusual among other active stars. It suggests a stable magnetic field orientation where spots are always generated at about the same location on the surface of the star.

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Documento generato il 11/07/20 alle ore 07:15:54