The DOI matches its Crossref record; 6 of the 7 references it cites were found in a registry or an index.
No planet for HD 166435
Open accessAbstract
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 photometrically variable and magnetically active. A detailed study of the phase stability of the radial-velocity signal revealed that the radial-velocity variability remains coherent only for durations of about 30 days. Analysis of the time variation of the spectroscopic line profiles using line bisectors revealed a 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 the presence 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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“Other parameters such as the span of the bisector slope and the full width at half-maximum (FWHM) of the cross-correlation function were measured as well. They provide good diagnostics for stellar activity (e.g. Queloz et al. 2001; Huélamo et al. 2008).”
From Mass and period limits on the ringed companion transiting the young star J1407 (2015) · cites this paper as Queloz et al. 2001
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Cites
A Jupiter-mass companion to a solar-type star
Mayor, M., & Queloz, D. (1995) · Nature · doi:10.1038/378355a0 · Cited by 4,111
Self-citationMannings, V., Boss, A., & Russell, S. (2000) · Icarus · doi:10.1006/icar.1999.6299 · Cited by 3,354 · cited 2×
“…we began a campaign of highprecision photometric observations with an automatic photoelectric telescope (APT) at Fairborn Observatory in Arizona to search for planetary transits and made tentative plans to announce the new planet at the Protostars and Planets IV conference (Mannings et al. 2000).”
BackgroundMethodEhlers, J., Hepp, K., Kippenhahn, M. R., WeidenmiJller, H. A., Zittartz, J., & Droz, M. (2001) · doi:10.1016/0030-3992(80)90094-8 · Cited by 2,242 · cited 1×
“This phenomena is observed on the Sun to a lesser degree where leader spots tend to be larger and to live longer than follower spots, resulting in a displacement up to 5 0 between the photocenters of the spot and the associated plages (Dobson-Hockey & Radick 1986).”
BackgroundCool Stars, Stellar Systems, and the Sun
Baliunas, S. L., & Hartmann, L. W. (1984) · Lecture notes in physics · doi:10.1007/3-540-12907-3 · Cited by 524 · cited 1×
“From 1998 June to 1998 August, 141 Ca II H and K measurements were made on 20 nights with the 100-inch telescope at Mount Wilson Observatory as part of the HK Project (Baliunas et al. 1998).”
MethodSelf-citationNew Developments in Array Technology and Applications
Philip, A. G. D., Janes, K. A., & Upgren, A. R. (1995) · Springer eBooks · doi:10.1007/978-94-011-0383-1 · Cited by 47 · cited 5×
“In addition to the stellar radial velocity, the cross-correlation function (CCF) provides additional information about features in the averaged spectral lines (see Queloz 1994 for a review).”
BackgroundMethodInfluentialStrach, E. (1996) · doi:10.1007/978-1-4471-0999-0_24 · Cited by 1
Research works printed but not linked: 2
- Mannings, V., Boss, A. P., & Russell, S. S. 2000, Protostars and Planets IV (Tucson: University of Arizona Press)
- Queloz, D., Mayor, M., Sivan, et al. 1998, in 'Brown Dwrafs and Extrasolar Planets', ASP Conf. Ser., vol. 134 , ed. R. Rebolo, E. L. Martin, M. R. Zapatero Osorio, 324.
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A terrestrial planet candidate in a temperate orbit around Proxima Centauri
Anglada-Escudé, G., Amado, P. J., Barnes, J. R., Berdiñas, Z. M., Butler, R. P., Coleman, G. A. L., de la Cueva, I., Dreizler, S., Endl, M., Giesers, B., et al. (2016) · Nature · doi:10.1038/nature19106 · Cited by 1,293
The stellar-activity-rotation relationship and the evolution of stellar dynamos
Wright, N. J., Drake, J. J., Mamajek, E. E., & Henry, G. W. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/743/1/48 · Cited by 882
Self-citationButler, R. P., Wright, J. T., Marcy, G. W., Fischer, D. A., Vogt, S. S., Tinney, C. G., Jones, H. R. A., Carter, B. D., Johnson, J. A., McCarthy, C., et al. (2006) · The Astrophysical Journal · doi:10.1086/504701 · Cited by 914
“…stars are bright enough to permit precise photometric and chromospheric monitoring by telescopes of modest size, permitting careful assessment of velocity jitter, starspots, and possible transits, e.g., Henry (1999); Henry et al. (2000); Queloz et al. (2001); Eaton, Henry, & Fekel (2003).”
BackgroundThe HARPS search for southern extra-solar planets: XXXI. The M-dwarf sample
Bonfils, X., Delfosse, X., Udry, S., Forveille, T., Mayor, M., Perrier, C., Bouchy, F., Gillon, M., Lovis, C., Pepe, F., et al. (2013) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201014704 · Cited by 653
“While its barycenter measures the radial-velocity, its bisector inverse slope (BIS – Queloz et al. 2001) and its full width half maximum (FWHM) can diagnose inhomogeneities of the stellar surface.”
BackgroundMethodSelf-citationKEPLER'S FIRST ROCKY PLANET: KEPLER-10b
Batalha, N. M., Borucki, W. J., Bryson, S. T., Buchhave, L. A., Caldwell, D. A., Christensen-Dalsgaard, J., Ciardi, D., Dunham, E. W., Fressin, F., Gautier, T. N., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/729/1/27 · Cited by 531
“When RV variations are the result of a blended spectrum between a star and an eclipsing binary, we expect the bisectors to reveal a phasemodulated line asymmetry (Queloz et al. 2001; Mandushev et al. 2005).”
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Metadata
- Authors
- Queloz, D., Henry, G. W., Sivan, J. P., Baliunas, S. L., Beuzit, J. L., Donahue, R. A., Mayor, M., Naef, D., Perrier, C., & Udry, S.
- Affiliations
- University of Geneva (CH)
- Tennessee State University (US)
- Observatoire de Haute-Provence (FR)
- Center for Astrophysics Harvard & Smithsonian (US)
- Venue
- Astronomy and Astrophysics
- Publisher
- EDP Sciences
- Published
- 2001-11
- Volume
- 379
- Issue
- 1
- Pages
- 279-287
- ISSN
- 0004-6361 (ISSN-L)
- 1432-0756
- OpenAlex
- W2116181668
- Cited by
- 913
- References
- 7
- Citations by year
- 2026: 15 · 2025: 42 · 2024: 47 · 2023: 34 · 2022: 43 · 2021: 46 · 2020: 50 · 2019: 51 · 2018: 49 · 2017: 39 · 2016: 62 · 2015: 37 · 2014: 40 · 2013: 34 · 2012: 48
- FWCI
- 7.54
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (9706268)
- Smithsonian Institution
- National Aeronautics and Space Administration (HRD-9706268, NCC596)
- Carnegie Institution of Washington
- Richard Lounsbery Foundation
- Fonds De La Recherche Scientifique - FNRS
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › History and Developments in Astronomy
- Keywords
- radial velocity variations, stellar activity, stellar spots, line bisectors, photometric variability, stellar magnetic activity, Ca II H and K lines, phase stability, binary star models
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