A Planet Orbiting the Star ρ Coronae Borealis

Noyes, R. W.; Korzennik, S. G.; Krockenberger, M.; Nisenson, P.; Brown, Timothy M.; Kennelly, E. J.; Horner, Scott D.

doi:10.1086/310754

Cited by 160 publications

(93 citation statements)

References 33 publications

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“…Therefore, assuming the rate of binary systems found above, we obtained 0.05 SB looking like exoplanet candidates among 102 bright G-type stars. In reality, candidate planets were found around 8 stars: GJ 61=υ And , GJ 324 = 55 Cnc , GJ 407 = 47 UMa (Butler & Marcy 1996), GJ 527A = τ Bootis ), GJ 606.2 = ρ CrB (Noyes et al 1997), GJ 765.1B = 16 Cyg B (Cochran et al 1997), GJ 848.4 = HD 210277 (Marcy et al 1999), and GJ 882 = 51 Peg (Mayor & Queloz 1995). The astrometric wobble of ρ CrB looks too large for a planetary component, and the system could be a pole-on binary Pourbaix & Arenou 2001), although Zucker & Mazeh (2001) pointed out that the significance of this wobble is not really convincing when the number of planet candidates which were examined is taken into account.…”

Section: False Alarms and True Exoplanetsmentioning

confidence: 99%

Multiplicity among solar–type stars

Halbwachs

Mayor²,

Udry³

et al. 2002

A&A

323

431

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Abstract. Two CORAVEL radial velocity surveys -one among stars in the solar neighbourhood, the other in the Pleiades and in Praesepe -are merged to derive the statistical properties of main-sequence binaries with spectral types F7 to K and with periods up to 10 years. A sample of 89 spectroscopic orbits was finally obtained. Among them, 52 relate to a free-of-bias selection of 405 stars (240 field stars and 165 cluster stars). The statistics corrected for selection effects yield the following results: (1) No discrepancy is found between the binaries among field stars and the binaries in open cluster. The distributions of mass ratios, of periods, the period-eccentricity diagram and the binary frequencies are all within the same error intervals. (2) The distribution of mass ratios presents two maxima: a broad peak from q ≈ 0.2 to q ≈ 0.7, and a sharp peak for q > 0.8 (twins). Both are present among the early-type as well as among the late-type part of the sample, indicating a scale-free formation process. The peak for q > 0.8 gradually decreases when long-period binaries are considered. Whatever their periods, the twins have eccentricities significantly lower than the other binaries, confirming a difference in the formation processes. Twins could be generated by in situ formation followed by accretion from a gaseous envelope, whereas binaries with intermediate mass ratios could be formed at wide separations, but they are made closer by migration led by interactions with a circumbinary disk. (3) The frequency of binaries with P < 10 years is about 14%. (4) About 0.3% of binaries are expected to appear as false positives in a planet search. Therefore, the frequency of planetary systems among stars is presently 7 +4 −2 %. The extension of the distribution of mass ratios in the planetary range would result in a very sharp and very high peak, well separated from the binary stars with low mass ratios.

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Section: False Alarms and True Exoplanetsmentioning

confidence: 99%

Multiplicity among solar–type stars

Halbwachs

Mayor²,

Udry³

et al. 2002

A&A

323

431

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show abstract

“…The standard technique used to detect such planets is to look for periodic Doppler shifts in the spectrum of the central star of the extrasolar planetary system (Mayor & Queloz 1995;Noyes et al 1997;. This technique, however, only returns M p sin i p , where M p is the mass of the orbiting body and i p is the inclination of the normal to its orbital plane relative to the line of sight.…”

Section: Introductionmentioning

confidence: 99%

Determining the Inclination of the Rotation Axis of a Sun‐like Star

Gizon

Solanki

2003

ApJ

280

329

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Asteroseismology provides us with the possibility of determining the angle, i, between the direction of the rotation axis of a pulsating Sun-like star and the line of sight. A knowledge of i is important not just for obtaining improved stellar parameters, but also in order to determine the true masses of extrasolar planets detected from the radial velocity shifts of their central stars. By means of Monte Carlo simulations, we estimate the precision of the measurement of i and other stellar parameters. We find that the inclination angle can be retrieved accurately when ie30 for stars that rotate at least twice as fast as the Sun.

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“…The current Doppler technique requires a highresolution grating spectrometer (e.g., Vogt et al 1994;Mayor & Queloz 1995;Butler et al 1996;Noyes et al 1997;Cochran et al 1997;Vogt et al 2000). The minimum typical line width of absorption-line features in stellar and solar spectra at 5000-6000 Å is ∼0.1 Å , about 5-6 km s Ϫ1 in equivalent Doppler velocity.…”

Section: Introductionmentioning

confidence: 99%

An Externally Dispersed Interferometer Prototype for Sensitive Radial Velocimetry: Theory and Demonstration on Sunlight

Erskine

2003

PUBL ASTRON SOC PAC

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ABSTRACT.A theory of operation of a wideband interferometric Doppler spectroscopy technique, called externally dispersed interferometry (EDI), is presented. The first EDI prototype was tested on sunlight and detected the 12 m s Ϫ1 amplitude lunar signature in Earth's motion. The hybrid instrument is an undispersed Michelson interferometer having a fixed delay of about 1 cm, in series with an external spectrograph of about 20,000 resolution. The Michelson provides the Doppler shift discrimination, while the external spectrograph boosts net white-light fringe visibility by reducing cross talk from adjacent continuum channels. A moiré effect between the sinusoidal interferometer transmission and the input spectrum heterodynes high spectral details to broad moiré patterns, which carry the Doppler information in its phase. These broad patterns survive the blurring of the spectrograph, which can have several times lower resolution than grating-only spectrographs typically used now for the Doppler planet search. This enables the net instrument to be dramatically smaller in size (∼1 m) and cost. The EDI behavior is compared and contrasted to the conventional grating-only technique.

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A Planet Orbiting the Star ρ Coronae Borealis

Cited by 160 publications

References 33 publications

Multiplicity among solar–type stars

Multiplicity among solar–type stars

Determining the Inclination of the Rotation Axis of a Sun‐like Star

An Externally Dispersed Interferometer Prototype for Sensitive Radial Velocimetry: Theory and Demonstration on Sunlight

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