A Redetermination of the Mass of Procyon

Girard, Terrence M.; Wu, H. R.; Lee, J. T.; Dyson, Samuel E.; Altena, W. F. van; Horch, Elliott; Gilliland, Ronald L.; Schaefer, K. G.; Bond, Howard E.; Ftaclas, C.; Brown, R. H.; Toomey, Douglas W.; Shipman, H. L.; Provencal, J. L.; Pourbaix, Dimitri

doi:10.1086/301353

Cited by 63 publications

(88 citation statements)

References 14 publications

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“…The derived gravity is in good agreement with the estimate of Allende Prieto & Lambert (1999), log g = 4.04 ± 0.14 dex, obtained from matching the observed M V and (B − V ) to the evolutionary models of Bertelli et al (1994) 5 . Our mass estimate is slightly lower from that given in Girard et al (2000), as we prefer to adopt the Hipparcos parallax and the angular separation determined from HST-WFPC2 observations, discarding the ground-based measurement. Adopting the parallax derived by Girard et al, p = (283.2 ± 1.5) × 10 −3 arcsec, we find only a minor correction to the derived mass:…”

Section: Fundamental Stellar Parametersmentioning

confidence: 68%

“…where α, α A , and P are the semi-major axis of the visual orbit or Procyon A, the semi-major axis of its orbit relative to the barycenter of the system, and the orbital period, respectively, and for which we have adopted α = 4.271 ± 0.032 arcsec, α A = 1.232 ± 0.08 arcsec, and P = 40.82 ± 0.06 yr. (Girard et al 2000), in combination with Hipparcos's parallax. The radius is…”

Section: Fundamental Stellar Parametersmentioning

confidence: 99%

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Signatures of Convection in the Spectrum of Procyon: Fundamental Parameters and Iron Abundance

Prieto

Asplund²,

López

et al. 2002

ApJ

170

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We have observed the spectrum of Procyon A (F5IV) from 4559 to 5780Å with a S/N of ∼ 10 3 and a resolving power of 2 × 10 5 . We have measured the line bisectors and relative line shifts of a large number of Fe I and Fe II lines, comparing them to those found in the Sun. A three-dimensional (3D) hydrodynamical model atmosphere has been computed and is tested against observations. The model reproduces in detail most of the features observed, although we identify some room for improvement. At all levels, the comparison of the 3D time-dependent calculations with the observed spectral lines shows a much better agreement than for classical homogeneous models, making it possible to refine previous estimates of the iron abundance, the projected rotational velocity, the limb-darkening, and the systemic velocity of the Procyon binary system. The difference between the iron abundance determined with the 3D model and its 1D counterpart is ∼ < 0.05 dex. We find consistency between the iron abundance derived from Fe I and Fe II lines, suggesting that departures from LTE in the formation of the studied lines are relatively small. The scatter in the iron abundance determined from different lines still exceeds the expectations from the uncertainties in the atomic data, pointing out that one or more components in the modeling can be refined further.

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Section: Fundamental Stellar Parametersmentioning

confidence: 68%

Section: Fundamental Stellar Parametersmentioning

confidence: 99%

Signatures of Convection in the Spectrum of Procyon: Fundamental Parameters and Iron Abundance

Prieto

Asplund²,

López

et al. 2002

ApJ

170

View full text Add to dashboard Cite

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“…They disagreed on the derived mass. Eggenberger et al found a mass that agrees well with the astrometric value derived by Girard et al (2000), whereas Provost et al found a mass that corresponds to the more recent value of Gatewood & Han (2006). Part of the reason for the difference in the two stellar evolution models comes from the slightly different large separation (which increases with the mass), and is partly due to the difference in the stellar evolution codes themselves.…”

Section: Introductionmentioning

confidence: 82%

Three-dimensional interferometric, spectrometric, and planetary views of Procyon

Chiavassa

Bigot

Kervella

et al. 2012

A&A

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Context. Procyon is one of the brightest stars in the sky and one of our nearest neighbours. It is therefore an ideal benchmark object for stellar astrophysics studies using interferometric, spectroscopic, and asteroseismic techniques. Aims. We use a new realistic three-dimensional (3D) radiative-hydrodynamical (RHD) model atmosphere of Procyon generated with the Stagger Code and synthetic spectra computed with the radiative transfer code Optim3D to re-analyze interferometric and spectroscopic data from the optical to the infrared. We provide synthetic interferometric observables that can be validated using observations. Methods. We computed intensity maps from a RHD simulation in two optical filters centered on 500 and 800 nm (Mark III) and one infrared filter centered on 2.2 μm (Vinci). We constructed stellar disk images accounting for the center-to-limb variations and used them to derive visibility amplitudes and closure phases. We also computed the spatially and temporally averaged synthetic spectrum from the ultraviolet to the infrared. We compare these observables to Procyon data. Results. We study the impact of the granulation pattern on center-to-limb intensity profiles and provide limb-darkening coefficients in the optical as well as in the infrared. We show how the convection-related surface structures affect the visibility curves and closure phases with clear deviations from circular symmetry, from the 3rd lobe on. These deviations are detectable with current interferometers using closure phases. We derive new angular diameters at different wavelengths with two independent methods based on 3D simulations. We find that θ Vinci = 5.390 ± 0.03 mas, which we confirm by comparison with an independent asteroseismic estimation (θ seismic = 5.360 ± 0.07 mas. The resulting T eff is 6591 K (or 6556 K depending on the bolometric flux used), which is consistent with the value of T eff,IR = 6621 K found with the infrared flux method. We measure a surface gravity log g = 4.01 ± 0.03 [cm/s 2 ] that is higher by 0.05 dex than literature values. Spectrophotometric comparisons with observations provide very good agreement with the spectral energy distribution and photometric colors, allowing us to conclude that the thermal gradient in the simulation matches Procyon fairly well. Finally, we show that the granulation pattern of a planet-hosting Procyon-like star has a non-negligible impact on the detection of hot Jupiters in the infrared using interferometry closure phases. It is then crucial to have a comprehensive knowledge of the host star to directly detect and characterize hot Jupiters. In this respect, RHD simulations are very important to achieving this aim.

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“…The proper motions of known pairs in the HIP are reduced to the photocentre, barycentre or components separately, depending on the results of the mission. In Table 2 the barycentric proper motion taken or calculated from the HIP is marked as m whereas the photocentric one is marked as p. The Hipparcos proper motion of Procyon was recalculated by Girard et al (2000) in a combination of Hipparcos and ground-based data.…”

Section: Comparison With Known Orbitsmentioning

confidence: 99%

“…Photocentric orbits by Strand (1951), Irwin et al (1992) and Girard et al (2000) are shown in Fig. 2 as dashed, • 3 104.…”

Section: α CMI (Procyon)mentioning

confidence: 99%

Photocentric orbits from a direct combination of ground-based astrometry with Hipparcos

Gontcharov

Kiyaeva

2002

A&A

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Abstract. Complementing the Proper Motions of Fundamental Stars catalogue by Gontcharov et al. (CDS,) the photocentric orbits of some FK5/Hipparcos stars are calculated in a direct combination of the Hipparcos data with astrometric ground-based observational catalogues having epochs later than 1939. Some capabilities and limitations of this method are discussed in a comparison of our results with known orbits of Sirius, Procyon, Rasalhague, µ Cas and others. We conclude that this direct combination is an acceptable tool to discover and investigate photocentric orbits with periods from 10 to 55 years and the semi-major axis of apparent ellipses >0.08 arcsec. It is particularly suitable for pairs with large magnitude difference as well as for calculation of the preliminary orbits of new astrometric binaries which will be considered in forthcoming papers. In this paper new photocentric orbits and component masses are calculated for 4 pairs: α UMa, β LMi, δ And and ξ Aqr.

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A Redetermination of the Mass of Procyon

Cited by 63 publications

References 14 publications

Signatures of Convection in the Spectrum of Procyon: Fundamental Parameters and Iron Abundance

Signatures of Convection in the Spectrum of Procyon: Fundamental Parameters and Iron Abundance

Three-dimensional interferometric, spectrometric, and planetary views of Procyon

Photocentric orbits from a direct combination of ground-based astrometry with Hipparcos

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