Accurate fundamental parameters for 23 bright solar-type stars
By H. Bruntt, T. Bedding, P. Quirion, G. Curto, F. Carrier, B. Smalley, T. Dall, T. Arentoft, M. Bazot, R. P. Butler. 2010
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We combine results from interferometry, asteroseismology and spectroscopy to determine accurate fundamental parameters of 23 bright solar-type stars, from spectral type F5 to K2 and luminosity classes III–V. For some stars we can use direct techniques to determine the mass, radius, luminosity and effective temperature, and we compare with indirect methods that rely on photometric calibrations or spectroscopic analyses. We use the asteroseismic information available in the literature to infer an indirect mass with an accuracy of 4–15 per cent. From indirect methods we determine luminosity and radius to 3 per cent. We find evidence that the luminosity from the indirect method is slightly overestimated (≈5 per cent) for the coolest stars, indicating that their bolometric corrections (BCs) are too negative. For Teff we find a slight offset of −40 ± 20 K between the spectroscopic method and the direct method, meaning the spectroscopic temperatures are too high. From the spectroscopic analysis we determine the detailed chemical composition for 13 elements, including Li, C and O. The metallicity ranges from [Fe/H] =− 1. 7t o+0.4, and there is clear evidence for α-element enhancement in the metal-poor stars. We find no significant offset between the spectroscopic surface gravity and the value from combining asteroseismology with radius estimates. From the spectroscopy we also determine v sin i and we present a new calibration of macroturbulence and microturbulence. From the comparison between the results from the direct and spectroscopic methods we claim that we can determine Teff ,l ogg and [Fe/H] with absolute accuracies of 80 K, 0.08 and 0.07 dex. Photometric calibrations of Str¨ omgren indices provide accurate results for Teff and [Fe/H] but will be more uncertain for distant stars when interstellar reddening becomes important. The indirect methods are important to obtain reliable estimates of the fundamental parameters of relatively faint stars when interferometry cannot be used. This paper is the first to compare direct and indirect methods for a large sample of stars, and we conclude that indirect methods are valid, although slight corrections may be needed.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/7aeb17f394d94a50060c4b521211377606e87406
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Citations in the corpus
- A non-LTE study of neutral and singly-ionized iron line spectra in 1D models of the Sun and selected late-type stars ? (2011, methodology): “Our adopted stellar parameters of these three stars (Table 3) were taken from different studies, but they turned out to be consistent within 1σ with the data of Bruntt et al. (2010).”
- THE K2 ECLIPTIC PLANE INPUT CATALOG (EPIC) AND STELLAR CLASSIFICATIONS OF 138,600 TARGETS IN CAMPAIGNS 1–8 (2015, result): “In addition to broadband photometry the KIC includes Kepler magnitudes (Kp), which were defined using gri magnitudes through a calibration of the expected flux in the Kepler bandpass, and stellar properties derived from fitting photometry to synthetic colors from model atmospheres.”
- Asteroseismology of Solar-Type and Red-Giant Stars (2013, background): “Bruntt et al. (2010), Bedding (2011) and Miglio (2012) compared asteroseismic and independently determined properties (e.g., from binaries) of a selection of bright solar-type stars and red giants, which all showed solar-like oscillations in observations made from either ground-based telescopes or…”
- Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “On the other hand, for ξ Hya, a third giant in our sample with similar parameters as β Gem and Vir, the single spectroscopic log g determination by Bruntt et al. (2010) agrees very well with the fundamental value.”
- CALCULATING ASTEROSEISMIC DIAGRAMS FOR SOLAR-LIKE OSCILLATIONS (2011, methodology): “The metallicities adopted for this modeling were −0.10 ± 0.07 for β Hyi (Bruntt et al. 2010) and +0.30 ± 0.05 for η Boo (Taylor 1996).”
- REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1–16 TRANSIT DETECTION RUN (2013, methodology): “We note that the properties are based on different spectroscopic analysis pipelines such as SME (Spectroscopy Made Easy, Valenti & Piskunov 1996), SPC (Stellar Parameter Classification, Buchhave et al. 2012), VWA (Versatile Wavelength Analysis, Bruntt et al. 2010), and ROTFIT (Frasca et al. 2003), a”
- Gaia FGK benchmark stars: Metallicity (2013, methodology): “The PASTEL catalogue has only two works reporting parameters for this star, where McWilliam (1990)obtained [Fe/H]= -0.04 while Bruntt et al. (2010) obtained [Fe/H]= +0.23.”
- The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets (2017, methodology): “They used the VWA (Bruntt et al. 2010) analysis tool to perform an iterative, line-by-line spectroscopic synthesis to match the observed spectra.”
- The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, background): “…abundances, pmode frequencies, mass, radius, surface gravity, and effective temperatures) are very well known for both stars (e.g., Bedding et al., 2004; Butler et al., 2004; Kjeldsen et al., 2005; Porto de Mello et al., 2008; Bruntt et al., 2010; Karoff et al., 2007; Chaplin et al., 2009).”
- Determining stellar macroturbulence using asteroseismic rotational velocities from Kepler (2014, methodology): “In this section we compare our calibration with some of the most widely used vmac relationships in the literature; namely those of Gray (1984a), Valenti & Fischer (2005) and Bruntt et al. (2010).”