A Grid of NLTE Line-blanketed Model Atmospheres of Early B-Type Stars

By T. Lanz, I. Hubeny. 2006

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We have constructed a comprehensive grid of 1540 metal line-blanketed, NLTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to early B-type stars. The BSTAR2006 grid considers 16 values of effective temperatures, 15,000 K ≤ Teff ≤ 30,000 K with 1000 K steps, 13 surface gravities, 1.75 ≤ log g ≤ 4.75 with 0.25 dex steps, six chemical compositions, and a microturbulent velocity of 2 km s-1. The lower limit of log g for a given effective temperature is set by an approximate location of the Eddington limit. The selected chemical compositions range from twice to one-tenth of the solar metallicity and metal-free. Additional model atmospheres for B supergiants (log g ≤ 3.0) have been calculated with a higher microturbulent velocity (10 km s-1) and a surface composition that is enriched in helium and nitrogen and depleted in carbon. This new grid complements our earlier OSTAR2002 grid of O-type stars (our Paper I). The paper contains a description of the BSTAR2006 grid and some illustrative examples and comparisons. NLTE ionization fractions, bolometric corrections, radiative accelerations, and effective gravities are obtained over the parameter range covered by the grid. By extrapolating radiative accelerations, we have determined an improved estimate of the Eddington limit in absence of rotation between 55,000 and 15,000 K. The complete BSTAR2006 grid is available at the TLUSTY Web site.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c8fe631bf540ee330879e7789f8aa510c4e79c42

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Citations in the corpus

A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS (2010, methodology): “Plane-parallel models, such as ATLAS (Kurucz 2005) or TLUSTY (Lanz & Hubeny 2003, 2007), cannot account for spectral lines forming in the wind and are obviously not suitable for our purpose.”
THE RED MSX SOURCE SURVEY: THE MASSIVE YOUNG STELLAR POPULATION OF OUR GALAXY (2013, methodology): “The last model sequence uses the same data as applied in the modelling of Davies et al. (2011), with the stellar models coming from Martins et al. (2005) and Lanz & Hubeny (2007).”
THE DATA REDUCTION PIPELINE FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (2015, methodology): “…K • 2.0 < log g < 5.0 • −2.0 < [Fe/H] < 0.3 The ASS T (Koesterke et al. 2008; Koesterke 2009, 2012) spectral synthesis package was used for cool and warm stars (Teff ≤ 10,000 K) and TLUSTY (Hubeny 1988; Hubeny & Lanz 1995; Hubeny et al. 1998; Lanz & Hubeny 2007) for hot stars (Teff ≥ 15,000 K).”
INTRINSIC COLORS, TEMPERATURES, AND BOLOMETRIC CORRECTIONS OF PRE-MAIN-SEQUENCE STARS (2013, background): “…of the adopted Teff , including Balona (1994); Bertone et al. (2004); Flower (1996); Bessell et al. (1998); Masana et al. (2006); Schmidt-Kaler (1982); Code et al. (1976); Casagrande et al. (2006, 2008, 2010); Lanz & Hubeny (2007); Vacca et al. (1996); Lanz & Hubeny (2003)14 where they applicable.”
Accretion disks in luminous young stellar objects (2015, background): “Assuming that the centimeter continuum emission comes from an optically thin Hii region, one can deduce the Lyman-continuum photons emitted per second (NLy) (e.g., Mezger & Henderson, 1967) and relate it to the spectral type (Martins et al., 2005; Lanz & Hubeny, 2007; Davies et al., 2011).”
The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, unknown): “Bolometric corrections were obtained from LMC-metallicity models (Lanz & Hubeny 2007) for the primary component, and together with an adopted distance modulus of 18 m .”
A STELLAR ROTATION CENSUS OF B STARS: FROM ZAMS TO TAMS (2010, background): “For example, Lanz & Hubeny (2007) show that the non-LTE Hγ profiles tend to be slightly stronger and broader than those derived from LTE atmospheres (see their Fig.”
Visual and ultraviolet flux variability of the bright CP star θ Aurigae (2015, methodology): “For each model atmosphere we calculated the synthetic spectrum using the code SYNSPEC with atomic data from Lanz & Hubeny (2007).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…ionizing spectra come from the library of metal line-blanketed, non-local thermodynamic equilibrium (non-LTE), plane-parallel, hydrostatic models of Lanz & Hubeny (2003, 2007), which reach effective temperatures of up to 55,000 K and cover a wide range of metallicities (from zero to twice solar).”
SPITZER SAGE INFRARED PHOTOMETRY OF MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD (2009, methodology): “We compare the observed colors with colors of plane-parallel non-LTE TLUSTY stellar atmosphere models (Lanz & Hubeny 2003, 2007) of appropriate metallicity and effective temperatures.”
THE MASS OF THE BLACK HOLE IN CYGNUS X-1 (2011, background): “For the specific case of Cygnus X-1, the range of temperature–gravity pairs on the star contained points that are outside the OSTAR2002+BSTAR2006 model grids (Lanz & Hubeny 2003, 2007).”