2007 **Abstract:** 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 ≤ T eff ≤ 30 000 K with 1 000 K steps, 13 surface gravities, 1.75 ≤ log g ≤ 4.75 with 0.25 dex steps, 6 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 l…

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“…), the theoretical spectra computed by Kunze do not include the metal line blanketing. This indicates that they probably overestimate the effective temperatures by as much as ∼2000 K. Even when one compares the synthetic spectra from the O-star grid, and the later published spectra from the B-star grid (Lanz & Hubeny 2007) in the overlapping temperature range, it turns out that the two sets of model spectra differ from each other since the B-star values are based on somewhat improved input physics. Clearly, without further progress in the model spectra, one cannot do any better.…”

confidence: 99%

“…), the theoretical spectra computed by Kunze do not include the metal line blanketing. This indicates that they probably overestimate the effective temperatures by as much as ∼2000 K. Even when one compares the synthetic spectra from the O-star grid, and the later published spectra from the B-star grid (Lanz & Hubeny 2007) in the overlapping temperature range, it turns out that the two sets of model spectra differ from each other since the B-star values are based on somewhat improved input physics. Clearly, without further progress in the model spectra, one cannot do any better.…”

confidence: 99%

“…The analysis makes use of grids of model atmospheres calculated using the and codes (Hubeny 1988;Hubeny & Lanz 1995;Hubeny et al 1998;Lanz & Hubeny 2007). Details of the methods adopted can be found in Hunter et al (2007), while a more detailed discussion of the grids can be found in Ryans et al (2003), Dufton et al (2005) 2 .…”

confidence: 99%

“…The expression for the complex amplitudes of the light variations in a given passband within the linear and zero-rotation approximation can be found, e.g., in Daszyńska-Daszkiewicz et al (2002), and need not be repeated here. To compute the values of these observables, we used the nonadiabatic pulsational code of Dziembowski (1977) and tables of the fluxes in photometric passbands and nonlinear limb-darkening coefficients computed by Daszyńska-Daszkiewicz & Szewczuk (2011) on the basis of the NLTE atmosphere models of Lanz & Hubeny (2007).…”

confidence: 99%