The Kurucz (Smithsonian) Atomic and Molecular Database

The spectrum of FG Sagittae after photometric recovery in 2000

“…It is interesting to note that, if this value of [C/H] is used with the Jurcsik (1996) relation of the inter-fade periods of R CrB stars as a function of carbon abundance, we get that period ~700 days, Grevesse et al (1996), log CEI relative to H 2 Gonzalez et al (1998) 3 Bell (1976) 4 Thévenin (1989Thévenin ( ,1990 5 Cowley et al (2000) 6 Kurucz (1993) which is right the mean time interval between the observed major brightness drops of FG Sge. We confirm the absence of 13 C, which is not an unexpected result taking into account the very large enhancements of s-process elements.…”

“…Some of.the oscillator strengths in the line-list were changed to the values given by Thevenin (1989Thevenin ( , 1990. Also, some heavy element lines from the lists by Cowley et al (2000) and by Kurucz (1993) were added. The sources of log gf-s are also indicated in Table 1.…”

Properties and calibrations of the Washington photometric system from synthetic photometry

“…First, a grid of blanketed model atmospheres for F to K-type stars constructed by Buser & Kurucz 1992 (hereafter BKLATE) which combine the Kurucz & Peytremann (1975) atomic lines list (~ 10 6 ) used in the early-type models of Kurucz (1979) with the atmosphere models for late-type stars of Gustafsson et al (1975), Bell et al (1976), Gustafsson (1979). Second, the extensive and homogeneous grid of new blanketed model atmospheres of Kurucz (1991Kurucz ( ,1992, hereafter K92) covering a large range of temperatures and metallicities and using a large (~ 50 · 10 6 ) list of atomic and molecular opacities.…”

Hot Stars: Old-Fashioned or Trendy?

“…The complete set of observed emission line ratios of Ne and Ar is shown in Figure 7 together with the corresponding results of nebular model computations for which solar metallicity and a gas density of 800 cm −3 has been assumed, and which are based on LTE (static atmosphere from Kurucz, 1992) as well as NLTE (expanding atmosphere from Pauldrach et al, 2001) spectral energy distributions.…”