Papers on effective temperature calibrations
Bell R.A., Gustafsson B. (1989, MNRAS 236, 653)
Abstract
Temperature scales are found for G and K dwarf and giant stars, using
new tables of synthetic infrared colours as well as the infrared flux ratio
method. The temperature of 95 individual stars are given. The colours are
presented for grids of flux constant, line blanketed models. One grid has
been published previously, as have some colours for the visible region
of the spectrum. The models of the grid are in the range 4000 K < Teff <
6000 K, 0.75 < log g < 3.00, -3.0 < [A/H] < 0.00. A grid of dwarf models,
with the same temperature and abundance range but with 3.75 < log g < 4.5
is also used. The colours are computed from two series of overlapping
synthetic spectra, which have been calculated with a resolution of 0.1 A
between 3000 and 12000 A and 1.0 A between 0.9 and 6.0 microns.
Buser R., Kurucz R.L. (1978, A&A 70, 555)
Abstract
We present synthetic UBV colors for early-type stars computed from a new
grid of blanketed model atmosphere by Kurucz (1978), and from the revised
response functions by Buser (1978). Excellent agreement with Johnson's (1966)
mean intrinsic U-B and B-V colors for main sequence is obtained. The
theoretical efective temperature scale and the bolometric corrections agree
well with the empirical results found by Code et al. (1976).
Castelli F. (1993, Mem. S.A.It. , 585)
Abstract
For B-type stars, when Kurucz (1992a) new models are used, effective temperature
derived from fluxes agree well with effective temperature derived from the
co photometric index, provided that Vega, assumed as zero point for the
colours, is identified with the model Teff = 9500 K, logg = 4.05, vturb = 2 km/s,
and [M/H] = -0.5.
Fuhrmann K., Axer M., Gehren T. (1994, A&A 285, 585)
Abstract
Effective temperatures obtained from synthesis of the extended profile wings
of the first four Balmer lines are presented for more than 100 dwarfs and
subgiants of different metal abundances and surface gravities in the
temperature range from 5000 to 6500 K. Line formation is based on
homogeneous ODF blanketed model atmospheres in LTE. The resulting temperature
of the more metal-rich stars differ systematically from those determined
by the reference to synthetic broad- or intermediate-band colours such as
B-V, b-y, R-I or V-K. While the Balmer line temperatures give room to only
very small individual errors and result in a convincingly small mean
error for all four lines, the scatter against temperatures determined from
broad-band colours is by far outside the internal errors claimed in recent
applications. This may be attributed to either (a) observational errors,
(b) dependence on the relative mixture of metal abundances, (c) unknown
line blocking in most of the visible and near-infrared spectrum or (d) the
inhomogeneity found in the granulation patterns of stellar surfaces. Our
results suggest that broad-band colours are insuficient individual
temperature indicators, reliable only in a statistical sense.
Taylor B.J. (1994, PASP 106, 452)
Abstract
A calibration presented in a previous paper is used in this paper to derive
temperatures for FGK stars near the main sequence. The calibration is checked
against published counterparts, and it is found that previous calibrations
have not established K-dwarf temperatures in particular beyond reasonnable
doubt. The database assembled to derive the temperatures is described, and
the problems posed by close binaries are evaluated. The newly derived
temperatures are used to check a line-depth ratio proposed as a
thermometer by Gray and Johanson (1991, PASP 103, 439), and it is found
that the ratio is metallicity-sensitive. Temperatures are given for a total
of 417 stars.
McWilliams A. (1991, AJ 101, 1065)
Abstract
Effective temperature for a handful of F supergiants have been determined
using the Infrared Flux method, and have been used to calibrate various
broadband colors. The calibrations are in good agreement with a recent
theoretical calibration of F supergiant temperature scale.
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Last update: 7 July 1996