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.


Jean-Claude.Mermilliod@obs.unige.ch
Last update: 7 July 1996