Astron. Astrophys. 363, 1081-1190 (2000)

A new non-linear limb-darkening law for LTE stellar atmosphere models

Calculations for at several surface gravities ^*

A. Claret

Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain

Received 21 July 2000 / Accepted 15 September 2000

Abstract

A new non-linear limb-darkening law, based on the Least-Squares Method (LSM), is presented. This law is able to describe the intensity distribution much more accurately than any of the old ones given that the differences I(model)-I(fitting) are of some order of magnitude smaller than those derived from other approximations. This new law shows several advantages: it represents well the intensity distribution, the flux is conserved with high accuracy and it permits the use of a single law for the whole HR Diagram since the bi-parametric laws are only marginally valid in certain ranges of effective temperatures. The limb-darkening coefficients are computed for the 12 commonly used photometric bands . Bolometric and monochromatic calculations are also available. The computations are presented for 19 metallicities ranging from 10^-5 up to 10⁺¹ solar abundances, with log g varying between 0 and 5.0 and effective temperatures between 2000 K-50000 K. Results for microturbulent velocities of 0, 1, 2, 4, 8 km/s are also available. With this set of data it was possible to investigate, for the first time, the influence of such parameters in the limb-darkening. Limb-brightening, instead of limb-darkening, was detected for some models.

It is shown that the limb-darkening coefficients derived using the Flux Conservation Method (FCM) do not describe very well the intensity distribution, mainly near the border of the disk. On the contrary, the present coefficients, based on the LSM, represent very well the function I(µ) at any part of the disk for any filter or wavelength, log g, effective temperature, metallicity and microturbulent velocity.

The results are presented in 46 tables for the 12 filters (bolometric) and can be retrieved from the CDS. Due to the size of the remaining tables, mainly the monochromatic, these are available only on request (CD ROMs).

Key words: stars: atmospheres stars: binaries: eclipsing

* Tables 1-47 are available in electronic form at the CDS via anonymous ftp to ftp://cdsarc.u-strasbg.fr/pub/cats/J/A+A/363/1081 (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/363/1081 . Additional data are available on CD ROMs upon request. See online edition of A&A for Fig. 1, Fig. 4, Fig. 6 and Fig. 7 are only available here in the online version.

Send offprint requests to: claret@iaa.es

This article contains no SIMBAD objects.

Contents

• 1. Introduction
• 2. Numerical method and the models of stellar atmosphere
  • 2.1. A new non-linear law
  • 2.2. Least-squares and flux conservation methods
  • 2.3. Description of the stellar atmosphere models
• 3. Discussion of the results
  • 3.1. The effects of metallicity and microturbulent velocity on the LDC: ATLAS models
  • 3.2. PHOENIX models: monochromatic and 12 passbands calculations
• 4. Tables organization and final remarks
• Acknowledgements
• References

© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000
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