期刊
ASTRONOMY & ASTROPHYSICS
卷 613, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201732447
关键词
hydrodynamics; stars: atmospheres; techniques: photometric; techniques: spectroscopic
资金
- Research Council of Lithuania [MIP-089/2015]
- Sonderforschungsbereich of the German Research Foundation (DFG) [SFB 881]
- Research Council of Lithuania
Aims. We studied the influence of convection on the spectral energy distributions (SEDs), photometric magnitudes, and colour indices of different types of stars across the H-R diagram. Methods. The 3D hydrodynamical (COBOLD)-B-5, averaged < 3D >, and 1D hydrostatic LHD model atmospheres were used to compute SEDs of stars on the main sequence (MS), main sequence turn-off (TO), subgiant branch (SGB), and red giant branch (RGB), in each case at two different effective temperatures and two metallicities, [M/H] = 0.0 and -2.0. Using the obtained SEDs, we calculated photometric magnitudes and colour indices in the broad-band Johnson-Cousins UBVRI and 2MASS JHK(s), and the medium-band Stromgren uvby photometric systems. Results. The 3D-1D differences in photometric magnitudes and colour indices are small in both photometric systems and typically do not exceed +/- 0.03 mag. Only in the case of the coolest giants located on the upper RGB are the differences in the U and u bands able reach approximate to -0.2 mag at [M/H] = 0.0 and approximate to -0.1 mag at [M/H] = 2.0. Generally, the 3D-1D differences are largest in the blue-UV part of the spectrum and decrease towards longer wavelengths. They are also sensitive to the effective temperature and are significantly smaller in hotter stars. Metallicity also plays a role and leads to slightly larger 3D-1D differences at [M/H] = 0.0. All these patterns are caused by a complex interplay between the radiation field, opacities, and horizontal temperature fluctuations that occur due to convective motions in stellar atmospheres. Although small, the 3D-1D differences in the magnitudes and colour indices are nevertheless comparable to or larger than typical photometric uncertainties and may therefore cause non-negligible systematic differences in the estimated effective temperatures.
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