2015A&A...581A..36M


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.06CEST03:28:05

2015A&A...581A..36M - Astronomy and Astrophysics, volume 581A, 36-36 (2015/9-1)

The flux-weighted gravity-luminosity relationship of blue supergiant stars as a constraint for stellar evolution.

MEYNET G., KUDRITZKI R.-P. and GEORGY C.

Abstract (from CDS):

The flux-weighted gravity-luminosity relationship (FGLR) of blue supergiant stars (BSG) links their absolute magnitude to the spectroscopically determined flux-weighted gravity logg/Teff4. BSG are the brightest stars in the universe at visual light and the application of the FGLR has become a powerful tool for determining extragalactic distances. Observationally, the FGLR is a tight relationship with only small scatter. It is, therefore, ideal for using as a constraint for stellar evolution models. The goal of this work is to investigate whether stellar evolution can reproduce the observed FGLR and to develop an improved foundation for the FGLR as an extragalactic distance indicator. We used different grids of stellar models for initial masses between 9 and 40M and for metallicities between Z=0.002 and 0.014, with and without rotation, which were computed with various mass loss rates during the red supergiant phase. For each of these models, we discuss the details of post-main sequence evolution and construct theoretical FGLRs by means of population synthesis models that we then compare with the observed FGLR. In general, the stellar evolution model FGLRs agree reasonably well with the observed one. There are, however, differences between the models, in particular with regard to the shape and width (scatter) in the flux-weighted gravity-luminosity plane. The best agreement is obtained with models that include the effects of rotation and assume that the large majority, if not all, of the observed BSG evolve toward the red supergiant phase and that only a few are evolving back from this stage. The effects of metallicity on the shape and scatter of the FGLR are small. The shape, scatter, and metallicity dependence of the observed FGLR are explained well by stellar evolution models. This provides a solid theoretical foundation for using this relationship as a robust extragalactic distance indicator.

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Journal keyword(s): supergiants - stars: rotation - galaxies: distances and redshifts

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME WLM Galaxy G 00 01 57.9 -15 27 50   11.50 11.10 10.93   ~ 576 2
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9475 1
3 NGC 300 GiG 00 54 53.4460065856 -37 41 03.182962667 8.83 8.69 8.13 7.46   ~ 1308 2
4 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5147 1
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14869 1
6 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4488 2
7 M 81 Sy2 09 55 33.17306143 +69 03 55.0609270   7.89 6.94     ~ 3972 5
8 NGC 3109 G 10 03 06.877 -26 09 34.46 11.10 10.42 10.04 9.91   ~ 695 2
9 NGC 3621 AGN 11 18 16.300 -32 48 45.36 10.10 9.44 9.56 8.07 10.1 ~ 489 3
10 M 106 Sy2 12 18 57.620 +47 18 13.39   9.14 8.41 8.11   ~ 2120 3

    Equat.    Gal    SGal    Ecl

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2020.08.06-03:28:05

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