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Table 2

Teff and log g from previous analyses of G191−B2B.

Teff log g
Reference Method
[K] [cm/s2]
61 900 7.5a Shipman (1979) LTE, pure H, optical colors
56 788 ± 3336 5.95 ± 0.04 Koester et al. (1979) LTE, pure H, optical colors,b
62 250 ± 3520 7.55 ± 0.35 Holberg et al. (1986) LTE, pure H, H i L α line
59 250 ± 2000 7.50 ± 0.10 Kidder (1990) LTE, pure H, H i Hγ and Hδ lines
cited by Holberg et al. (1991)
61 000 8.00a Green et al. (1990) LTE, H+He, extreme ultraviolet (EUV) continuum
61 170 8.00a Finley et al. (1990) LTE, H+He, ultraviolet (UV) continuum
62 250 ± 1000 8.00a Finley et al. (1990) LTE, H+He, H i L α line
62 250 7.55 Vennes et al. (1991) NLTE, H+HeCNSi, UV spectrum
53 500 ± 500 Koester & Finley (1992) LTE, H+Hec, UV continuum
60 500 ± 900 7.50 ± 0.05 Vidal-Madjar et al. (1994) LTE, H+He, H i Balmer lines
57 900 ± 1500 7.50a Dupuis et al. (1995) NLTE, pure H, EUV continuumd
54 000 ± 800 7.50a Dupuis et al. (1995) NLTE, H+CNOFe, EUV continuumd
60 500 ± 1000 7.5 Lanz et al. (1996) LTE, H+HeC, H i Balmer lines
56 000 ± 1000 7.5 Lanz et al. (1996) NLTE, H+HeC, H i Balmer lines
55 200 ± 1000 7.5 Lanz et al. (1996) NLTE, H+HeCFe, H i Balmer lines
64 000 ± 1000 7.64 ± 0.06 Vennes et al. (1996) LTE, pure H, H i Lyman lines
57 900 ± 1500 7.5 Vennes et al. (1996) LTE, pure H, extreme UV (EUV) continuumd
64 100 ± 700 7.69 ± 0.04 Vennes et al. (1996) LTE, H+CNOFe, H i Balmer lines
52 600 ± 800 7.53 ± 0.07 Vennes et al. (1996) LTE, H+CNOFe, H i Lyman lines
54 000 ± 800 7.5 Vennes et al. (1996) LTE, H+CNOFe, EUV continuumd
61 193 ± 241 7.49 ± 0.01 Finley et al. (1997) LTE, H-Ni, H i Balmer lines
59 160 7.36 Barstow et al. (1998) NLTE, pure H, H i Balmer lines
59 190 7.36 Barstow et al. (1998) NLTE, H+He, H i Balmer lines
59 060 7.36 Barstow et al. (1998) NLTE, H+He + heavy-metal poor, H i Balmer lines
53 840 7.38 Barstow et al. (1998) NLTE, H+He + heavy-metal rich, H i Balmer lines
52 920 ± 350 7.36 ± 0.03 Barstow et al. (1998) NLTE, H+He + heavy-metal rich, H i Lyman linese
56 000 7.6 Wolff et al. (1998) LTE + NLTE, H+CNOSiFeNi, EUV continuumd
56 000 7.6 Dreizler & Wolff (1999) NLTE, H+CNOSiFeNi, diffusion model, EUV to optical
54 600 ± 200 7.60 ± 0.02 Barstow et al. (2001) NLTE, H+HeCNOSiFeNi, H i Balmer lines
52 930 ± 3600 7.16 ± 0.2 Barstow et al. (2001) NLTE, H+HeCNOSiFeNi, H i Lyman linesf
53 180 ± 530 7.43 ± 0.04 Barstow et al. (2001) NLTE, H+HeCNOSiFeNi, H i Lyman linese
56 000 7.59 Schuh et al. (2002) NLTE, H+HeCNOSiFeNi, diffusion model, EUV continuumd
54 000 7.5 Holberg et al. (2003) NLTE, metal lines
58 865 ± 706 7.57 ± 0.038 Lajoie & Bergeron (2007) NLTEg, pure H, H i Balmer lines
60 680 ± 15 000 7.57h Lajoie & Bergeron (2007) NLTEg, pure H, H i Lyman linesi
57 414 ± 4700 7.57h Lajoie & Bergeron (2007) NLTEg, pure H, V-normalization method
61 980 ± 514 7.56 ± 0.04 Allende Prieto et al. (2009) NLTE, Hj, H i Balmer lines
60 920 ± 993 7.55 ± 0.05 Gianninas et al. (2011) NLTE, H+CNO, H i Balmer linesk

Notes.

(a)

Assumed log g value.

(b)

The authors note that the results are extrapolated from their model grid.

(c)

Stratified model, hydrogen-layer mass between 6 × 10-15 and 8 × 10-15M⊙.

(d)

Extreme Ultraviolet Explorer (EUVE, http://heasarc.gsfc.nasa.gov/docs/euve/euve.html) observations.

(e)

Orbiting and Retrievable Far and Extreme Ultraviolet Spectrometer (ORFEUS, http://www.uni-tuebingen.de/en/4221) and FUSE observations.

(f)

Hopkins Ultraviolet Telescope (HUT, http://praxis.pha.jhu.edu/) observations.

(g)

International Ultraviolet Explorer (IUE) observations.

(h)

Adopted from their optical solution.

(i)

Models described in Liebert et al. (2005).

(j)

The authors note that Teff may be overestimated by ≈6000 K because their pure-H models are inappropriate due to the photospheric metal content.

(k)

New H i Stark line-broadening tables from Tremblay & Bergeron (2009).

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