Atmospheric, evolutionary, and spectral models of the brown dwarf Gliese 229 B

Science

Volumn 272, Issue 5270, 1996, Pages 1919-1920

  Marley, M S ^a   Saumon, D ^b   Guillot, T ^b   Freedman, R S ^c   Hubbard, W B ^b   Burrows, A ^b   Lunine, J I ^b  

^a NEW MEXICO STATE UNIVERSITY   (United States)

^b UNIVERSITY OF ARIZONA   (United States)

^c NASA AMES RESEARCH CENTER   (United States)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; ASTRONOMY; ATMOSPHERE; EVOLUTION; GRAVITY; MATHEMATICAL ANALYSIS; MODEL; PRIORITY JOURNAL;

EID: 0030037262     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.272.5270.1919     Document Type: Article

References (31)

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4. K. Matthews, T. Nakajima, S. R. Kulkarni, B. R. Oppenheimer, in preparation; T. R. Geballe, S. R. Kulkarni, C. E. Woodward, G. C. Sloan, Astrophys. J., in press.
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14. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
15. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
16. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
17. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
18. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
19. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
20. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
21. 3 was included in the spectral models but not in the temperature profile computation. The baseline models assume that the atmosphere is free of clouds.
22. For the temperature profile computation, we treated the molecular opacity using the k-coefficient method [R. Goody, R. West, L. Chen, D. Crisp, J. Quant. Spectrosc. Radiat. Transfer 42, 539 (1989)]. After a radiative-equilibrium temperature profile was found, we iteratively adjusted the atmosphere to self-consistently solve for the size of the convection zones, given the specified internal heat flux. Given the radiative-convective temperature-pressure profiles, we generated high-resolution synthetic spectra by solving the radiative transfer equation [P. Bergeron, F. Wesemael, G. Fontaine, Astrophys. J. 367, 253 (1991)]. Eighteen thousand frequency points were used in the spectral region from 1 to 15.4 μm. These spectra were smoothed with a Gaussian-bandpass filter giving a final resolution of λ/Δλ = 600.
23. For the temperature profile computation, we treated the molecular opacity using the k-coefficient method [R. Goody, R. West, L. Chen, D. Crisp, J. Quant. Spectrosc. Radiat. Transfer 42, 539 (1989)]. After a radiative-equilibrium temperature profile was found, we iteratively adjusted the atmosphere to self-consistently solve for the size of the convection zones, given the specified internal heat flux. Given the radiative-convective temperature-pressure profiles, we generated high-resolution synthetic spectra by solving the radiative transfer equation [P. Bergeron, F. Wesemael, G. Fontaine, Astrophys. J. 367, 253 (1991)]. Eighteen thousand frequency points were used in the spectral region from 1 to 15.4 μm. These spectra were smoothed with a Gaussian-bandpass filter giving a final resolution of λ/Δλ = 600.
24. K. Matthews, T. Nakajima, S. Kulkarni, B. Oppenheimer, Int. Astron. Union Circ. 6280 (1995).
25. B. Fegley Jr. and K. Lodders, Icarus 110, 117 (1994).
26. K. Lodders, personal communication.
27. A. Burrows, D. Saumon, T. Guillot, W. B. Hubbard, J. I. Lunine, Nature 375, 299 (1995).
28. D. Saumon et al., Astrophys. J. 460, 993 (1996).
29. T. Guillot, D. Gautier, G. Chabrier, B. Mosser, Icarus 112, 337 (1994).
30. G. Lindal, Astron. J. 103, 967 (1992).
31. D.S. is a Hubble Fellow. T.G. is supported by the European Space Agency. This research was supported by grants from NASA and NSF. We thank T. Geballe for digital versions of the GI 229 B spectrum, K. Lodders for chemical-equilibrium calculations, and K. Zahnle for an insightful review.