Photon Heating of Envelopes around Young Stellar Objects: An Explanation for CO J = 6-5 Emission
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[1] A. Tielens,et al. Photon-dominated regions around cool stars: The effects of the color temperature of the radiation field , 1994 .
[2] A. Tielens,et al. THE PHOTOELECTRIC HEATING MECHANISM FOR VERY SMALL GRAPHITIC GRAINS AND POLYCYCLIC AROMATIC HYDROCARBONS , 1994 .
[3] J. W. Kooi,et al. A lownoise 665 GHz SIS quasi-particle waveguide receiver , 1994 .
[4] A. Harris,et al. Submillimeter CO observations of warm gas around T Tauri stars , 1993 .
[5] P. Martin,et al. The Size Distribution of Interstellar Dust Particles as Determined from Extinction , 1993 .
[6] L. Hartmann,et al. Optical excess emission in T Tauri stars , 1991 .
[7] A. Dalgarno,et al. Interstellar Photodissociation and Photoionization Rates , 1991 .
[8] G. Basri,et al. Hamilton echelle spectra of young stars. I: Optical veiling , 1990 .
[9] T. Hartquist,et al. Ultraviolet radiation in molecular clouds , 1990 .
[10] Scott J. Kenyon,et al. Spectral energy distributions of T Tauri stars - Disk flaring and limits on accretion , 1987 .
[11] P. Cassen,et al. The collapse of the cores of slowly rotating isothermal clouds , 1984 .
[12] B. Draine,et al. CO line emission from shock waves in molecular clouds , 1984 .
[13] F. Shu. Self-similar collapse of isothermal spheres and star formation. , 1977 .