Photodissociation Fronts

Bruce T. Draine, Dept. of Astrophysical Sciences, Princeton University

Some Papers

• Weingartner, J.C., & Draine, B.T. 2001, "Photoelectric Emission from Interstellar Dust: Grain Charging and Gas Heating" ( ApJ Suppl, 134, 263)
• Weingartner, J.C., & Draine, B.T. 2001, "Forces on Dust Grains Exposed to Anisotropic Radiation Fields" ( ApJ, 553, 581)
• Bertoldi, F., Draine, B.T., Rosenthal, D., Timmermann, R., Ramsay Howat, S.K., Geballe, T., Feuchtgruber, H., and Drapatz, S. 2000, "Excitation of H2 and HD in shocks and PDRs" ( in IAU Symposium 197: Astrochemistry, p. 191)
• Draine, B.T., and Bertoldi, F. 2000, "Theoretical Models of Photodissociation Fronts" ( in H2 in Space, p. 131)
• Draine, B.T. 2000, "Gamma Ray Bursts in Molecular Clouds: H2 Absorption and Fluorescence" ( ApJ, 532, 273)
• Draine, B.T., & Bertoldi, F. 1999a, "Heating the Gas in Photodissociation Fronts" ( ESA SP 427, 523)
• Vicini, B., Natta, A., Marconi, A., Testi, L., Hollenbach, D., & Draine, B.T. 1999, "A Near-Infrared Study of the Planetary Nebula NGC 2346" ( Astron. Astrophys., 342, 823)
• Bertoldi, F., Draine, B.T., Drapatz, S. Rosenthal, D., Timmerman, R., Wright, C.M. 1999, "ISO looks at shocks and photodissociation regions" ( in The Physics and Chemistry of the Interstellar Medium, Proceedings of the 3rd Cologne-Zermatt Symposium, 120)
• Timmermann, R., Bertoldi, F., Wright, C.M., Drapatz, S., Draine, B.T., Haser, L., & Sternberg, A. 1996, "H_2 infrared line emission from S140: a warm PDR", Astr. Ap., 315, L281.
• Draine, B.T., & Bertoldi, F. 1996, "Structure of Stationary Photodissociation Fronts", ( ApJ, 468, 269).
• Bertoldi, F., & Draine, B.T. 1996, "Non-Equilibrium Photodissociation Regions: I. Ionization-Dissociation Fronts", ( ApJ, 458, 222.

Catalog of PDR Models

• am3d (n=10^2,chi=1,diff.dust,T_0=300,cos(theta)=1) file= spdf.irs.am3d
• am3o (n=10^2,chi=1,orion dust,T_0=300,cos(theta)=1) file= spdf.irs.am3o
• aw3d (n=10^2,chi=1,diff.dust,T_0=500,cos(theta)=1) file= spdf.irs.aw3d
• aw3o (n=10^2,chi=1,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.aw3o
• bw3d (n=10^2,chi=10,diff.dust,T_0=500,cos(theta)=1) file= spdf.irs.bw3d
• bw3o (n=10^2,chi=10,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.bw3o
• bh3d (n=10^2,chi=10,diff.dust,T_0=1000,cos(theta)=1) file= spdf.irs.bh3d
• bh3o (n=10^2,chi=1,orion dust,T_0=1000,cos(theta)=1) file= spdf.irs.bh3o
• Bm3o (n=10^3,chi=10,orion dust,T_0=300,cos(theta)=1) file= spdf.irs.Bm3o
• Bw3o (n=10^3,chi=10,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Bw3o
• Cw3o (n=10^3,chi=10^2,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Cw3o
• Ch3o (n=10^3,chi=10^2,orion dust,T_0=1000,cos(theta)=1) file= spdf.irs.Ch3o
• Gm3o (n=10^4,chi=10^2,orion dust,T_0=300,cos(theta)=1) file= spdf.irs.Gm3o
• Gw3o (n=10^4,chi=10^2,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Gw3o
• Hw3o (n=10^4,chi=10^3,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Hw3o
• Hh3o (n=10^4,chi=10^3,orion dust,T_0=1000,cos(theta)=1) file= spdf.irs.Hh3o
• Lm3o (n=10^5,chi=10^3,orion dust,T_0=300,cos(theta)=1) file= spdf.irs.Lm3o
• Lw3o (n=10^5,chi=10^3,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Lw3o
• Mw3o (n=10^5,chi=10^4,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Mw3o
• Mh3o (n=10^5,chi=10^4,orion dust,T_0=1000,cos(theta)=1) file= spdf.irs.Mh3o
• Qm3o (n=10^6,chi=10^4,orion dust,T_0=300,cos(theta)=1) file= spdf.irs.Qm3o
• Qw3o (n=10^6,chi=10^4,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Qw3o
• Rw3o (n=10^6,chi=10^5,orion dust,T_0=500,cos(theta)=1) file= spdf.irs.Rw3o
• Rh3o (n=10^6,chi=10^5,orion dust,T_0=1000,cos(theta)=1) file= spdf.irs.Rh3o
• n2023a (n=10^5,chi=5000,orion dust,T_0=500,cos(theta)=0.2) file= spdf.irs.n2023a
• n2023b (n=10^5,chi=5000,orion dust,T_0=900,cos(theta)=0.2) file= spdf.irs.n2023b

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