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We use observations of the CI, CII, HI, and H_2 column densities along lines of sight in the Galactic plane to determine the formation rate of H_2 on grains and to determine chemical reaction rates with Polycyclic Aromatic Hydrocarbons. Photodissociation region models are used to find the best fit parameters to the observed columns. We find the H_2 formation rate on grains has a low rate (R ~ 1 x 10^(-17) cm^(3) s^(-1)) along lines of sight with low column density (A_V < 0.25) and low molecular fraction (f_(H_2) < 10^(-4)). At higher column densities (0.25 < A_V <2.13), we find a rate of R ~ 3.5x10^(-17) cm^(3) s^(-1). The lower rate at low column densities could be the result of grain processing by interstellar shocks which may deplete the grain surface area or process the sites of H +H formation, thereby inhibiting H_2 production. Alternatively, the formation rate may be normal, and the low molecular fraction may be the result of lines of sight which graze larger clouds. Such lines of sight would have a reduced H_2 self-shielding compared to the line-of-sight column. We find the reaction C^+ +PAH^- --> C + PAH^0 is best fit with a rate 2.4 x 10^(-7) Phi_PAH T_2^(-0.5) cm^(3) s^(-1) with T_2= T/100 K and the reaction C^+ + PAH^0 --> C + PAH^+ is best fit with a rate 8.8x 10^(-9)Phi_PAH cm^(3) s^(-1). In high column density gas we find Phi_PAH ~ 0.4. In low column density gas, Phi_PAH is less well constrained with Phi_PAH ~ 0.2 - 0.4.
With the high-resolution spectroscopy now available in the optical and satellite UV, it is possible to determine the neutral/ionized column density ratios for several different elements in a single cloud. Assuming ionization equilibrium for each elem
We use a series of N-body/smoothed particle hydrodynamics simulations and analytic arguments to show that the presence of an effective temperature floor in the interstellar medium at T_F ~ 10^4 K naturally explains the tendency for low-mass galaxies
Following our initial discovery of blue luminescence in the spectrum of the Red Rectangle (RR) and its identification as fluorescence by small three- to four-ringed polycyclic aromatic hydrocarbon (PAH) molecules, we report on the spatial correlation
Blue Luminescence (BL) was first discovered in a proto-planetary nebula, the Red Rectangle (RR) surrounding the post-AGB star HD 44179. BL has been attributed to fluorescence by small, 3-4 ringed neutral polycyclic aromatic hydrocarbon (PAH) molecule
Paircorrelations and the magnetic susceptibility of electrons in a spherical cavity are studied both for grand canonical and the canonical ensemble. The coupling constant of the $BCS$ Hamiltonian is adjusted to experimental values of the gap paramete