CHEMISTRY IN A PROTOPLANETARY NEBULA

In this paper we investigate gas-phase chemistry in the remnant 'superwind' of a carbon-rich red giant star, during its transition to a planetary nebula. The interacting stellar winds model is used. It is found that during the first few hundred years of transition, significant abundances of a few small molecules and ions (e.g. CH+, CH2+, CH3+, CH, CH2, NH) may occur in the thin, dense, shocked shell of gas predicted by thiS model, but that most molecules observed in protoplanetary nebulae will be rapidly destroyed, through photodissociation by strong UV from the central star. If dense clumps are present during transition, they may allow the gas-phase formation and/or survival of small amounts of some molecules, such as HCN, CN, C2H2, and HC3N, until about 2000 yr after termination of the superwind; and young, fully developed planetary nebulae may show observable amounts of polyatomic molecules by this means. Such clumping may explain the existence of, e.g., HCN in NGC 7027.

PHOSPHORUS CHEMISTRY IN DENSE INTERSTELLAR CLOUDS

I have used recent laboratory studies on the reactions of the phosphorus hydride ions, PH(n)+ (n = 0-4) to construct a new model of phosphorus chemistry in interstellar clouds. I find that the non-detection of PN in cold, dark clouds in consistent with the chemical models only if the depletion of phosphorus in large, approximately 10(4) in TMC-1. Although the laboratory studies indicate that organo-phosphorus chains C(n)P can be formed, this large depletion precludes the detection of any phosphorus-bearing moleclues in cold clouds. However, in warm clouds associated with star formation, the depletion of phosphorus may be reduced. In this case one can reproduce the PN abundance toward Orion KL with a depletion factor of about 300. Interestingly, if the organo-phosphorus species are not destroyed by O atoms, I predict fractional abundances in Ori KL of between 10(-11) and 10(-10) for C(n)P (n = 2-4) and HCCP.

Liquid-liquid slug flow: Hydrodynamics and pressure drop

In this paper, the hydrodynamics and the pressure drop of liquid-liquid slug flow in round microcapillaries are presented. Two liquid-liquid flow systems are considered, viz. water-toluene and ethylene glycol/water-toluene. The slug lengths of the alternating continuous and dispersed phases were measured as a function of the slug velocity (0.03-0.5 m/s), the organic-to-aqueous flow ratio (0.1-4.0), and the microcapillary internal diameter (248 and 498 mu m). The pressure drop is modeled as the sum of two contributions: the frictional and the interface pressure drop. Two models are presented, viz, the stagnant film model and the moving film model. Both models account for the presence of a thin liquid film between the dispersed phase slug and the capillary wall. It is found that the film velocity is of negligible influence on the pressure drop. Therefore, the stagnant film model is adequate to accurately predict the liquid-liquid slug flow pressure drop. The influence of inertia and the consequent change of the slug cap curvature are accounted for by modifying Bretherton's curvature parameter in the interface pressure drop equation. The stagnant film model is in good agreement with experimental data with a mean relative error of less than 7%.