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The rate coefficient for the formation of aluminium monochloride, AlCl, from the radiative association of aluminium and chlorine atoms is estimated as a function of temperature. The coupling of the Al and Cl atoms through the A1Π molecular electronic state, which undergoes radiative transition to the X1Σ+ ground state, is the most efficient transition to form AlCl. The rate constant was found to vary with temperature according to the expressions k(T) = 1.22 × 10-16(T/300)0.40exp (-748/T) cm3 s-1 for temperatures between 300 and 1000 K, and k(T) = 2.20 × 10-16(T/300)0.175exp (-1067/T) cm3 s-1 for temperatures between 1000 and 14 000 K. [ABSTRACT FROM AUTHOR]

ABSTRACT We present optical photometry and spectroscopy of the peculiar Type IIn/Ibn supernova (SN) 2011hw. Its optical light curve exhibits a slower decline rate than that of normal SNe Ibc, with a peak absolute magnitude of −19.5 (unfiltered) and a secondary rise 20-30 d later of −18.3 mag ( R). Spectra of SN 2011hw are highly unusual compared to those of normal SN types, most closely resembling the spectra of SNe Ibn. We centre our analysis on comparing SN 2011hw to the well-studied Type Ibn SN 2006jc. While the two SNe have many important similarities, the differences are quite telling: compared to SN 2006jc, SN 2011hw has weaker He i and Ca ii lines and relatively stronger H lines, its light curve exhibits a higher visual-wavelength luminosity and slower decline rate, and emission lines associated with the progenitor's circumstellar material (CSM) are narrower. One can reproduce the unusual continuum shape of SN 2011hw with roughly equal contributions from a 6000-K blackbody and a spectrum of SN 2006jc. We attribute this blackbody-like emission component and many other differences between the two SNe to a small amount of additional H in SN 2011hw, analogous to the small H mass that makes SNe IIb differ from SNe Ib. Slower speeds in the CSM and somewhat elevated H content suggest a connection between SN 2011hw's progenitor and Ofpe/WN9 stars, which have been associated with luminous blue variables (LBVs) in their hot quiescent phases, and are H poor - but not H free like classical Wolf-Rayet (WR) stars. Comparisons between SN 2011hw and SN 2006jc can be largely understood if their progenitors exploded at different points in the transitional evolution from an LBV to a WR star. [ABSTRACT FROM AUTHOR]

The rate coefficients for the formation of carbon monophosphide (CP) and silicon monophosphide (SiP) by radiative association are estimated for temperatures ranging from 300 to 14 100 K. In this temperature range, the radiative association rate coefficients are found to vary from to and from to for CP and SiP, respectively. In both cases, rate coefficients increase slowly with the increase in temperature. [ABSTRACT FROM AUTHOR]