office: 60 Garden Street Room P-243 Mail stop 50 Cambridge, MA 02138 phones: 617-495-4984 or 496-7534 fax: 617-495-7455 page: 617-896-1241 e-mail: email@example.com emergencies: call 617-495-7289 (Donna Coletti), 5-4862 (09:30-14:00 only), 5-4865, 5-7377, or 5-7051 to try to locate meupdated (in part): 16 December, 1996
He is also a member of the Science team for the Ultraviolet Coronal Spectrometer that observed the solar corona from the Spartan 201 satellite that was launched and retrieved by STS-64 and 69. The Spartan UVCS will be launched again in late 1997 on STS-87.
Additional papers can be found through searches of the ADS Instrumentation database and the ADS Physics and Geophysics database. Beware of false `hits'.
In collaboration with others in the laboratory, he has measured transition probabilities (A-values) of allowed lines of iron group elements; made the first measurements of the A-values of some of the spin-changing, `intersystem' lines used in interstellar-cloud abundance determinations and in line-ratio methods for diagnostics of astrophysical plasmas; and measured absorption cross sections and f-values for lines of molecules seen, or expected to be seen, in the absorption spectra of diffuse and translucent interstellar clouds.
He has published 74 papers in books or refereed journals, mostly on these subjects and on instrumentation for high resolution spectroscopy, for FUV and EUV radiometry, and for spectroscopic and radiometric measurements from spacecraft.
Smith served as Secretary of Commission 14 (Atomic & Molecular Data) of the IAU and as a member of the Organizing Committee for the meetings held in August 1994.
In their studies of atoms and ions of astrophysical interest, Smith and colleagues have measured f-values for intersystem lines in low-Z ions. When reliable oscillator strengths are available, these weak lines are particularly useful for interstellar abundance determinations and for plasma density diagnostic techniques that are used by astronomers. The CfA measurements have motivated reevaluation of a number of calculated values of these parameters.
A. G. Calamai, Smith, and S. D. Bergeson, recently published the first measured lifetimes for the 3s2 3p 2Po - 3s3p2 4P intersystem lines of Si II. Cardelli et al. (ApJ 420, L29, 1993) used spectra obtained with the GHRS on HST to study absorption by interstellar silicon toward zeta Oph. They detected absorption by some of the intersystem lines at ~235 nm and by the resonance multiplet at ~181 nm. Column densities derived from both sets of lines agreed, thus confirming both sets of oscillator strengths and the observational and data analysis techniques. Cardelli et al. point out that, because the f-values for the weaker intersystem lines are now available, these will be useful for column density determinations in regions of high silicon abundance where the resonance lines would be saturated.
Last update August, 1996