Zero-phonon emission bands of solid hydrogen at 6-12 μm wavelength. An astrophysical phenomenon

Details Zero-phonon emission bands of solid hydrogen at 6-12 μm wavelength. An astrophysical phenomenon Zero-phonon emission bands of solid hydrogen at 6-12 μm wavelength. An astrophysical phenomenon

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ltp....35..311s&link_type=abstract

Low Temperature Physics, Volume 35, Issue 4, pp. 311-317 (2009).

Other

Phonon Interactions, Crystal And Ligand Fields, Nuclear States And Interactions, Other Nonmetallic Inorganics, Atomic Processes And Interactions, Molecular And Chemical Processes And Interactions

Scientific paper

Infrared emission bands in the wavelength range of 6-12 μm observed in the ISO-SWS mission are assigned to rotational zero-phonon bands of solid parahydrogen by using Van Kranendonk's approximate rigid-lattice method. This method is based on superposed electric quadrupole pair interactions and superposed quadrupole induced dipole moments of pairs in the hcp crystal. Accordingly, the approximate formalism uses zero-order H2 pair wave functions. Symmetry effects of the hcp crystal require preference of rotational pair transitions. The interaction potential of the pairs is confined to the electric quadrupole-quadrupole interaction. Zero-phonon emission bands of H2 pair transitions fitted to the spectrum contain at least one delocalized j=2 state initially and/or finally because of their significantly enhanced emission rates. They also yield the characteristic bandwidths which fit nicely to the widths of the observed features. The frequency positions of the seven pure parahydrogen pair transitions used, obtained from experimentally determined rotational solid hydrogen energy levels, are in perfect agreement with the observed features, whereas the three mixed ortho-parapair transitions need a presently unknown frequency correction, caused by the migration of the ortho-H2 molecules into the parahydrogen crystal prior to emission, the so-called initial excess binding energies. The astrophysical setup of the observed source is discussed in the end of the paper.

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