Molecular hydrogen in planetary nebulae

Details Molecular hydrogen in planetary nebulae Molecular hydrogen in planetary nebulae

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...130..151i&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 130, no. 1, Jan. 1984, p. 151-156.

Astronomy and Astrophysics

Astrophysics

39

Hydrogen Clouds, Infrared Spectra, Molecular Clouds, Planetary Nebulae, Astronomical Models, Line Spectra, Molecular Excitation, Particle Collisions, Shock Fronts, Thermodynamic Equilibrium

Scientific paper

The author reports the detection of molecular hydrogen in six planetary nebulae; four others show no such emission. Two nebulae show an unidentified 2.285 μm feature previously seen only in NGC 7027. The strength of the υ = 1 - 0 S(2) line of H2 argues against radiative excitation of the molecular gas by near-UV photons, and so the data are interpreted in terms of the shock excitation model of Kwan (1977). Following this model rotation temperatures of 1000 - 2000K, preshock densities of 104 - 105 cm-3, and shocked H2 masses of ≡10-3 M_sun; are derived. The presence of shocked molecular gas in a large fraction of planetary nebulae indicates that many if not most planetaries must be optically thick in the Lyman continuum.

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