Mg-H(+) charge transfer and MG line intensities in gaseous nebulae

Details Mg-H(+) charge transfer and MG line intensities in gaseous nebulae Mg-H(+) charge transfer and MG line intensities in gaseous nebulae

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.235.1245a&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 235, Dec. 15, 1988, p. 1245-1255. Research supported by

Astronomy and Astrophysics

Astronomy

30

Atomic Spectra, Charge Transfer, Magnesium, Nebulae, Hydrogen Ions, Photoionization, Planetary Nebulae, Protons, Reaction Kinetics

Scientific paper

Cross sections determined for the charge-transfer reaction Mg + H(+) yields Mg(+) + H do not provide evidence for the existence of a Mg-abundance gradient within gaseous nebulae. In the domain of energies relevant to these nebulae, charge transfer into the 3p state of Mg(+) occurs via coupling to an intermediate molecular state which correlates with H + Mg(+)(4s). Photoionization models reveal that Mg abundances derived from Mg I, II, or V agree in any one nebula to within a factor of 2.

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