Observation and interpretation of temperature gradients in the Orion Nebula

Details Observation and interpretation of temperature gradients in the Orion Nebula Observation and interpretation of temperature gradients in the Orion Nebula

Sep 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977apj...216..427p&link_type=abstract

Astrophysical Journal, Part 1, vol. 216, Sept. 1, 1977, p. 427-432.

Astronomy and Astrophysics

Astronomy

10

Gas Spectroscopy, Nebulae, Radiative Recombination, Radio Sources (Astronomy), Temperature Gradients, Abundance, Gas Temperature, Helium, Hydrogen, Interstellar Chemistry, Metal Vapors, Radiation Hardening

Scientific paper

Radio recombination lines of hydrogen and helium, measured at several positions in Orion A, show that the gas kinetic temperature is nearly 3000 K higher at the nebular periphery than at the core, in agreement with recent optical results. Theoretical models suggest that the effect of radiation hardening is not sufficient to account for the observed temperature gradient. It is proposed that much of the temperature gradient results from a gradient in the gas-phase metal abundance, caused by evaporation of grains near the central star; in this case an outward decrease of O/H in the gas by a factor of about 4 is required.

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