Another problem is that with the RL abundances, the energy balance of the Orion nebula is not well understood. If the CEL/RL abundance discrepancy were caused by temperature fluctuations in the nebula, as argued by some authors, the same kind of discrepancy should be seen for the other elements, such as C, N and Ne, which is not what we find in the present study. This result calls for further investigation. We find that the oxygen nebular abundance based on recombination lines agrees much better with the stellar abundances than the one derived from the collisionally excited lines. We compare the resulting gas+dust nebular abundances with the stellar abundances of a sample of 13 B-type stars from the Orion star-forming region (Ori OB1), analyzed in Papers I and III of this series. We estimate the amount of oxygen trapped in dust grains for several scenarios of dust formation. We re-evaluate the CEL and RL abundances of several elements in the Orion nebula and estimate the associated uncertainties, taking into account the uncertainties in the ionization correction factors for unseen ions. We re-examine the recombination/collisional emission line (RL/CEL) nebular abundance discrepancy problem in the light of recent high-quality abundance determinations in young stars in the Orion star-forming region. LUTH, Observatoire de Paris, CNRS, Université ParisĪims. Astronomical objects: linking to databasesĮ-mail: de Astrofísica, Universidad de La.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences
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