Abstract
Abstract We use Cloudy to re-examine excitation of [O i] 6300 Å and [O i] 5577 Å in the X-ray driven photoevaporative wind models of Owen and collaborators, and in more recent magnetothermal models by Wang et al. We find that, at the measured accretion luminosities, the far-ultraviolet (FUV) radiation would populate the upper levels of the oxygen, which would eventually contribute to the [O i] lines. FUV pumping competes with collisions as an excitation mechanism of the [O i] lines, and they each originate from a distinct region in the protostellar disk environment. Consequently, the line strengths and shapes of [O i] 6300 Å and [O i] 5577 Å would be affected by the inclusion of FUV pumping in the radiation transport simulations.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
