Astronomy and Astrophysics – Astronomy
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.6001s&link_type=abstract
American Astronomical Society, 182nd AAS Meeting, #60.01; Bulletin of the American Astronomical Society, Vol. 25, p.897
Astronomy and Astrophysics
Astronomy
Scientific paper
The strength of the He I 2.06 microns emission line relative to hydrogen recombination features has been previously proposed as a diagnostic of effective temperature Teff for stars powering HII regions. Such an indicator would be of particular interest for constraining the high-end initial mass function in starbursts. This talk will present new calculations bearing on the sensitivity of the 2.06 microns feature to nebular conditions. The results illustrate a number of complications for interpreting the He I/Brgamma ratio as a constraint on Teff. The ratio is sensitive to the relative volumes of He(+) and H(+) , as well as the relative ionization fractions of He and H within the He(+) zone, both of which respond to variation in Teff. Predicted values of He I/Brgamma are also sensitive to nebular geometry, dust content, density, and helium abundance. The present examples suggest that caution is required in intepreting measured ratios as indices of ionizing continuum shape.
No associations
LandOfFree
The He I 2.06 microns/Brgamma Ratio as a Nebular Diagnostic does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The He I 2.06 microns/Brgamma Ratio as a Nebular Diagnostic, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The He I 2.06 microns/Brgamma Ratio as a Nebular Diagnostic will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1849992