Helium abundance and ionization structure in the Orion nebula: radio recombination lines observations

Details Helium abundance and ionization structure in the Orion nebula: radio recombination lines observations Helium abundance and ionization structure in the Orion nebula: radio recombination lines observations

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...464..995p&link_type=abstract

Astronomy and Astrophysics, Volume 464, Issue 3, March IV 2007, pp.995-1002

Astronomy and Astrophysics

Astrophysics

3

Ism: Abundances, Ism: Hii Regions, Radio Lines: Ism, Ism: Individual Objects: Orion Nebula

Scientific paper

Results of the Ori A HII region mapping based on hydrogen (H), helium (He) and carbon (C) Radio Recombination lines (RRL) are presented. Observations were made with the same angular resolution (2') using the 32 m VLBI dish of Medicina (Italy, 22.4 GHz) and the Pushchino RT-22 dish (Russia, 36.5 GHz). The behaviour of the ionized helium abundance, y^+, with distance from the center shows that the He+ zone size is smaller than that of H^+. Such a behaviour is different for the core and for the envelope, as well as for different directions from the center. The helium abundance, N(He)/N(H)=10.0(± 0.8)%, is measured. Derived line radial velocities, their widths and y+ data support the well-known "blister-type" structure of this HII region. LTE electron temperatures (7800-9600 K) are also measured.
Appendices (Figs. 15, 16 and Sect. 4.1 "Carbon RRLs") are only available in electronic form at http://www.aanda.org

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