A study of the asymmetry in the H{2}O maser line at λ = 1.35 cm on the base of the hyperfine structure

Details A study of the asymmetry in the H{2}O maser line at λ = 1.35 cm on the base of the hyperfine structure A study of the asymmetry in the H{2}O maser line at λ = 1.35 cm on the base of the hyperfine structure

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008a%26a...492..475l&link_type=abstract

Astronomy and Astrophysics, Volume 492, Issue 2, 2008, pp.475-480

Astronomy and Astrophysics

Astrophysics

2

Line: Profiles, Masers, Radiative Transfer

Scientific paper

The results of analyzing asymmetry in the H2O maser lines at λ = 1.35 cm are presented. We investigated in detail the known mechanism of the asymmetry origin due to the hyperfine structure of the 616 to 523 transition and different (not equidistant) positions of the corresponding triplet components. The triplet of the lines is characterized by the sum of extinction factors that are continuously transformed into a single-peaked asymmetric extinction coefficient, with the increase in the Doppler widths (characterizing by effective Doppler velocity u_D). A noticeable asymmetry corresponds to u_D≤ 0.5-1 km s-1. For higher values of uD the extinction factor approaches a Gaussian shape with the decreasing magnitude of the profile asymmetry. An appreciable asymmetry in unsaturated maser lines can only arise at u_D≤ 0.5 km s-1, if there are very narrow linewidths (Δ u≈ 0.2-0.4 km s-1). But observed saturated masers possess a fairly high degree of the line asymmetry, 10-40%. Most probably, this asymmetry is a result of rebroadening of the linewidth up to the value that is comparable to the width of the asymmetric extinction coefficient.

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