Abundances of HDE 341617 (Arellano Ferro+, 2001)

Details Abundances of HDE 341617 (Arellano Ferro+, 2001) Abundances of HDE 341617 (Arellano Ferro+, 2001)

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ycat..33680250a&link_type=abstract

VizieR On-line Data Catalog: J/A+A/368/250. Originally published in: 2001A&A...368..250A

Other

Protostars, Planetary Nebulae, Equivalent Widths, Radial Velocities

Scientific paper

Table 11.dat: Several absorption lines of He I, O II, Si III and Fe II are detected. The radial velocity, for each individual line unambiguously identified is given. For He I two groups of lines are identified at average velocities of 52.6+/-8.3km/s (4 lines) and 75.0+/-3.7km/s (4 lines). This suggests some stratification in the atmosphere. The rest of the species however average 73.3+/-2.9km/s (15 lines). The low dispersion in the radial velocity suggests that all these lines are formed in the same region of the stellar atmosphere and no stratification is evident.
Table 12.dat: the emission spectrum, formed in the outer envelope and/or in the nebulosity, consists of lines of Fe II, [Fe II], Fe III, [S II], O I, [N II] and Si II. The radial velocities of emission lines are all very consistent and average 54.3+/-3.4km/s. The difference of radial velocities between the absorption and emission lines indicates that the nebulosity expands at about 19km/s. The Balmer lines show emission on top of the stellar absorption. The emission is shifted relative to the absorption and is consistent with the radial velocities of other emission features, showing that it is also produced in the same region.
(2 data files).

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