High Dispersion Spectra Investigation of the Planetary Nebula NGC 6833: Expansion Velocity and Recombination Line

다국어 초록 (Multilingual Abstract)

Using the spectroscopic data secured with the Hamilton Echelle Spectrograph attached to a 3-m telescope at the Lick Observatory, we derived the expansion velocities from various line profiles of Hi, He i, Ciii, Nii, Niii, [N ii], Oii, [O i], [Oii], [Oiii], [Ne iii], [Ar iii], [Ar iv], [S ii], [S iii], [Cl iii], and [Cl iv] in the 3600 °A to 10,000 °A wavelength range based on the full width at half maximum and the double peak. Using the recombination or permitted lines, we also derived elemental abundances and compared them with other values derived with forbidden lines and those found in the literature. The faster expansion velocities of the permitted Oii, Nii, Niii and perhaps Cii lines imply the existence of a somewhat smaller inner shell inside the outer main shell. The symmetrical shape of the permitted line profiles also indicates that these permitted line zone is symmetrical, e.g., a spherical shell or bipolar + torus structures, which might be evidence of relatively recent ejection from the central star. The nebular shell likely consists of a swiftly expanding inner shell and an outer normal shell excited by a central star of about 55,000 K. The former compact zone appears to be responsible for the permitted C, N, and O lines while the latter extended shell appears to be responsible for H, He, and forbidden lines. The location, large radial velocity, and less-enhanced C, N, and O abundances imply that NGC 6833 is likely to be a halo planetary nebulae.

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