High-velocity flow in the central part of the highly evolved planetary nebula Abell 30

Details High-velocity flow in the central part of the highly evolved planetary nebula Abell 30 High-velocity flow in the central part of the highly evolved planetary nebula Abell 30

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106..165y&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 106, no. 696, p. 165-169

Astronomy and Astrophysics

Astronomy

8

Planetary Nebulae, Stellar Envelopes, Stellar Evolution, Stellar Mass Ejection, Stellar Motions, Stellar Spectra, Stellar Winds, Velocity Distribution, Velocity Measurement, Astronomical Spectroscopy, Companion Stars, Interstellar Matter, Red Giant Stars

Scientific paper

We obtained a high-dispersion (O III) lambda 5007 spectrum of the highly evolved planetary nebula, Abell 30 (PK 208 + 33 deg 1 = IRAS 08440 + 1803). We found a high-velocity component in the profile, whose expansion velocity is derived from its full width at half maximum, 166 km/sec, and from the full width at zero intensity, VFWZI approximately equals 450 km/sec, in addition to the two velocity components from the previously identified knots. Moreover, from the position of the broad component, we determined the systemic velocity as Vsys = 13 km/sec in the frame of the Local Standard of Rest. These narrow components are attributed to J2 and J3-H4 identified by Jacoby (1979) and Hazard et al. (1980). Because Abell 30 is famous as a hydrogen-deficient planetary nebula, we suggest that its central star, having already shed its hydrogen envelope to expose the helium core, is now shedding its helium envelope. Abell 30 is, therefore, considered to have experienced the secondary ejection phase. Moreover the evidence of the existence of the fast stellar wind suggests that there is a dramatic effect on the material around the central star. We briefly discuss the origin of such a high-velocity flow.

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