Kinematics and origin of the ringed bipolar nebula MZ 1

Details Kinematics and origin of the ringed bipolar nebula MZ 1 Kinematics and origin of the ringed bipolar nebula MZ 1

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...329..683m&link_type=abstract

Astronomy and Astrophysics, v.329, p.683-690 (1998)

Astronomy and Astrophysics

Astrophysics

4

Planetary Nebulae: Mz 1, Stars: Mass Loss, Ism: Jets And Outflows

Scientific paper

High resolution, spatially resolved measurements of the Hα , [NII] 6584 protect { Angstroms} and [SII] emission lines of the bipolar planetary nebula Mz 1 have been obtained with the Manchester Echelle Spectrometer on the Anglo-Australian telescope. The echelle profiles for slit positions that cross the central nebular core have been analysed and related to a previously obtained CCD image of the region. A well defined `ring like' structure, readily apparent in our Hα nii\ image, is shown to be expanding with the main bulk of the nebula at 23 km s(-1) and in a manner which is well represented by a cylindrical model with expansion velocities proportional to the radial distance from centre to cylinder edge. The dynamical lifetime of the nebula is of the order of 7,000 years. Estimates of the electron density from [SII] emission-line ratios suggest a density in the ring of order 1700 cm(-3) compared to 400 cm(-3) in the rest of the nebular core. Combining this result with IRAS measurements, we estimate a mass of the nebula of order 0.5 Msun. We discuss the probable origin and history of the nebula in terms of interacting stellar winds and consider the bipolar nebula as having been formed either via a fast wind in an aspherical density distribution, or through a superwind confined by an equatorial disc. In either case a relatively high mass-loss rate (>= 5 x 10(-5) Msunyr(-1) ) is inferred for the superwind phase prior to the existence of a fast wind phase of the current central star.

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