The nature and structure of the emission line nebula K3-35: a very young planetary nebula with precessing bipolar jet-like outflows?

Details The nature and structure of the emission line nebula K3-35: a very young planetary nebula with precessing bipolar jet-like outflows? The nature and structure of the emission line nebula K3-35: a very young planetary nebula with precessing bipolar jet-like outflows?

Jul 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.298..243m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 298, Issue 1, pp. 243-250.

Astronomy and Astrophysics

Astronomy

13

Stars: Mass-Loss, Ism: Jets And Outflows, Ism: Kinematics And Dynamics, Planetary Nebulae: Individual: K3-35, Radio Continuum: Ism

Scientific paper

We present Hα, [NII]6583 and 6-cm continuum images of the emission line nebula K3-35. The optical images reveal an extended nebula (size ~=11x9arcsec^2 in [NII]) in which most of the emission originates in a very narrow (width 0.7-1.3 arcsec) S-shaped region which extends almost all along the nebula (~=7 arcsec). The 6-cm continuum emission also arises in this narrow region, which is characterized by an exceedingly high point-symmetry and systematic and continuous changes of the orientation with respect to the nebular centre. The properties of the narrow region suggest that it represents a system of precessing bipolar jet-like components. Two low-excitation, compact bipolar knots near the tips of the jet-like components are observed in the deduced [NII]/Hα image ratio. These knots may be generated by the interaction of the collimated outflows with surrounding material. A comparison of the optical and radio images shows the existence of differential extinction within the nebula. Maximum extinction is observed in a disc-like region which traces the equator of the elliptical shell previously observed at 20-cm continuum. All available data strongly suggest that K3-35 is a very young planetary nebula in which we could be observing the first stages of the formation of collimated outflows and point-symmetric structures typically observed in planetary nebulae. The properties of the jet-like components in K3-35 are in good agreement with models of binary central stars in which highly collimated outflows originate either from a precessing accretion disc or via magnetic collimation in a precessing star.

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