The Kinematics and Morphologies of Planetary Nebulae with Close-Binary Central Stars

Details The Kinematics and Morphologies of Planetary Nebulae with Close-Binary Central Stars The Kinematics and Morphologies of Planetary Nebulae with Close-Binary Central Stars

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..240..429m&link_type=abstract

Binary Stars as Critical Tools and Tests in Contemporary Astrophysics, International Astronomical Union. Symposium no. 240, he

Astronomy and Astrophysics

Astrophysics

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Scientific paper

A programme is currently underway to study the kinematics and morphologies of PNe known to contain close-binary central stars. Three of the observed PNe have eclipsing binaries: Abell 63, Abell 46 and SuWt2.; these objects are important because their physical parameters can be determined in a model independent way. The properties of these PNe can then be used as tests of stellar evolutionary theory. Long-slit spectra of northern sky targets were obtained in 2004 with the Manchester echelle spectrometer combined with the 2.1-m San Pedro Martir telescope. Southern sky targets were observed in 2005 using UCLES onboard the 3.9-m Anglo-Australian telescope, and the EMMI spectrograph combined with the 3.58-m ESO New Technology Telescope in La Silla. The test case of the programme is Abell 63 as it contains an almost totally eclipsing binary core. The nebula has two faint, elongated lobes and a tube-like appearance. Two end-caps are visible in [NII] at the tips of the lobes. Slits were positioned along the major and minor axes of the nebula. The longslit spectra from the major axis show clear Halpha line-splitting, which can be attributed to receding and approaching sides of an expanding hollow tube. The longslit spectra from the minor axis show a velocity ellipse, which is characteristic of viewing a hollow tube in cross-section. Soker (1998) predicted that bipolar nebulae with very elongated lobes must be produced by an intrinsically collimated fast wind (or jets) puncturing through a pre-existing spherical AGB wind. Soker proposed that the presence of a low-mass companion star is necessary for the production of jets via an accretion disk around the secondary. We tested this hypothesis for Abell 63 using a hydrodynamic simulation of a low-density 400 kms^-1 jet blowing into a uniform, static AGB wind. The resulting morphology closely resembled that of Abell 63.

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