The Kinematics of the Extensive Bipolar Lobes and Symmetric Knots of the Planetary Nebula KjPn 8 (PK 112-00 1)

Details The Kinematics of the Extensive Bipolar Lobes and Symmetric Knots of the Planetary Nebula KjPn 8 (PK 112-00 1) The Kinematics of the Extensive Bipolar Lobes and Symmetric Knots of the Planetary Nebula KjPn 8 (PK 112-00 1)

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...475..705l&link_type=abstract

Astrophysical Journal v.475, p.705

Astronomy and Astrophysics

Astronomy

28

Ism: Jets And Outflows, Ism: Kinematics And Dynamics, Ism: Structure, Ism: Planetary Nebulae: Individual Alphanumeric: Kjpn 8

Scientific paper

Spatially resolved profiles of the H alpha and [N II] 6548 and 6584 A lines have been obtained with the Manchester echelle spectrometer, combined with the 2.1 m San Pedro Martir telescope, over the bipolar lobes, the symmetric low-ionization knots, and the bright core of the planetary nebula KjPn 8. The lobes of this Galactic bipolar nebula have the largest angular extent, 14' x 4', yet discovered. A wedge-shaped outflow from the core in a northwestern direction has a receding radial velocity of 200 km s-1 with respect to the systemic radial velocity (Vhel = -44 km s-1). An approaching counterflow, toward the southeast, has a radial velocity difference of 206 km s-1. Individual knots, in one of the pairs of symmetric groups, have similarly symmetric radial velocities of +/-220 km s-1 with respect to the systemic radial velocity. Remarkably, these extreme radial velocities for each knot are continuous down to the systemic radial velocity. The diffuse, but limb-brightened, bipolar lobes emit split [N II] lambda 6584 profiles at +/-40 km s-1 with respect to the systemic radial velocity over large angular extents. There is some evidence that these split components converge to the systemic radial velocity at these bright rims. It is concluded that the extensive lobes are three-dimensional structures and most likely represent the earliest outflows from the nebular core. VLA observations at 3.5 cm, with an angular resolution of 0."9, show that the 4" diameter core of KjPn 8 has a clumpy structure. The two most prominent knots observed in the radio continuum could be aligned with the fastest ejecta observed at the larger scale and may represent material ejected in the last few decades. Various possibilities for the generation of these observed kinematic features are explored. In particular, the action of bipolar, episodic jets is considered for the creation of the high-velocity, symmetric groups of collisionally ionized knots.

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