What is shaping the planetary nebula K3-35?

Details What is shaping the planetary nebula K3-35? What is shaping the planetary nebula K3-35?

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..275..414g&link_type=abstract

Jets at all Scales, Proceedings of the International Astronomical Union, IAU Symposium, Volume 275, p. 414-415

Astronomy and Astrophysics

Astronomy

Magnetic Fields: Masers - Stars: Planetary Nebulae: Individual (K 3-35), Ism: Jets And Outflows

Scientific paper

K 3-35 is a very young planetary nebula (PN) with a characteristic S-shaped radio emission morphology. It is the first PN where water vapor maser was detected: the emission is located in a torus-like structure with a radius of 100 AU and also at the surprisingly large distance of 5000 AU from the star, in the tips of the bipolar lobes. Several mechanism have been proposed to explain the bipolar morphology of PNe, and in the case of K 3-35 we believe we may be observing several of them at the same time: i) a disk-like structure traced by the H2O masers, ii) a precessing bipolar jet probably due to the presence of a binary companion and iii) circular polarization in the OH 1665 MHz masers, which suggests the presence of a magnetic field. Additional observations and modeling are needed to establish what mechanisms are shaping K 3-35.

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