A kinematic determination of the structure of the double ring planetary nebula NGC 2392, the Eskimo

Details A kinematic determination of the structure of the double ring planetary nebula NGC 2392, the Eskimo A kinematic determination of the structure of the double ring planetary nebula NGC 2392, the Eskimo

Oct 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...362..226o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 362, Oct. 10, 1990, p. 226-234.

Astronomy and Astrophysics

Astrophysics

24

Kinematics, Planetary Nebulae, Ring Structures, Stellar Structure, Stellar Winds, Line Of Sight, Oort Cloud, Solar System, Three Dimensional Models

Scientific paper

Slit spectra and existing 'velocity cube' data have been used to determine the structure of the double ring PN NGC 2392. The inner shell is a stellar wind-sculpted prolate spheroid with a ratio of axes of 2:1 and the approaching end of the long axis pointed 20 deg from the line of sight in P.A. = 200 deg. The outer ring is caused by an outer disk with density dropping off with distance from the central star and with distance from its plane, which is the same as the equatorial band of high density in the inner shell. The outer disk contains a ring of higher density knots at a distance of 16 arcsec and is losing material through free expansion, forming an outer envelope of increasing velocity. Forbidden S II spectra are used to determine the densities in all of the major regions of the nebula. It is argued that the filamentary cores at the centers of the knots seen in the outer ring originate in the sublimation of bodies formed at the same time as the parent star.

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