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

Journal Article · Mon Oct 01 00:00:00 EDT 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/169258· OSTI ID:6164188

O'dell, C R; Weiner, L D; Chu, Yoyhua ^[1]

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1. Rice Univ., Houston, TX (USA) Illinois Univ., Urbana (USA)

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. 26 refs.

• OSTI ID: 6164188
• Journal Information: Astrophysical Journal; (USA), Vol. 362; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
PLANETARY NEBULAE
MORPHOLOGY
MATHEMATICAL MODELS
PARTICLE KINEMATICS
RINGS
SOLAR SYSTEM
STELLAR WINDS
THREE-DIMENSIONAL CALCULATIONS
NEBULAE
STELLAR ACTIVITY
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources