The evolution of the planetary nebula NGC 6826

Journal Article · Fri Jun 01 04:00:00 EDT 1990 · Astronomical Journal; (USA)

DOI:https://doi.org/10.1086/115466· OSTI ID:6692210

Plait, P; Soker, N ^[1]

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1. Virginia Univ., Charlottesville (USA) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)

The density and mass profiles of the planetary nebula NGC 6826 are studied. New CCD images are used to deconvolve the density from the emission measure in H-alpha, assuming that the planetary nebula is spherically symmetric. For an assumed distance of 1.54 kpc the mass of the inner region r less than 13 arcsec is about 0.15 solar mass and that the entire visible planetary nebula is 0.54 solar mass. The possible formation of the dense shell at the edge of the nebula as a result of interaction with the ISM is discussed. The formation of the spherical outer halo together with an elliptical inner region can be explained by a low mass companion to the progenitor of NGC 6826 that was evaporated or collided with the central star. 28 refs.

• OSTI ID: 6692210
• Journal Information: Astronomical Journal; (USA), Journal Name: Astronomical Journal; (USA) Vol. 99; ISSN 0004-6256; ISSN ANJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BALMER LINES
BINARY STARS
CHARGE-COUPLED DEVICES
COLLISIONS
DENSITY
DISTRIBUTION
EMISSION SPECTRA
MASS DISTRIBUTION
NEBULAE
PHYSICAL PROPERTIES
PLANETARY NEBULAE
SEMICONDUCTOR DEVICES
SPATIAL DISTRIBUTION
SPECTRA
STAR EVOLUTION
STARS
STELLAR ACTIVITY
STELLAR WINDS