Planetary nebulae NGC 6826 and NGC 2899: early aspherical mass loss?

By systematically searching regions around planetary nebulae (PNe) for signs of interactions of their precursors’ wind with ambient matter we found a number of huge IRAS dust structures. Some of them may be chance projections, but a few appear to be real, like those around NGC 6826 and NGC 2899. In...

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Bibliographic Details
Published in:Astrophysics and space science 2009-10, Vol.323 (4), p.323-327
Main Authors: Aryal, B., Rajbahak, C., Weinberger, R.
Format: Article
Language:English
Subjects:
Astrobiology
Astronomy
Astrophysics
Astrophysics and Astroparticles
Cosmology
Dust
Infrared imaging systems
Nebulae
Observations and Techniques
Original Article
Physics
Physics and Astronomy
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Stars & galaxies
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Summary:By systematically searching regions around planetary nebulae (PNe) for signs of interactions of their precursors’ wind with ambient matter we found a number of huge IRAS dust structures. Some of them may be chance projections, but a few appear to be real, like those around NGC 6826 and NGC 2899. In the case of NGC 6826 we noticed a giant (∼2°) bipolar dust emission, whose axis is along the proper motion of the central star. The PN itself is offset in the direction of motion both as to the center of this ∼30 pc large dust structure and to the center of a similarly large new H α nebula. NGC 2899 was found in the center of a 14×11 pc quadrupolar cavity, whose directions of axes coincide with the directions of the main axes of the optical PN. In both cases, the formation of these structures appears to have commenced in the asymptotic giant branch (AGB) phase.
ISSN:0004-640X
1572-946X
DOI:10.1007/s10509-009-0076-9