J/ApJS/112/487 Planetary nebulae classification (Soker 1997)
Properties that cannot be explained by the progenitors of planetary nebulae
Soker N.
<Astrophys. J. Suppl. Ser. 112, 487 (1997)>
=1997ApJS..112..487S 1997ApJS..112..487S (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae
Keywords: catalogs - ISM: structure - planetary nebulae: general -
stars: evolution
Abstract:
I classify a large number of planetary nebulae (458) according to the
process that caused their progenitors to blow axisymmetrical winds.
The classification is based primarily on the morphologies of the
different planetary nebulae, assuming that binary companions, stellar
or substellar, are necessary in order to have axisymmetrical mass loss
on the asymptotic giant branch. I propose four evolutionary classes,
according to the binary-model hypothesis:
(1) Progenitors of planetary nebulae that did not interact with any
companion. These amount to ∼10% of all planetary nebulae.
(2) Progenitors that interact with stellar companions that avoided a
common envelope, 11+2-3% of all nebulae.
(3) Progenitors that interact with stellar companions via a common
envelope phase, 23+11-5% of all nebulae.
(4) Progenitors that interact with substellar (i.e., planets and brown
dwarfs) companions via a common envelope phase, 56+5-8% of all
nebulae.
In order to define and build the different classes, I start with
clarifying some relevant terms and processes related to binary
evolution. I then discuss kinematical and morphological properties of
planetary nebulae that appear to require the interaction of the
planetary nebula progenitors and/or their winds with companions,
stellar or substellar.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 47 18 Single-progenitor PNe
table3.dat 60 52 A close stellar companion which avoided
common envelope
table4.dat 57 113 Common envelope with a stellar companion
table5.dat 54 275 Common envelope with a substellar companion
tables.tex 76 600 LaTeX version of the tables
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
Byte-by-byte Description of file: table?.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Object Object name
17- 26 A10 --- PNG PN G designation as in Catalog V/84
28- 29 A2 --- Conf [HL ] Confidence (1)
31- 44 A14 --- Dev Deviation (2)
46- 60 A15 --- Com Comments (3)
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Note (1): In table2 and table4, L means that the PNe may belong to table5
LL means that it may belong to table 3
In table3 and table5, L means that the PNe may belong to table4
Note (2): The letters in parentheses following the ISM mark give the direction
of the PN relative to the ISM.
WB: the deviation from axisymmetry is caused by a wide binary
ISM/WB: the deviation may be caused by the ISM or a wide binary
EWB: possible presence of an extreme-wide-binary
ISM-B: possibility that the ISM-magnetic field shaped the structure on
the outskirts
Question mark following ISM means that it is hard to tell from the
image whether the ISM really influences the PN morphology.
Note (3): PO stands for `pole-on', which means that these PN may be ellipticals
observed pole-on.
CB signifies PNe which are known to have close binary central stars
(Bond 1995, Ann. Israel Phys. Soc. 11, 61)
(No PN G): PNe which are not listed in the catalogue of
Acker et al. (1992, Cat. V/84)
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Acknowledgements: Soker Noam
(End) Patricia Bauer [CDS] 12-Dec-1997