J/A+A/541/A98 Interacting planetary nebulae (Ali+, 2012)
Interacting planetary nebulae. I. Classification and orientation.
Ali A., Sabin L., Snaid S., Basurah H.M.
<Astron. Astrophys., 541, A98-98 (2012)>
=2012A&A...541A..98A 2012A&A...541A..98A
ADC_Keywords: Planetary nebulae ; Interstellar medium
Keywords: planetary nebulae: general - methods: statistical
Abstract:
We discuss the classification and orientation of planetary nebulae
that interact with the interstellar medium throughout the Milky Way. A
sample of 117 confirmed interacting planetary nebulae is used for this
purpose. Our results indicate that the majority of interacting objects
are located close to the Galactic plane, and ∼77% of them are located
inside the Galactic thin disk.
Description:
The present sample has been established by collecting IPNe data from a
large number of articles discussing the subject.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 125 117 The main parameters of the interacting planetary
nebulae sample
refs.dat 143 103 References
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
J/AJ/115/1989 : Distances of galactic planetary nebulae (Tajitsu+, 1998)
J/ApJS/112/487 : Planetary nebulae classification (Soker 1997)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Sequential number
5- 15 A11 --- PN PN name
17- 22 F6.2 deg GLON Galactic longitude
24- 29 F6.2 deg GLAT Galactic latitude
31- 42 A12 --- r_IA Reference for interaction angle
46- 47 I2 deg IA ? Measured interaction angle
49- 50 I2 deg e_IA ? rms uncertainty on IA
52- 56 I5 pc Dist ? Distance
58- 61 A4 --- n_Dist Measurement method used (1)
63- 70 A8 --- r_Dist References for IPNe distance
72- 79 F8.2 arcsec theta Angular radius θ
81- 83 I3 --- r_theta ? References for IPNe radius
85- 89 F5.2 km/s Vexp ? Expansion velocity
91- 97 A7 --- r_Vexp References for IPNe expansion velocity
99-104 F6.1 pc Z ? Height above the plane
107-111 F5.3 pc R ? Linear radius
113-120 E8.3 yr Tdyn ? Dynamical age
122-125 A4 --- Stage [WZO1-4 ] WZO stage (WZO1 to WZO4) (2)
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Note (1): Methods as follows:
Ind = means individual distance
Ph02 = means distances calculated according to Phillips distance
scale (2002ApJS..139..199P 2002ApJS..139..199P)
St = means statistical distances from literature
Note (2): According to 3D-hydrodynamic simulations by Wareing, Zijlstra and
O’Brien (2007MNRAS.382.1233W 2007MNRAS.382.1233W) from the beginning of the slow AGB
wind phase to the end of the post-AGB/PN phase. The PN-ISM interaction
process can be divided into four stages:
* in stage WZO1, the PN expands freely within the bubble of the undisturbed
slow AGB wind material and is unaffected by the AGB wind-ISM interaction.
* in stage WZO2, the PN interacts with the bow shock formed during the AGB
wind-ISM interaction process, and the density and the emission in the
upstream side increases accordingly;
* in stage WZO3, the geometric center of the PN is moving downstream away
from the central star
* in stage WZO4, the PN is completely disrupted and the central star is
outside the PN.
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Ref Reference number
5- 23 A19 --- BibCode BibCode
25- 57 A33 --- Aut Author's name
60-143 A84 --- Com Comments
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Jul-2012