Reference : Revisited mass-loss rates for the nuclei of the planetary nebulae NGC 6210, NGC 6826 ...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/20722
Revisited mass-loss rates for the nuclei of the planetary nebulae NGC 6210, NGC 6826 and NGC 6543 - The first order moment W1 of subordinate line profiles
English
Hutsemekers, Damien mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Surdej, Jean mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
1987
Astronomy and Astrophysics
EDP Sciences
173
101-107
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] B STARS ; LINE SHAPE ; MASS FLOW RATE ; PLANETARY NEBULAE ; STELLAR ENVELOPES ; STELLAR MASS EJECTION ; ABUNDANCE ; COMPUTATIONAL ASTROPHYSICS ; CYGNUS CONSTELLATION ; NUCLEI ; OPTICAL THICKNESS ; VELOCITY DISTRIBUTION
[en] The authors present the results of numerical calculations for the first order moment W[SUB]1[/SUB] of subordinate P Cygni line profiles as a function of the parameter W[SUB]1[/SUB][SUP]0[/SUP]alphaM>n[SUB]g[/SUB]<[SUB]s[/SUB], where Mrepresents the mass-loss rate of the central star and >n[SUB]g[/SUB]<[SUB]s[/SUB] the average fractional abundance of the relevant ion across the region of the envelope where the subordinate line profile is formed. The calculations clearly show that for unsaturated P Cygni line profiles the relation W[SUB]1[/SUB]alphaM>n[SUB]g[/SUB]<[SUB]s[/SUB] holds irrespective of the type of the opacity and/or velocity distributions. For currently observed P Cygni line profiles, the misuse of this relation can lead to an underestimate of the mass-loss rates by more than one order of magnitude. This is illustrated for the case of 3 selected central stars of planetary nebulae (NGC 6210, NGC 6826 and NGC 6543) for which mass-loss rates have been revisited.
http://hdl.handle.net/2268/20722
The authors thank EDP Sciences for their deposit authorization

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