Accreting white dwarfs among the planetary nebulae most luminous in [O III] λ5007 emission

Noam Soker

doi:10.1086/500291

Accreting white dwarfs among the planetary nebulae most luminous in [O III] λ5007 emission

Noam Soker^*

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

17 Scopus citations

Abstract

I propose that some of the most luminous planetary nebulae (PNs) are actually proto-PNs, where a companion white dwarf (WD) accretes mass at a relatively high rate from the post-asymptotic giant branch star that blew the nebula. The WD sustains a continuous nuclear burning and ionizes the nebula. The WD is luminous enough to make the dense nebula luminous in the [O III] λ5007 line. In young stellar populations these WD accreting systems account for a small fraction of [O III]-luminous PNs, but in old stellar populations these binaries might account for most, or even all, of the [O III]-luminous PNs. This might explain the puzzling constant cutoff (maximum) [O III] λ5007 luminosity of the planetary nebula luminosity function across different galaxy types.

Original language	English
Pages (from-to)	966-970
Number of pages	5
Journal	Astrophysical Journal
Volume	640
Issue number	2 I
DOIs	https://doi.org/10.1086/500291
State	Published - 1 Apr 2006
Externally published	Yes

Keywords

Binaries: close
Planetary nebulae: general
Stars: AGB and post-AGB

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10.1086/500291

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title = "Accreting white dwarfs among the planetary nebulae most luminous in [O III] λ5007 emission",

abstract = "I propose that some of the most luminous planetary nebulae (PNs) are actually proto-PNs, where a companion white dwarf (WD) accretes mass at a relatively high rate from the post-asymptotic giant branch star that blew the nebula. The WD sustains a continuous nuclear burning and ionizes the nebula. The WD is luminous enough to make the dense nebula luminous in the [O III] λ5007 line. In young stellar populations these WD accreting systems account for a small fraction of [O III]-luminous PNs, but in old stellar populations these binaries might account for most, or even all, of the [O III]-luminous PNs. This might explain the puzzling constant cutoff (maximum) [O III] λ5007 luminosity of the planetary nebula luminosity function across different galaxy types.",

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N2 - I propose that some of the most luminous planetary nebulae (PNs) are actually proto-PNs, where a companion white dwarf (WD) accretes mass at a relatively high rate from the post-asymptotic giant branch star that blew the nebula. The WD sustains a continuous nuclear burning and ionizes the nebula. The WD is luminous enough to make the dense nebula luminous in the [O III] λ5007 line. In young stellar populations these WD accreting systems account for a small fraction of [O III]-luminous PNs, but in old stellar populations these binaries might account for most, or even all, of the [O III]-luminous PNs. This might explain the puzzling constant cutoff (maximum) [O III] λ5007 luminosity of the planetary nebula luminosity function across different galaxy types.

AB - I propose that some of the most luminous planetary nebulae (PNs) are actually proto-PNs, where a companion white dwarf (WD) accretes mass at a relatively high rate from the post-asymptotic giant branch star that blew the nebula. The WD sustains a continuous nuclear burning and ionizes the nebula. The WD is luminous enough to make the dense nebula luminous in the [O III] λ5007 line. In young stellar populations these WD accreting systems account for a small fraction of [O III]-luminous PNs, but in old stellar populations these binaries might account for most, or even all, of the [O III]-luminous PNs. This might explain the puzzling constant cutoff (maximum) [O III] λ5007 luminosity of the planetary nebula luminosity function across different galaxy types.

KW - Binaries: close

KW - Planetary nebulae: general

KW - Stars: AGB and post-AGB

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U2 - 10.1086/500291

DO - 10.1086/500291

M3 - 文章

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JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 I

ER -

Accreting white dwarfs among the planetary nebulae most luminous in [O III] λ5007 emission

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Keywords

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