Photoionization models of the Eskimo nebula: evidence for a binary central star?

A. Danehkar, D. J. Frew, Q. A. Parker, O. De Marco

    Research output: Chapter in Book/Report/Conference proceedingConference proceeding contributionpeer-review

    10 Citations (Scopus)

    Abstract

    The ionizing star of the planetary nebula NGC 2392 is too cool to explain the high excitation of the nebular shell, and an additional ionizing source is necessary. We use photoionization modeling to estimate the temperature and luminosity of the putative companion. Our results show it is likely to be a very hot (Teff ≃ 250 kK), dense white dwarf. If the stars form a close binary, they may merge within a Hubble time, possibly producing a Type Ia supernova.

    Original languageEnglish
    Title of host publicationFrom Interacting Binaries to Exoplanets: Essential Modeling Tools
    EditorsMercedes T. Richards, Ivan Hubeny
    Place of PublicationCambridge; New York
    PublisherCambridge University Press
    Pages470-471
    Number of pages2
    Volume7
    ISBN (Print)9781107019829
    DOIs
    Publication statusPublished - Jul 2011
    EventIAU Symposium - Lima, Peru, Lima
    Duration: 5 Jan 201114 Jan 2011

    Publication series

    NameProceedings of the International Astronomical Union
    NumberS282
    Volume7
    ISSN (Print)17439213
    ISSN (Electronic)17439221

    Conference

    ConferenceIAU Symposium
    CityLima
    Period5/01/1114/01/11

    Keywords

    • Planetary nebulae: individual (NGC 2392)
    • photoionization codes
    • shock models

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