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dc.contributor.authorBond, Howard
dc.contributor.authorRobin, Ciardullo
dc.contributor.authorEsplin, Taran L.
dc.contributor.authorHawley, Steven A.
dc.contributor.authorLiebert, James
dc.contributor.authorMunari, Ulisse
dc.date.accessioned2017-11-06T20:23:41Z
dc.date.available2017-11-06T20:23:41Z
dc.date.issued2016-07-27
dc.identifier.citationBond, H. E., Ciardullo, R., Esplin, T. L., Hawley, S. A., Liebert, J., & Munari, U. (2016). The Nucleus Of The Planetary Nebula Egb 6 As A Post-Mira Binary. The Astrophysical Journal, 826(2), 139. doi:10.3847/0004-637x/826/2/139en_US
dc.identifier.urihttp://hdl.handle.net/1808/25273
dc.description.abstractEGB 6 is a faint, large, ancient planetary nebula (PN). Its central star, a hot DAOZ white dwarf (WD), is a prototype of a rare class of PN nuclei associated with dense, compact emission-line knots. The central star also shows excess fluxes in both the near-infrared (NIR) and mid-infrared (MIR). In a 2013 paper, we used Hubble Space Telescope (HST) images to show that the compact nebula is a point-like source, located 0 16 (∼118 AU) from the WD. We attributed the NIR excess to an M dwarf companion star, which appeared to coincide with the dense emission knot. We now present new ground-based NIR spectroscopy, showing that the companion is actually a much cooler source with a continuous spectrum, apparently a dust-enshrouded low-luminosity star. New HST images confirm common proper motion of the emission knot and red source with the WD. The I-band, NIR, and MIR fluxes are variable, possibly on timescales as short as days. We can fit the spectral energy distribution (SED) with four blackbodies (the WD, a ∼1850 K NIR component, and MIR dust at 385 and 175 K). Alternatively, we show that the NIR/MIR SED is very similar to that of Class 0/I young stellar objects. We suggest a scenario in which the EGB 6 nucleus is descended from a wide binary similar to the Mira system, in which a portion of the wind from an AGB star was captured into an accretion disk around a companion star; a remnant of this disk has survived to the present time and is surrounded by gas photoionized by UV radiation from the WD.en_US
dc.publisherAmerican Astronomical Societyen_US
dc.rights© 2016. The American Astronomical Society. All rights reserved.en_US
dc.subjectBinariesen_US
dc.subjectVisual-planetary nebulaeen_US
dc.subjectGeneral-White dwarfsen_US
dc.titleTHE NUCLEUS OF THE PLANETARY NEBULA EGB 6 AS A POST-MIRA BINARYen_US
dc.typeArticleen_US
kusw.kuauthorHawley, Steven A.
kusw.kudepartmentPhysics and Astronomyen_US
dc.identifier.doi10.3847/0004-637X/826/2/139en_US
kusw.oaversionScholarly/refereed, publisher versionen_US
kusw.oapolicyThis item meets KU Open Access policy criteria.en_US
dc.rights.accessrightsopenAccess


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