COMPLEX VARIABILITY OF THE Hα EMISSION LINE PROFILE OF THE T TAURI BINARY SYSTEM KH 15D: THE INFLUENCE OF ORBITAL PHASE, OCCULTATION BY THE CIRCUMBINARY DISK, AND ACCRETION PHENOMENA

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dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.volumeNumber751en_US
dc.contributor.authorHamilton, Catrina M.en_US
dc.contributor.authorJohns-Krull, Christopher M.en_US
dc.contributor.authorMundt, Reinharden_US
dc.contributor.authorHerbst, Williamen_US
dc.contributor.authorWinn, Joshua A.en_US
dc.date.accessioned2013-03-13T18:45:38Zen_US
dc.date.available2014-03-19T05:10:04Zen_US
dc.date.issued2012en_US
dc.description.abstractWe have obtained 48 high-resolution echelle spectra of the pre-main-sequence eclipsing binary system KH 15D (V582 Mon, P = 48.37 days, e ∼ 0.6, MA = 0.6M , MB = 0.7M ). The eclipses are caused by a circumbinary disk (CBD) seen nearly edge on, which at the epoch of these observations completely obscured the orbit of star B and a large portion of the orbit of star A. The spectra were obtained over five contiguous observing seasons from 2001/2002 to 2005/2006 while star A was fully visible, fully occulted, and during several ingress and egress events. The Hα line profile shows dramatic changes in these time series data over timescales ranging from days to years. A fraction of the variations are due to “edge effects” and depend only on the height of star A above or below the razor sharp edge of the occulting disk. Other observed variations depend on the orbital phase: the Hα emission line profile changes from an inverse P-Cygni-type profile during ingress to an enhanced double-peaked profile, with both a blue and a red emission component, during egress. Each of these interpreted variations are complicated by the fact that there is also a chaotic, irregular component present in these profiles. We find that the complex data set can be largely understood in the context of accretion onto the stars from a CBD with gas flows as predicted by the models of eccentric T Tauri binaries put forward by Artymowicz & Lubow, G¨unther & Kley, and de Val-Borro et al. In particular, our data provide strong support for the pulsed accretion phenomenon, in which enhanced accretion occurs during and after perihelion passage.en_US
dc.embargo.terms1 yearen_US
dc.identifier.citationHamilton, Catrina M., Johns-Krull, Christopher M., Mundt, Reinhard, et al.. "COMPLEX VARIABILITY OF THE Hα EMISSION LINE PROFILE OF THE T TAURI BINARY SYSTEM KH 15D: THE INFLUENCE OF ORBITAL PHASE, OCCULTATION BY THE CIRCUMBINARY DISK, AND ACCRETION PHENOMENA." <i>The Astrophysical Journal,</i> 751, (2012) The American Astronomical Society: http://dx.doi.org/10.1088/0004-637X/751/2/147.en_US
dc.identifier.doihttp://dx.doi.org/10.1088/0004-637X/751/2/147en_US
dc.identifier.urihttps://hdl.handle.net/1911/70563en_US
dc.language.isoengen_US
dc.publisherThe American Astronomical Societyen_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.subject.keywordbinariesen_US
dc.subject.keywordeclipsing – binariesen_US
dc.subject.keywordspectroscopic – starsen_US
dc.subject.keywordindividual (KH 15D)en_US
dc.titleCOMPLEX VARIABILITY OF THE Hα EMISSION LINE PROFILE OF THE T TAURI BINARY SYSTEM KH 15D: THE INFLUENCE OF ORBITAL PHASE, OCCULTATION BY THE CIRCUMBINARY DISK, AND ACCRETION PHENOMENAen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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