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Title:
KH 15D: A Spectroscopic Binary
Authors:
Johnson, John Asher; Marcy, Geoffrey W.; Hamilton, Catrina M.; Herbst, William; Johns-Krull, Christopher M.
Affiliation:
AA(Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720-3411 , .), AB(Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720-3411 , .), AC(Visiting Astronomer, McDonald Observatory, which is operated by the University of Texas at Austin.; Department of Physics and Astronomy, Rice University, 6100 Main Street, Houston, TX 77005; , .), AD(Van Vleck Observatory, Wesleyan University, Middletown, CT 06459; .), AE(Visiting Astronomer, McDonald Observatory, which is operated by the University of Texas at Austin.; Department of Physics and Astronomy, Rice University, 6100 Main Street, Houston, TX 77005; , .)
Publication:
The Astronomical Journal, Volume 128, Issue 3, pp. 1265-1272. (AJ Homepage)
Publication Date:
09/2004
Origin:
UCP
AJ Keywords:
Stars: Binaries: Spectroscopic, Stars: Circumstellar Matter, Stars: Individual: Alphanumeric: KH 15D, Stars: Pre-Main-Sequence, Techniques: Radial Velocities
DOI:
10.1086/422735
Bibliographic Code:
2004AJ....128.1265J

Abstract

We present the results of a high-resolution spectroscopic monitoring program of the eclipsing pre-main-sequence star KH 15D that reveal it to be a single-lined spectroscopic binary. We find that the best-fit Keplerian model has a period P=48.38 days, which is nearly identical to the photometric period. Thus, we find the best explanation for the periodic dimming of KH 15D is that the binary motion carries the currently visible star alternately above and behind the edge of an obscuring cloud. The data are consistent with the models involving an inclined circumstellar disk, as recently proposed by Winn et al. and Chiang & Murray-Clay. We show that the mass ratio expected from models of pre-main-sequence evolution, together with the mass constraints for the visible star, restrict the orbital eccentricity to 0.68<=e<=0.80 and the mass function to 0.125Msolar<=FM/sin3i<=0.5 Msolar.

Based on observations obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the Naional Aeronautics and Space Administration; at Las Campanas Observatory of the Carnegie Institution with the Magellan II Clay Telescope; and at McDonald Observatory of the University of Texas at Austin.

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