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Title:
Properties of the δ Scorpii Circumstellar Disk from Continuum Modeling
Authors:
Carciofi, A. C.; Miroshnichenko, A. S.; Kusakin, A. V.; Bjorkman, J. E.; Bjorkman, K. S.; Marang, F.; Kuratov, K. S.; García-Lario, P.; Calderón, J. V. Perea; Fabregat, J.; Magalhães, A. M.
Affiliation:
AA(Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900, São Paulo, SP, Brazil ), AB(Department of Physics and Astronomy, University of North Carolina at Greensboro, P.O. Box 26170, Greensboro, NC 27402-6170; Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390.), AC(Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119992, Russia; Fesenkov Astrophysical Institute, Kamenskoe plato, Almaty 480068, Kazakhstan.), AD(Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390.), AE(Ritter Observatory, Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606-3390.), AF(South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa.), AG(Fesenkov Astrophysical Institute, Kamenskoe plato, Almaty 480068, Kazakhstan.), AH(European Space Astronomy Centre, Research and Scientific Support Department of ESA, Villafranca del Castillo, Apartado de Correos 50727, E-28080 Madrid, Spain.), AI(European Space Astronomy Centre, Villafranca del Castillo, Apartado de Correos 50727, E-28080 Madrid, Spain.), AJ(Observatorio Astronómico, Universidad de Valencia, 46100 Burjassot, Valencia, Spain.), AK(Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900, São Paulo, SP, Brazil )
Publication:
The Astrophysical Journal, Volume 652, Issue 2, pp. 1617-1625. (ApJ Homepage)
Publication Date:
12/2006
Origin:
UCP
Astronomy Keywords:
Stars: Circumstellar Matter, Methods: Numerical, Stars: Emission-Line, Be, Stars: Individual: Constellation Name: δ Scorpii, Techniques: Photometric, Techniques: Polarimetric
DOI:
10.1086/507935
Bibliographic Code:
2006ApJ...652.1617C

Abstract

We present optical WBVR and infrared JHKL photometric observations of the Be binary system δ Sco obtained in 2000-2005, and mid-infrared (10 and 18 μm) photometry and optical (λλ3200-10500) spectropolarimetry obtained in 2001. Our optical photometry confirms the results of a frequent visual monitoring being done by amateurs. The 2001 spectral energy distribution and polarization are successfully modeled with a three-dimensional non-LTE Monte Carlo code that self-consistently calculates the hydrogen level populations, electron temperature, and gas density for hot star disks. Our disk model is hydrostatically supported in the vertical direction and radially controlled by viscosity. Such a disk model has essentially only two free parameters, viz., the equatorial mass-loss rate and the disk outer radius, if one assumes a prescription for the viscosity. We find that the primary companion is surrounded by a small (7R*), geometrically-thin disk, which is highly nonisothermal and fully ionized. Our model requires an average equatorial mass-loss rate of 1.5×10-9 Msolar yr-1 to successfully explain the observations. In 2005, we detected a significant simultaneous decrease in the object's optical and near-infrared brightness, which is associated with a continuous rise in the hydrogen line equivalent widths. We discuss possible causes for this unusual phenomenon, which is difficult to explain in view of current models of Be star disks.
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