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The outer disk of the classical Be star ψ Per

  • Robert Klement (a1) (a2), Alex C. Carciofi (a3), Thomas Rivinius (a2), Lynn D. Matthews (a4), Richard Ignace (a5), Jon E. Bjorkman (a6), Rodrigo G. Vieira (a3), Bruno C. Mota (a3), Daniel M. Faes (a3) and Stanislav Štefl...

Abstract

To this date ψ Per is the only classical Be star that was angularly resolved in radio (by the VLA at λ = 2 cm). Gaussian fit to the azimuthally averaged visibility data indicates a disk size (FWHM) of ~500 stellar radii (Dougherty & Taylor 1992). Recently, we obtained new multi-band cm flux density measurements of ψ Per from the enhanced VLA. We modeled the observed spectral energy distribution (SED) covering the interval from ultraviolet to radio using the Monte Carlo radiative transfer code HDUST (Carciofi & Bjorkman 2006). An SED turndown, that occurs between far-IR and radio wavelengths, is explained by a truncated viscous decretion disk (VDD), although the shallow slope of the radio SED suggests that the disk is not simply cut off, as is assumed in our model. The best-fit size of a truncated disk derived from the modeling of the radio SED is 100+5 −15 stellar radii, which is in striking contrast with the result of Dougherty & Taylor (1992). The reasons for this discrepancy are under investigation.

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References

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Carciofi, A.C. & Bjorkman, J.E., 2006, ApJ, 639, 1081
Dougherty, S.M. & Taylor, A.R., 1992, Nature, 359, 808
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The outer disk of the classical Be star ψ Per

  • Robert Klement (a1) (a2), Alex C. Carciofi (a3), Thomas Rivinius (a2), Lynn D. Matthews (a4), Richard Ignace (a5), Jon E. Bjorkman (a6), Rodrigo G. Vieira (a3), Bruno C. Mota (a3), Daniel M. Faes (a3) and Stanislav Štefl...

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