Hostname: page-component-77c89778f8-sh8wx Total loading time: 0 Render date: 2024-07-21T04:23:22.022Z Has data issue: false hasContentIssue false

The outer disk of the classical Be star ψ Per

Published online by Cambridge University Press:  28 July 2017

Robert Klement
Affiliation:
Astronomical Institute of Charles University, Charles University, V Holešovičkách 2, 180 00, Prague 8, Czech Republic, email: robertklement@gmail.com European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago, Chile
Alex C. Carciofi
Affiliation:
Instituto de Astronomia, Geofíisica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo, Brazil
Thomas Rivinius
Affiliation:
European Southern Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, Santiago, Chile
Lynn D. Matthews
Affiliation:
MIT Haystack Observatory, off Route 40, Westford MA 01886, USA
Richard Ignace
Affiliation:
Department of Physics & Astronomy, East Tennessee State University, Johnson City, TN 37614, USA
Jon E. Bjorkman
Affiliation:
Ritter Observatory, Department of Physics & Astronomy, University of Toledo, Toledo, OH 43606, USA
Rodrigo G. Vieira
Affiliation:
Instituto de Astronomia, Geofíisica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo, Brazil
Bruno C. Mota
Affiliation:
Instituto de Astronomia, Geofíisica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo, Brazil
Daniel M. Faes
Affiliation:
Instituto de Astronomia, Geofíisica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, 05508-090, São Paulo, Brazil
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

References

Carciofi, A.C. & Bjorkman, J.E., 2006, ApJ, 639, 1081 Google Scholar
Dougherty, S.M. & Taylor, A.R., 1992, Nature, 359, 808 CrossRefGoogle Scholar