Spectral energy distributions of be and other massive stars

Y. Touhami; N. D. Richardson; D. R. Gies; G. H. Schaefer; T. S. Boyajian; S. J. Williams; E. D. Grundstrom; M. V. Mcswain; D. P. Clemens; B. Taylor

doi:10.1086/652009

Spectral energy distributions of be and other massive stars

Y. Touhami^*, N. D. Richardson, D. R. Gies, G. H. Schaefer, T. S. Boyajian, S. J. Williams, E. D. Grundstrom, M. V. Mcswain, D. P. Clemens, B. Taylor

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

20 Citations (Scopus)

Abstract

We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high-angular-resolution interferometric observations to model the density structure and sky orientation of the gas surrounding these stars. We also present a montage of the Hα and near-infrared emission lines that form in Be star disks. We find that a simplified measurement of the IR excess flux appears to be correlated with the strength of emission lines from high level transitions of hydrogen. This suggests that the near-IR continuum and upper level line fluxes both form in the inner part of the disk, close to the star.

Original language	English
Pages (from-to)	379-395
Number of pages	17
Journal	Publications of the Astronomical Society of the Pacific
Volume	122
Issue number	890
DOIs	https://doi.org/10.1086/652009
Publication status	Published - Apr 2010
Externally published	Yes

Access to Document

10.1086/652009

Cite this

@article{b7f08c0066bc41c68707701956af7956,

title = "Spectral energy distributions of be and other massive stars",

abstract = "We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high-angular-resolution interferometric observations to model the density structure and sky orientation of the gas surrounding these stars. We also present a montage of the Hα and near-infrared emission lines that form in Be star disks. We find that a simplified measurement of the IR excess flux appears to be correlated with the strength of emission lines from high level transitions of hydrogen. This suggests that the near-IR continuum and upper level line fluxes both form in the inner part of the disk, close to the star.",

author = "Y. Touhami and Richardson, {N. D.} and Gies, {D. R.} and Schaefer, {G. H.} and Boyajian, {T. S.} and Williams, {S. J.} and Grundstrom, {E. D.} and Mcswain, {M. V.} and Clemens, {D. P.} and B. Taylor",

year = "2010",

month = apr,

doi = "10.1086/652009",

language = "English",

volume = "122",

pages = "379--395",

journal = "Publications of the Astronomical Society of the Pacific",

issn = "0004-6280",

publisher = "Institute of Physics Publishing",

number = "890",

}

TY - JOUR

T1 - Spectral energy distributions of be and other massive stars

AU - Touhami, Y.

AU - Richardson, N. D.

AU - Gies, D. R.

AU - Schaefer, G. H.

AU - Boyajian, T. S.

AU - Williams, S. J.

AU - Grundstrom, E. D.

AU - Mcswain, M. V.

AU - Clemens, D. P.

AU - Taylor, B.

PY - 2010/4

Y1 - 2010/4

N2 - We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high-angular-resolution interferometric observations to model the density structure and sky orientation of the gas surrounding these stars. We also present a montage of the Hα and near-infrared emission lines that form in Be star disks. We find that a simplified measurement of the IR excess flux appears to be correlated with the strength of emission lines from high level transitions of hydrogen. This suggests that the near-IR continuum and upper level line fluxes both form in the inner part of the disk, close to the star.

AB - We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high-angular-resolution interferometric observations to model the density structure and sky orientation of the gas surrounding these stars. We also present a montage of the Hα and near-infrared emission lines that form in Be star disks. We find that a simplified measurement of the IR excess flux appears to be correlated with the strength of emission lines from high level transitions of hydrogen. This suggests that the near-IR continuum and upper level line fluxes both form in the inner part of the disk, close to the star.

UR - http://www.scopus.com/inward/record.url?scp=77950352500&partnerID=8YFLogxK

U2 - 10.1086/652009

DO - 10.1086/652009

M3 - Article

AN - SCOPUS:77950352500

SN - 0004-6280

VL - 122

SP - 379

EP - 395

JO - Publications of the Astronomical Society of the Pacific

JF - Publications of the Astronomical Society of the Pacific

IS - 890

ER -

Spectral energy distributions of be and other massive stars

Abstract

Access to Document

Other files and links

Fingerprint

Cite this