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Title: AN INTERFEROMETRIC AND SPECTROSCOPIC ANALYSIS OF THE MULTIPLE STAR SYSTEM HD 193322

Abstract

The star HD 193322 is a remarkable multiple system of massive stars that lies at the heart of the cluster Collinder 419. Here we report on new spectroscopic observations and radial velocities of the narrow-lined component Ab1 which we use to determine its orbital motion around a close companion Ab2 (P = 312 days) and around a distant third star Aa (P = 35 years). We have also obtained long baseline interferometry of the target in the K' band with the CHARA Array which we use in two ways. First, we combine published speckle interferometric measurements with CHARA separated fringe packet measurements to improve the visual orbit for the wide Aa,Ab binary. Second, we use measurements of the fringe packet from Aa to calibrate the visibility of the fringes of the Ab1,Ab2 binary, and we analyze these fringe visibilities to determine the visual orbit of the close system. The two most massive stars, Aa and Ab1, have masses of approximately 21 and 23 M{sub sun}, respectively, and their spectral line broadening indicates that they represent extremes of fast and slow projected rotational velocity, respectively.

Authors:
; ;  [1]
  1. Center for High Angular Resolution Astronomy, Georgia State University, Mt. Wilson, CA 91023 (United States)
Publication Date:
OSTI Identifier:
21583057
Resource Type:
Journal Article
Journal Name:
Astronomical Journal (New York, N.Y. Online)
Additional Journal Information:
Journal Volume: 142; Journal Issue: 1; Other Information: DOI: 10.1088/0004-6256/142/1/21; Journal ID: ISSN 1538-3881
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; INTERFEROMETRY; LINE BROADENING; ORBITS; RADIAL VELOCITY; STAR EVOLUTION; STARS; EVOLUTION; VELOCITY

Citation Formats

Ten Brummelaar, Theo A., Farrington, Christopher D., and Schaefer, Gail H., E-mail: theo@chara-array.org, E-mail: farrington@chara-array.org, E-mail: schaefer@chara-array.org. AN INTERFEROMETRIC AND SPECTROSCOPIC ANALYSIS OF THE MULTIPLE STAR SYSTEM HD 193322. United States: N. p., 2011. Web. doi:10.1088/0004-6256/142/1/21.
Ten Brummelaar, Theo A., Farrington, Christopher D., & Schaefer, Gail H., E-mail: theo@chara-array.org, E-mail: farrington@chara-array.org, E-mail: schaefer@chara-array.org. AN INTERFEROMETRIC AND SPECTROSCOPIC ANALYSIS OF THE MULTIPLE STAR SYSTEM HD 193322. United States. doi:10.1088/0004-6256/142/1/21.
Ten Brummelaar, Theo A., Farrington, Christopher D., and Schaefer, Gail H., E-mail: theo@chara-array.org, E-mail: farrington@chara-array.org, E-mail: schaefer@chara-array.org. Fri . "AN INTERFEROMETRIC AND SPECTROSCOPIC ANALYSIS OF THE MULTIPLE STAR SYSTEM HD 193322". United States. doi:10.1088/0004-6256/142/1/21.
@article{osti_21583057,
title = {AN INTERFEROMETRIC AND SPECTROSCOPIC ANALYSIS OF THE MULTIPLE STAR SYSTEM HD 193322},
author = {Ten Brummelaar, Theo A. and Farrington, Christopher D. and Schaefer, Gail H., E-mail: theo@chara-array.org, E-mail: farrington@chara-array.org, E-mail: schaefer@chara-array.org},
abstractNote = {The star HD 193322 is a remarkable multiple system of massive stars that lies at the heart of the cluster Collinder 419. Here we report on new spectroscopic observations and radial velocities of the narrow-lined component Ab1 which we use to determine its orbital motion around a close companion Ab2 (P = 312 days) and around a distant third star Aa (P = 35 years). We have also obtained long baseline interferometry of the target in the K' band with the CHARA Array which we use in two ways. First, we combine published speckle interferometric measurements with CHARA separated fringe packet measurements to improve the visual orbit for the wide Aa,Ab binary. Second, we use measurements of the fringe packet from Aa to calibrate the visibility of the fringes of the Ab1,Ab2 binary, and we analyze these fringe visibilities to determine the visual orbit of the close system. The two most massive stars, Aa and Ab1, have masses of approximately 21 and 23 M{sub sun}, respectively, and their spectral line broadening indicates that they represent extremes of fast and slow projected rotational velocity, respectively.},
doi = {10.1088/0004-6256/142/1/21},
journal = {Astronomical Journal (New York, N.Y. Online)},
issn = {1538-3881},
number = 1,
volume = 142,
place = {United States},
year = {2011},
month = {7}
}