ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR BF DRACONIS
Abstract
BF Dra is now known to be an eccentric double-lined F6+F6 binary star with relatively deep (0.7 mag) partial eclipses. Previous studies of the system are improved with 7494 differential photometric observations from the URSA WebScope and 9700 from the NFO WebScope, 106 high-resolution spectroscopic observations from the Tennessee State University 2 m automatic spectroscopic telescope and the 1 m coude-feed spectrometer at Kitt Peak National Observatory, and 31 accurate radial velocities from the CfA. Very accurate (better than 0.6%) masses and radii are determined from analysis of the two new light curves and four radial velocity curves. Theoretical models match the absolute properties of the stars at an age of about 2.72 Gyr and [Fe/H] = -0.17, and tidal theory correctly confirms that the orbit should still be eccentric. Our observations of BF Dra constrain the convective core overshooting parameter to be larger than about 0.13 H{sub p}. We find, however, that standard tidal theory is unable to match the observed slow rotation rates of the components' surface layers.
- Authors:
-
- Physics Department, University of Arkansas, Fayetteville, AR 72701 (United States)
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)
- Center of Excellence in Information Systems, Tennessee State University, Nashville, TN 37209 (United States)
- Physics Department, Southern Illinois University Edwardsville, Edwardsville, IL 62026 (United States)
- Instituto de Astrofisica de Andalucia, CSIC, Apdo. Postal 3004, E-18080 Granada (Spain)
- Publication Date:
- OSTI Identifier:
- 22034456
- Resource Type:
- Journal Article
- Journal Name:
- Astronomical Journal (New York, N.Y. Online)
- Additional Journal Information:
- Journal Volume: 143; Journal Issue: 6; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 1538-3881
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTRONOMY; ASTROPHYSICS; BINARY STARS; DIAGRAMS; ECLIPSE; HYDROGEN; IRON; LAYERS; MASS; ORBITS; RADIAL VELOCITY; ROTATION; TELESCOPES; VISIBLE RADIATION
Citation Formats
Sandberg Lacy, Claud H, Torres, Guillermo, Fekel, Francis C, Sabby, Jeffrey A, and Claret, Antonio. ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR BF DRACONIS. United States: N. p., 2012.
Web. doi:10.1088/0004-6256/143/6/129.
Sandberg Lacy, Claud H, Torres, Guillermo, Fekel, Francis C, Sabby, Jeffrey A, & Claret, Antonio. ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR BF DRACONIS. United States. https://doi.org/10.1088/0004-6256/143/6/129
Sandberg Lacy, Claud H, Torres, Guillermo, Fekel, Francis C, Sabby, Jeffrey A, and Claret, Antonio. 2012.
"ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR BF DRACONIS". United States. https://doi.org/10.1088/0004-6256/143/6/129.
@article{osti_22034456,
title = {ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY STAR BF DRACONIS},
author = {Sandberg Lacy, Claud H and Torres, Guillermo and Fekel, Francis C and Sabby, Jeffrey A and Claret, Antonio},
abstractNote = {BF Dra is now known to be an eccentric double-lined F6+F6 binary star with relatively deep (0.7 mag) partial eclipses. Previous studies of the system are improved with 7494 differential photometric observations from the URSA WebScope and 9700 from the NFO WebScope, 106 high-resolution spectroscopic observations from the Tennessee State University 2 m automatic spectroscopic telescope and the 1 m coude-feed spectrometer at Kitt Peak National Observatory, and 31 accurate radial velocities from the CfA. Very accurate (better than 0.6%) masses and radii are determined from analysis of the two new light curves and four radial velocity curves. Theoretical models match the absolute properties of the stars at an age of about 2.72 Gyr and [Fe/H] = -0.17, and tidal theory correctly confirms that the orbit should still be eccentric. Our observations of BF Dra constrain the convective core overshooting parameter to be larger than about 0.13 H{sub p}. We find, however, that standard tidal theory is unable to match the observed slow rotation rates of the components' surface layers.},
doi = {10.1088/0004-6256/143/6/129},
url = {https://www.osti.gov/biblio/22034456},
journal = {Astronomical Journal (New York, N.Y. Online)},
issn = {1538-3881},
number = 6,
volume = 143,
place = {United States},
year = {Fri Jun 15 00:00:00 EDT 2012},
month = {Fri Jun 15 00:00:00 EDT 2012}
}