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Title: Photometric properties for selected Algol-type binaries. VI. The newly discovered oEA star FR Orionis

Abstract

New photometry of the neglected eclipsing binary FR Orionis was obtained in 2012 November and December. Using the updated Wilson-Devinney program, the photometric elements were deduced from two-color light curves. The results indicate that this system is a semi-detached binary, with a mass ratio of 0.325(± 0.002) and a fill-out factor of the primary of f{sub p} = 73.5(± 0.2)%. The oscillating light curves imply that FR Ori may be an oscillating EA (oEA)-type star with a rapidly pulsating, mass-accreting primary component. After we removed the theoretical light curves from the observations, Fourier analysis revealed that the more massive component possibly shows a δ Scuti type pulsation with four detected frequencies. The dominant frequency is f {sub 1} = 38.6c day{sup –1} (i.e., P {sub puls} = 37.3 minutes), and the pulsation constant is Q = 0.014 days. Based on all available eclipsing times, the orbital period is undergoing a secular period increase with a rate of dP/dt = +8.85(±0.66) × 10{sup –8} day yr {sup –1}, which may be interpreted by mass transfer from the secondary to the primary. We expect that the more massive component will fill its Roche lobe due to mass transfer of the secondary. Therefore,more » the oEA star FR Ori may evolve into a contact configuration.« less

Authors:
 [1];
  1. School of Physics and Electronic Information, Huaibei Normal University, 235000 Huaibei, Anhui Province (China)
Publication Date:
OSTI Identifier:
22340018
Resource Type:
Journal Article
Journal Name:
Astronomical Journal (New York, N.Y. Online)
Additional Journal Information:
Journal Volume: 147; Journal Issue: 2; 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; BINARY STARS; COLOR; DIAGRAMS; ECLIPSE; FOURIER ANALYSIS; GALAXIES; MASS TRANSFER; PHOTOMETRY; PULSATIONS; ROCHE EQUIPOTENTIALS; STARS; VISIBLE RADIATION

Citation Formats

Yang, Y. -G., Wei, J. -Y., and Li, H.-L., E-mail: yygcn@163.com. Photometric properties for selected Algol-type binaries. VI. The newly discovered oEA star FR Orionis. United States: N. p., 2014. Web. doi:10.1088/0004-6256/147/2/35.
Yang, Y. -G., Wei, J. -Y., & Li, H.-L., E-mail: yygcn@163.com. Photometric properties for selected Algol-type binaries. VI. The newly discovered oEA star FR Orionis. United States. https://doi.org/10.1088/0004-6256/147/2/35
Yang, Y. -G., Wei, J. -Y., and Li, H.-L., E-mail: yygcn@163.com. 2014. "Photometric properties for selected Algol-type binaries. VI. The newly discovered oEA star FR Orionis". United States. https://doi.org/10.1088/0004-6256/147/2/35.
@article{osti_22340018,
title = {Photometric properties for selected Algol-type binaries. VI. The newly discovered oEA star FR Orionis},
author = {Yang, Y. -G. and Wei, J. -Y. and Li, H.-L., E-mail: yygcn@163.com},
abstractNote = {New photometry of the neglected eclipsing binary FR Orionis was obtained in 2012 November and December. Using the updated Wilson-Devinney program, the photometric elements were deduced from two-color light curves. The results indicate that this system is a semi-detached binary, with a mass ratio of 0.325(± 0.002) and a fill-out factor of the primary of f{sub p} = 73.5(± 0.2)%. The oscillating light curves imply that FR Ori may be an oscillating EA (oEA)-type star with a rapidly pulsating, mass-accreting primary component. After we removed the theoretical light curves from the observations, Fourier analysis revealed that the more massive component possibly shows a δ Scuti type pulsation with four detected frequencies. The dominant frequency is f {sub 1} = 38.6c day{sup –1} (i.e., P {sub puls} = 37.3 minutes), and the pulsation constant is Q = 0.014 days. Based on all available eclipsing times, the orbital period is undergoing a secular period increase with a rate of dP/dt = +8.85(±0.66) × 10{sup –8} day yr {sup –1}, which may be interpreted by mass transfer from the secondary to the primary. We expect that the more massive component will fill its Roche lobe due to mass transfer of the secondary. Therefore, the oEA star FR Ori may evolve into a contact configuration.},
doi = {10.1088/0004-6256/147/2/35},
url = {https://www.osti.gov/biblio/22340018}, journal = {Astronomical Journal (New York, N.Y. Online)},
issn = {1538-3881},
number = 2,
volume = 147,
place = {United States},
year = {Sat Feb 01 00:00:00 EST 2014},
month = {Sat Feb 01 00:00:00 EST 2014}
}