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Title: Photometric and Spectroscopic Observations of the Algol Type Binary V Triangle

Abstract

Time-series, multi-color photometry and high-resolution spectra of the short-period eclipsing binary V Tri were obtained through observation. The completely covered light and radial velocity (RV) curves of the binary system are presented. All times of light minima derived from both photoelectric and CCD photometry were used to calculate the orbital period and new ephemerides of the eclipsing system. The analysis of the O − C diagram reveals that the orbital period is 0.58520481 days, decreasing at a rate of dP / dt  = −7.80 × 10{sup −8} day yr{sup −1}. The mass transfer between the two components and the light-time-travel effect due to a third body could be used to explain the period decrease. However, a semi-detached configuration with the lower-mass component filling and the primary nearly filling each of their Roche lobes was derived from the synthesis of the light and RV curves by using the 2015 version of the Wilson–Devinney code. We consider the period decrease to be the nonconservative mass transfer from the secondary component to the primary and the mass loss of the system, which was thought to be an EB type, while it should be an EA type (semi-detached Algol-type) from our study. The masses, radii, and luminositiesmore » of the primary and secondary are 1.60 ± 0.07 M {sub ⊙}, 1.64 ± 0.02 R {sub ⊙}, and 14.14 ± 0.73 L {sub ⊙} and 0.74 ± 0.02 M {sub ⊙}, 1.23 ± 0.02 R {sub ⊙}, and 1.65 ± 0.05 L {sub ⊙}, respectively.« less

Authors:
; ; ; ; ;  [1];  [2];  [3];  [4]
  1. Department of Astronomy, Beijing Normal University, No. 19 Xinjiekouwai Street, Haidian District, Beijing 100875 (China)
  2. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China)
  3. Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 877, Ensenada, Baja California, C.P. 22830, México (Mexico)
  4. Physics and Space Science College, China West Normal University, Nanchong 637002 (China)
Publication Date:
OSTI Identifier:
22663631
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (New York, N.Y. Online); Journal Volume: 153; Journal Issue: 6; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BINARY STARS; CHARGE-COUPLED DEVICES; COLOR; DIAGRAMS; ECLIPSE; LUMINOSITY; MASS TRANSFER; PHOTOMETRY; RADIAL VELOCITY; RESOLUTION; ROCHE EQUIPOTENTIALS; STELLAR WINDS; SYNTHESIS; VISIBLE RADIATION

Citation Formats

Ren, A. B., Fu, J. N., Zhang, Y. P., Cang, T. Q., Li, C. Q., Khokhuntod, P., Zhang, X. B., Fox-Machado, L., and Luo, Y. P., E-mail: jnfu@bnu.edu.cn, E-mail: xzhang@bao.ac.cn. Photometric and Spectroscopic Observations of the Algol Type Binary V Triangle. United States: N. p., 2017. Web. doi:10.3847/1538-3881/AA6AF4.
Ren, A. B., Fu, J. N., Zhang, Y. P., Cang, T. Q., Li, C. Q., Khokhuntod, P., Zhang, X. B., Fox-Machado, L., & Luo, Y. P., E-mail: jnfu@bnu.edu.cn, E-mail: xzhang@bao.ac.cn. Photometric and Spectroscopic Observations of the Algol Type Binary V Triangle. United States. doi:10.3847/1538-3881/AA6AF4.
Ren, A. B., Fu, J. N., Zhang, Y. P., Cang, T. Q., Li, C. Q., Khokhuntod, P., Zhang, X. B., Fox-Machado, L., and Luo, Y. P., E-mail: jnfu@bnu.edu.cn, E-mail: xzhang@bao.ac.cn. Thu . "Photometric and Spectroscopic Observations of the Algol Type Binary V Triangle". United States. doi:10.3847/1538-3881/AA6AF4.
@article{osti_22663631,
title = {Photometric and Spectroscopic Observations of the Algol Type Binary V Triangle},
author = {Ren, A. B. and Fu, J. N. and Zhang, Y. P. and Cang, T. Q. and Li, C. Q. and Khokhuntod, P. and Zhang, X. B. and Fox-Machado, L. and Luo, Y. P., E-mail: jnfu@bnu.edu.cn, E-mail: xzhang@bao.ac.cn},
abstractNote = {Time-series, multi-color photometry and high-resolution spectra of the short-period eclipsing binary V Tri were obtained through observation. The completely covered light and radial velocity (RV) curves of the binary system are presented. All times of light minima derived from both photoelectric and CCD photometry were used to calculate the orbital period and new ephemerides of the eclipsing system. The analysis of the O − C diagram reveals that the orbital period is 0.58520481 days, decreasing at a rate of dP / dt  = −7.80 × 10{sup −8} day yr{sup −1}. The mass transfer between the two components and the light-time-travel effect due to a third body could be used to explain the period decrease. However, a semi-detached configuration with the lower-mass component filling and the primary nearly filling each of their Roche lobes was derived from the synthesis of the light and RV curves by using the 2015 version of the Wilson–Devinney code. We consider the period decrease to be the nonconservative mass transfer from the secondary component to the primary and the mass loss of the system, which was thought to be an EB type, while it should be an EA type (semi-detached Algol-type) from our study. The masses, radii, and luminosities of the primary and secondary are 1.60 ± 0.07 M {sub ⊙}, 1.64 ± 0.02 R {sub ⊙}, and 14.14 ± 0.73 L {sub ⊙} and 0.74 ± 0.02 M {sub ⊙}, 1.23 ± 0.02 R {sub ⊙}, and 1.65 ± 0.05 L {sub ⊙}, respectively.},
doi = {10.3847/1538-3881/AA6AF4},
journal = {Astronomical Journal (New York, N.Y. Online)},
number = 6,
volume = 153,
place = {United States},
year = {Thu Jun 01 00:00:00 EDT 2017},
month = {Thu Jun 01 00:00:00 EDT 2017}
}
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