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Title: Pulsations and period changes of the non-Blazhko RR lyrae variable Y oct observed from Dome A, Antarctica

Abstract

During the operation of the Chinese Small Telescope Array (CSTAR) in Dome A of Antarctica in the years 2008, 2009, and 2010, large amounts of photometric data have been obtained for variable stars in the CSTAR field. We present here the study of one of six RR Lyrae variables, Y Oct, observed with CSTAR in Dome A, Antarctica. Photometric data in the i band were obtained in 2008 and 2010, with a duty cycle (defined as the fraction of time representing scientifically available data to CSTAR observation time) of about 44% and 52%, respectively. In 2009, photometric data in the g and r bands were gathered for this star, with a duty cycle of 65% and 60%, respectively. Fourier analysis of the data in the three bands only shows the fundamental frequency and its harmonics, which is characteristic of the non-Blazhko RR Lyrae variables. Values of the fundamental frequency and the amplitudes, as well as the total pulsation amplitude, are obtained from the data in the three bands separately. The amplitude of the fundamental frequency and the total pulsation amplitude in the g band are the largest, and those in the i band the smallest. Two-hundred fifty-one times of maximummore » are obtained from the three seasons of data, which are analyzed together with 38 maximum times provided in the GEOS RR Lyrae database. A period change rate of −0.96 ± 0.07 days Myr{sup −1} is then obtained, which is a surprisingly large negative value. Based on relations available in the literature, the following physical parameters are derived: [Fe/H] = −1.41 ± 0.14, M{sub V} = 0.696 ± 0.014 mag, V−K = 1.182 ± 0.028 mag, logT{sub eff} = 3.802 ± 0.003 K, logg = 2.705 ± 0.004, logL/L{sub ⊙} = 1.625 ± 0.013, and logM/M{sub ⊙} = −0.240 ± 0.019.« less

Authors:
; ; ; ;  [1]; ;  [2]; ; ;  [3]; ; ; ; ; ; ; ;  [4];  [5];  [6]
  1. Department of Astronomy, Beijing Normal University, Beijing 100875 (China)
  2. Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A and M University, College Station, TX (United States)
  3. School of Physics, University of New South Wales, NSW (Australia)
  4. Chinese Center for Antarctic Astronomy, Nanjing (China)
  5. Center for Astrophysics, Lawrence Berkeley National Laboratory, Berkeley, CA (United States)
  6. Department of Astronomy and Astrophysics and Enrico Fermi Institute, University of Chicago, Chicago, IL (United States)
Publication Date:
OSTI Identifier:
22342159
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (New York, N.Y. Online); Journal Volume: 149; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; AMPLITUDES; ANTARCTICA; DATA; FOURIER ANALYSIS; HARMONICS; OPERATION; PHOTOMETRY; PULSATIONS; SEASONS; TELESCOPES; VARIABLE STARS

Citation Formats

Zhihua, Huang, Jianning, Fu, Weikai, Zong, Lingzhi, Wang, Zonghong, Zhu, M, Macri Lucas, Lifan, Wang, Ashley, Michael C. B., S, Lawrence Jon, Daniel, Luong-Van, Xiangqun, Cui, Long-Long, Feng, Xuefei, Gong, Qiang, Liu, Huigen, Yang, Xiangyan, Yuan, Xu, Zhou, Zhenxi, Zhu, R, Pennypacker Carl, and G, York Donald, E-mail: jnfu@bnu.edu.cn. Pulsations and period changes of the non-Blazhko RR lyrae variable Y oct observed from Dome A, Antarctica. United States: N. p., 2015. Web. doi:10.1088/0004-6256/149/1/25.
Zhihua, Huang, Jianning, Fu, Weikai, Zong, Lingzhi, Wang, Zonghong, Zhu, M, Macri Lucas, Lifan, Wang, Ashley, Michael C. B., S, Lawrence Jon, Daniel, Luong-Van, Xiangqun, Cui, Long-Long, Feng, Xuefei, Gong, Qiang, Liu, Huigen, Yang, Xiangyan, Yuan, Xu, Zhou, Zhenxi, Zhu, R, Pennypacker Carl, & G, York Donald, E-mail: jnfu@bnu.edu.cn. Pulsations and period changes of the non-Blazhko RR lyrae variable Y oct observed from Dome A, Antarctica. United States. doi:10.1088/0004-6256/149/1/25.
Zhihua, Huang, Jianning, Fu, Weikai, Zong, Lingzhi, Wang, Zonghong, Zhu, M, Macri Lucas, Lifan, Wang, Ashley, Michael C. B., S, Lawrence Jon, Daniel, Luong-Van, Xiangqun, Cui, Long-Long, Feng, Xuefei, Gong, Qiang, Liu, Huigen, Yang, Xiangyan, Yuan, Xu, Zhou, Zhenxi, Zhu, R, Pennypacker Carl, and G, York Donald, E-mail: jnfu@bnu.edu.cn. Thu . "Pulsations and period changes of the non-Blazhko RR lyrae variable Y oct observed from Dome A, Antarctica". United States. doi:10.1088/0004-6256/149/1/25.
@article{osti_22342159,
title = {Pulsations and period changes of the non-Blazhko RR lyrae variable Y oct observed from Dome A, Antarctica},
author = {Zhihua, Huang and Jianning, Fu and Weikai, Zong and Lingzhi, Wang and Zonghong, Zhu and M, Macri Lucas and Lifan, Wang and Ashley, Michael C. B. and S, Lawrence Jon and Daniel, Luong-Van and Xiangqun, Cui and Long-Long, Feng and Xuefei, Gong and Qiang, Liu and Huigen, Yang and Xiangyan, Yuan and Xu, Zhou and Zhenxi, Zhu and R, Pennypacker Carl and G, York Donald, E-mail: jnfu@bnu.edu.cn},
abstractNote = {During the operation of the Chinese Small Telescope Array (CSTAR) in Dome A of Antarctica in the years 2008, 2009, and 2010, large amounts of photometric data have been obtained for variable stars in the CSTAR field. We present here the study of one of six RR Lyrae variables, Y Oct, observed with CSTAR in Dome A, Antarctica. Photometric data in the i band were obtained in 2008 and 2010, with a duty cycle (defined as the fraction of time representing scientifically available data to CSTAR observation time) of about 44% and 52%, respectively. In 2009, photometric data in the g and r bands were gathered for this star, with a duty cycle of 65% and 60%, respectively. Fourier analysis of the data in the three bands only shows the fundamental frequency and its harmonics, which is characteristic of the non-Blazhko RR Lyrae variables. Values of the fundamental frequency and the amplitudes, as well as the total pulsation amplitude, are obtained from the data in the three bands separately. The amplitude of the fundamental frequency and the total pulsation amplitude in the g band are the largest, and those in the i band the smallest. Two-hundred fifty-one times of maximum are obtained from the three seasons of data, which are analyzed together with 38 maximum times provided in the GEOS RR Lyrae database. A period change rate of −0.96 ± 0.07 days Myr{sup −1} is then obtained, which is a surprisingly large negative value. Based on relations available in the literature, the following physical parameters are derived: [Fe/H] = −1.41 ± 0.14, M{sub V} = 0.696 ± 0.014 mag, V−K = 1.182 ± 0.028 mag, logT{sub eff} = 3.802 ± 0.003 K, logg = 2.705 ± 0.004, logL/L{sub ⊙} = 1.625 ± 0.013, and logM/M{sub ⊙} = −0.240 ± 0.019.},
doi = {10.1088/0004-6256/149/1/25},
journal = {Astronomical Journal (New York, N.Y. Online)},
number = 1,
volume = 149,
place = {United States},
year = {Thu Jan 01 00:00:00 EST 2015},
month = {Thu Jan 01 00:00:00 EST 2015}
}