Mass transfer and tidally tilted pulsation in the Algol-type system TZ Dra

Author:

Kahraman Aliçavuş F12ORCID,Handler G3,Aliçavuş F12,De Cat P4ORCID,Bedding T R56ORCID,Lampens P4,Ekinci Ö12,Gümüș D7,Leone F89

Affiliation:

1. Faculty of Sciences and Arts, Physics Department, Çanakkale Onsekiz Mart University, 17100 Canakkale, Turkey

2. Astrophysics Research Center and Ulupınar Observatory, Çanakkale Onsekiz Mart University, TR-17100 Canakkale, Turkey

3. Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, PL-00-716 Warsaw, Poland

4. Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussel, Belgium

5. Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Camperdown NSW 2006, Australia

6. Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

7. Institute of Graduate Studies in Science, Programme of Astronomy and Space Sciences, Istanbul University, 34116 Beyazit, Istanbul, Turkey

8. Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Universita di Catania, Via S. Sofia 78, I-95123 Catania, Italy

9. INAF, Osservatorio Astrofisico di Catania, Via S. Sofia 78, I-95123 Catania, Italy

Abstract

ABSTRACT Oscillating eclipsing Algols (oEAs) are remarkable systems that allow us to determine accurate fundamental stellar parameters (mass, radius) and probe the stellar interiors through pulsations. TZ Dra is an oEA system containing a δ Scuti component. To examine particular characteristics of such close systems including pulsations and mass transfer, we present a detailed photometric and spectroscopic study of TZ Dra. With the analysis of high-resolution spectra, the orbital parameters were determined by the radial velocity analysis and the atmospheric parameters were derived for the primary component. The binary modelling and the pulsational frequency analysis was carried out using the Transiting Exoplanet Survey Satellite data set. The H α line profiles show the signature of mass transfer from the cool to the hot binary component. The conclusion of mass transfer/mass-loss in the system was supported by the analysis of the orbital period changes. As a result, it was found that there is $3.52 \times 10^{-9}\, {\rm M}_\odot$ yr−1 mass-loss from the system most probably through the hotspot and stellar winds. Additionally, most pulsation frequencies originating from the primary component were found to be spaced by harmonics of the orbital frequencies in particular, 12 doublets spaced by 2forb were detected from which we infer that this star is a tidally tilted pulsator. A mean p-mode frequency spacing of ≈7.2 d−1 was found as well.

Funder

NCN

Istanbul University

Australian Research Council

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

Cited by 11 articles. 订阅此论文施引文献 订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献

同舟云学术

1.学者识别学者识别

2.学术分析学术分析

3.人才评估人才评估

"同舟云学术"是以全球学者为主线,采集、加工和组织学术论文而形成的新型学术文献查询和分析系统,可以对全球学者进行文献检索和人才价值评估。用户可以通过关注某些学科领域的顶尖人物而持续追踪该领域的学科进展和研究前沿。经过近期的数据扩容,当前同舟云学术共收录了国内外主流学术期刊6万余种,收集的期刊论文及会议论文总量共计约1.5亿篇,并以每天添加12000余篇中外论文的速度递增。我们也可以为用户提供个性化、定制化的学者数据。欢迎来电咨询!咨询电话:010-8811{复制后删除}0370

www.globalauthorid.com

TOP

Copyright © 2019-2024 北京同舟云网络信息技术有限公司
京公网安备11010802033243号  京ICP备18003416号-3