Zobrazeno 1 - 10
of 94
pro vyhledávání: '"Min-Yu Li"'
We model the TESS light curve of the binary system RX Dra, and also first calculate a lot of theoretical models to fit the g-mode frequencies previously detected from the TESS series of this system. The mass ratio is determined to be $q$=0.9026$^{+0.
Externí odkaz:
http://arxiv.org/abs/2405.15940
Autor:
Jia‐Qi Zhu, Han Wu, Xu Li, Min‐Yu Li, Zhen‐Li Li, Xin‐Fei Xu, Li‐Hui Gu, Dong‐Xu Yin, Feng Shen, Dong‐Sheng Huang, Tian Yang
Publikováno v:
Advanced Science, Vol 11, Iss 9, Pp n/a-n/a (2024)
Abstract Hepatocellular carcinoma (HCC) is acknowledged as an immunosuppressive neoplasm, whereby the inactive microenvironment facilitates immune tolerance and evasion of HCC. Post‐surgical resected liver cancer exhibits a proclivity for relapse,
Externí odkaz:
https://doaj.org/article/9069476f636a464499dd41f7cd6f3aaa
Autor:
Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun
Publikováno v:
The Astrophysical Journal, Vol 974, Iss 2, p 278 (2024)
Heartbeat stars (HBSs) with tidally excited oscillations (TEOs) are ideal astrophysical laboratories for studying the internal properties of the systems. In this paper, five new HBSs exhibiting TEOs are discovered using TESS photometric data. The orb
Externí odkaz:
https://doaj.org/article/de5c8261c3f34223b93d2cd43a2c93ba
Publikováno v:
The Astrophysical Journal, Vol 974, Iss 1, p 132 (2024)
Tilted disk precession exists in different objects. Negative superhumps (NSHs) in cataclysmic variable stars are believed to arise from the interaction between the reverse precession of a tilted disk and the streams from the secondary star. Utilizing
Externí odkaz:
https://doaj.org/article/040d5bb943854e40beb46238abce0734
Autor:
Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Fu-Xing Li, Xiang-Dong Shi, Min-Yu Li
Publikováno v:
The Astrophysical Journal, Vol 966, Iss 1, p 83 (2024)
TV Col is a long-period eclipsing intermediate polar (IP) prototype star for the negative superhump (NSH) system. We investigate the eclipse minima, eclipse depth, and NSH amplitude based on TESS photometry. Using the same analytical method as for SD
Externí odkaz:
https://doaj.org/article/d7f0538c7065424daf47ad5952b20c29
Autor:
Qi-Bin Sun, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Fu-Xing Li, Xiang-Dong Shi, Min-Yu Li
Publikováno v:
The Astrophysical Journal, Vol 962, Iss 2, p 123 (2024)
Negative superhumps (NSHs) are signals a few percent shorter than the orbital period of a binary star and are considered to originate from the reverse precession of the tilted disk. Based on TESS photometry, we find nine new cataclysmic variable star
Externí odkaz:
https://doaj.org/article/666b12549b004977946a640519c922a0
Autor:
Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Publikováno v:
The Astrophysical Journal, Vol 962, Iss 1, p 44 (2024)
Heartbeat stars (HBSs) with tidally excited oscillations (TEOs) are ideal laboratories for studying the effect of equilibrium and dynamical tides. However, studies of TEOs in Kepler HBSs are rare due to the need for better modeling of the equilibrium
Externí odkaz:
https://doaj.org/article/ea1543c292c044c98fef3f10a486ab8e
Publikováno v:
ACS Omega, Vol 6, Iss 25, Pp 16410-16418 (2021)
Externí odkaz:
https://doaj.org/article/3d7fe57d62964d14bf2ed24edf16904e
Autor:
Fu-Xing Li, Sheng-Bang Qian, Chu-Qi Wu, Min-Yu Li, Er-Gang Zhao, Wen-Ping Liao, Li-Ying Zhu, Qi-Bin Sun, Jia Zhang
Publikováno v:
The Astrophysical Journal, Vol 956, Iss 1, p 49 (2023)
Massive contact binaries refer to the close binary systems in which the components have filled their respective Roche lobes and share a common envelope with early-type spectra. Twin binaries are a special type of binary system characterized by two co
Externí odkaz:
https://doaj.org/article/8c0124a256d24623b343475dcbf6b1c5
Publikováno v:
The Astrophysical Journal, Vol 955, Iss 2, p 135 (2023)
AH Her is a Z Cam-type dwarf nova with an orbital period of ∼0.258 days. Dwarf nova oscillations and long-period dwarf nova oscillations have been detected, but no quasiperiodic oscillations (QPOs) and negative superhumps (NSHs) have been found. We
Externí odkaz:
https://doaj.org/article/6519e9de762945a8b350fbf75a26c842