发表机构
Xinjiang Astronomical Observatory, Chinese Academy of Sciences; Instituto de Astrofísica de Andalucía - CSIC; School of Astronomy and Space Science, University of Chinese Academy of Sciences; Chinese Academy of Sciences South America Center for Astronomy（中国科学院新疆天文台; 安达卢西亚天体物理研究所-西班牙国家研究委员会; 中国科学院大学天文与空间科学学院; 中国科学院南美天文中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
通过脉动时钟的相位与频率调制分析，探测到δ Scuti双星TIC 160582982中一颗大质量不可见伴星，其质量函数暗示伴星可能为中子星或恒星质量黑洞。
AI 中文摘要
我们介绍了TIC 160582982，这是一颗具有动力学上大质量不可见伴星的偏心$\delta$ Scuti双星系统。六个相干的高频压力模被用作脉动时钟，得到了相位调制轨道，其轨道周期$P_{\rm orb}=89.29\pm0.19$天，偏心率$e=0.539^{+0.040}_{-0.037}$，以及$a_1\sin i/c=145.6^{+3.7}_{-3.4}$秒，对应$K_1=42.2^{+2.2}_{-1.8}$ km s$^{-1}$和质量函数$f(M)=0.416^{+0.032}_{-0.028}\\,M_\odot$。对两个最强模的独立频率调制分析给出了一致的轨道解。由大气参数和光谱能量分布（SED）约束的旋转MIST等时线给出$M_1=1.93\pm0.19\\,M_\odot$和$R_1=2.65\pm0.23\\,R_\odot$。质量函数暗示形式上的边缘视向最小伴星质量约为$1.80\\,M_\odot$。假设伴星是发光的在主序星，并考虑非食几何，得到$M_2=2.19^{+1.24}_{-0.34}\\,M_\odot$和轨道倾角$i=61.5^{+16.6}_{-19.6}$度。然而，无论是在光度上还是光谱上，都没有发现存在发光对应体的明确证据。这表明伴星可能是一个大质量致密天体，例如中子星甚至恒星质量黑洞，作为大质量不可见双星伴星。未来的相位分辨高分辨率光谱观测对于获得独立的轨道约束并澄清伴星的性质至关重要。
英文摘要
We present TIC 160582982, an eccentric $δ$ Scuti binary with a dynamically massive unseen companion. Six coherent high-frequency pressure modes used as pulsation clocks yield a phase-modulation orbit with $P_{\rm orb}=89.29\pm0.19$ d, $e=0.539^{+0.040}_{-0.037}$, and $a_1\sin i/c=145.6^{+3.7}_{-3.4}$ s, corresponding to $K_1=42.2^{+2.2}_{-1.8}$ km s$^{-1}$ and $f(M)=0.416^{+0.032}_{-0.028}\,M_\odot$. An independent frequency-modulation analysis of the two strongest modes gives a consistent orbital solution. Rotating MIST isochrones constrained by the atmospheric parameters and spectral energy distribution (SED) give $M_1=1.93\pm0.19\,M_\odot$ and $R_1=2.65\pm0.23\,R_\odot$. The mass function implies a formal edge-on minimum companion mass of approximately $1.80\,M_\odot$. Assuming a luminous main-sequence companion and including the non-eclipsing geometry gives $M_2=2.19^{+1.24}_{-0.34}\,M_\odot$ and $i=61.5^{+16.6}_{-19.6}$ deg. However, no clear evidence for the presence of a luminous counterpart is found, either photometrically or spectroscopically. This suggests the presence of a massive compact object, such as a neutron star or even a stellar-mass black hole, as the massive unseen binary companion. Future phase-resolved high-resolution spectroscopy will be crucial for obtaining an independent orbital constraint and clarifying the nature of the companion.
Comments14 pages, 6 figures. Accepted for publication in The Astrophysical Journal
