PSR J0435+3233 三星系统
The PSR J0435+3233 Triple System
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中文总结 AI 辅助
本研究证认PSR J0435+3233为特殊的分层三星系统，通过多波段数据拟合确定其内外轨道参数与天体质量，为研究原始三星系统演化提供了独特样本。
中文摘要 AI 辅助
三星系统的详细演化过程复杂且尚不明确。基于光学/红外与伽马射线存档数据，我们证认了脉冲星 PSR J0435+3233 是一个处于分层三星系统中的伽马射线脉冲星，其近距内双星伴星为一颗氦白矮星（WD），远距第三伴星为一颗类太阳恒星。PSR J0435+3233 与 WD 伴星构成周期 $P_{\rm orb1}=8$ 天、偏心率 $e=0.00016$ 的圆轨道；第三伴星为 G 型亚巨星，质量为 $0.98(12) M_\bigodot$，距地球 $2.1(4)$ 千秒差距。通过同时拟合 PSR J0435+3233 16.7 年的伽马射线自旋周期变化、4.6 年的射电自旋周期变化、内轨道参数变化、夏皮罗延迟、盖亚天体测量数据及外伴星质量，我们确定了第三伴星的外椭圆轨道，其周期 $P_{\rm orb2}\backsim26900$ 天，偏心率 $e_2=0.5983$。外轨道要么与内轨道近乎垂直（互倾角约 $84^\text{o}$），要么呈现约 $55^\text{o}$ 的中等互倾角。对于前者几何构型，脉冲星、WD、第三伴星的质量分别为 $1.15^{+0.06}_{-0.04} M_\bigodot$、$0.271^{+0.010}_{-0.006} M_\bigodot$、$0.96(4) M_\bigodot$；对于后者几何构型，对应质量分别为 $1.29^{+0.14}_{-0.11} M_\bigodot$、$0.296^{+0.022}_{-0.018} M_\bigodot$、$1.12^{+0.06}_{-0.05} M_\bigodot$。该三星系统是开展多波段观测、研究原始三星系统演化路径与动力学过程的独特天体，最终将演化为包含一颗中子星和两颗白矮星的系统。
英文摘要
The detailed evolution of triple star systems is complicated and poorly known. Using archived optical/infrared and $γ$-ray data, we identified the pulsar PSR~J0435+3233 as a $γ$-ray pulsar in a hierarchical triple system, with a helium white dwarf (WD) as a close inner binary companion and a Sun-like star as the distant tertiary. PSR~J0435+3233 and the WD companion are in a circular orbit with a period of $P_{\rm orb1} = 8.0$~days and an eccentricity of $e=0.00016$. The tertiary is a G-type subgiant with a mass of $0.98(12)\, M_\odot$ at a distance of $2.1(4)$\, kpc from the Earth. By simultaneously fitting the observed spin-period variations of the $γ$-ray emission (over 16.7 years) and radio emission (over 4.9 years) from PSR~J0435+3233, the changes in the inner orbital parameters, the Shapiro delay, Gaia astrometry, and the outer companion mass, we determined the outer elliptical orbit for the tertiary, with a period $P_{\rm orb2} = 73.5$~yrs and an eccentricity $e_2 = 0.598$. The outer orbit is either nearly perpendicular to the inner orbit with a mutual inclination of $\sim 85^\circ$, or moderately inclined by $\sim 54^\circ$. For the former geometry, the pulsar, the WD, and the tertiary star have masses of $1.16(5)\, M_\odot$, $0.273(8)\, M_\odot$, and $0.91(5)\, M_\odot$, respectively; for the latter geometry, the corresponding masses are $1.34(15)\, M_\odot$, $0.305(23)\, M_\odot$, and $1.13(7)\, M_\odot$. This is a unique triple system for detailed multi-band observations and for studying the evolutionary path and dynamic processes of a primordial triple star system. It will ultimately evolve into a system consisting of a neutron star and two white dwarfs.
发表机构
- National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
- School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）
- State Key Laboratory of Radio Astronomy and Technology（射电天文与技术国家重点实验室）
- Institute for Astronomy, School of Physics, Zhejiang University（浙江大学物理学院天体物理研究所）
- International Center of Supernovae (ICESUN), Yunnan Key Laboratory of Supernova Research, Yunnan Observatories, Chinese Academy of Sciences (CAS)（中国科学院云南天文台超新星国际研究中心（ICESUN）、云南省超新星研究重点实验室）
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