发表机构
South African Astronomical Observatory; Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Capodimonte; Department of Physics, University of the Free State; National Astronomical Observatories, Chinese Academy of Sciences; CRESST II and X-ray Astrophysics Laboratory, NASA/GSFC; Department of Physics, University of Maryland, Baltimore County; Institute of Space Sciences (ICE, CSIC); School of Physics and Astronomy, University of Southampton; Centre for Extragalactic Astronomy, Department of Physics, Durham University; Istituto Nazionale di Astrofisica, Osservatorio di Astrofisica（南非天文台; 意大利国家天体物理研究所卡波迪蒙特天文台; 自由大学物理系; 中国科学院国家天文台; NASA/戈达德太空飞行中心 CRESST II 与 X射线天体物理实验室; 马里兰大学巴尔的摩分校物理系; 空间科学研究所（CSIC）; 南安普顿大学物理与天文学学院; 杜伦大学物理系河外天文研究中心; 意大利国家天体物理研究所天体物理观测站）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究基于 XMM-Newton 和 TESS 数据，首次详细分析了中间偏振星 Swift J0614.0+1709 的 X 射线与光学辐射，确认其自转周期约 1411 秒，揭示能量依赖的 X 射线脉冲及复杂光学变化，并指出其为高光度源，为后续多波段研究提供重要目标。
AI 中文摘要
我们基于一次指向性 XMM-Newton 观测，并结合 TESS 的长期光学测光，首次对中间偏振星 Swift J0614.0+1709 进行了详细的 X 射线与光学研究。在 X 射线中探测到周期约为 1411 秒的白矮星自转周期的强相干调制，证实了该系统的磁性本质。X 射线自转脉冲表现出显著的能量依赖性，调制幅度随能量升高而减小，这与吸积流中的相位相关吸收一致。相位分辨光谱进一步表明，自转变异性主要由部分覆盖吸收体的覆盖分数变化驱动。宽带 X 射线光谱可由部分吸收的热等离子体模型很好地描述，其温度约为 12 keV，并包含一个温度约为 63 eV 的软黑体成分。推断的辐射光度约为 5×10^34 erg s^-1，使该源跻身于较明亮的中间偏振星之列。TESS 观测揭示了轨道调制与自转调制相对强度的扇区间显著变化。虽然自转信号始终占主导地位，但拍频调制变化显著，并在一个扇区中完全消失，这表明再处理区域的贡献随时间变化。轨道调制幅度（以及较小程度上的自转调制幅度）在较亮的光学状态下有增强的趋势，表明质量转移率的变化可能影响光学辐射和调制幅度。总体而言，Swift J0614.0+1709 是一颗相对 X 射线明亮的中间偏振星，表现出复杂的光学变异性，其特征是脉冲形态的变化和重复的增亮事件，使其成为未来同步光学与 X 射线研究的宝贵目标。
英文摘要
We present the first detailed X-ray and optical study of the intermediate polar Swift J0614.0+1709 based on a pointed XMM-Newton observation complemented by long-term optical photometry from TESS. A strong coherent modulation at the white dwarf spin period was detected in X-rays, with a period of $\sim$1411 s, confirming the magnetic nature of the system. The X-ray spin pulse exhibits a pronounced energy dependence, with the modulation amplitude decreasing towards higher energies, consistent with phase-dependent absorption in the accretion flow. Phase-resolved spectroscopy further shows that the spin variability is primarily driven by changes in the covering fraction of the partial-covering absorber. The broadband X-ray spectrum is well described by a partially absorbed thermal plasma model with a temperature of $\sim$12 keV and a soft blackbody component at $\sim$63 eV. The inferred bolometric luminosity of $\sim$5$\times$10$^{34}$ erg s$^{-1}$ places the source among the more luminous intermediate polars. The TESS observations reveal substantial sector-to-sector variability in the relative strengths of the orbital and spin modulations. While the spin signal remains persistently dominant, the beat modulation varies significantly and disappears entirely in one Sector, suggesting temporal changes in the contribution of the reprocessing region(s). The orbital and, to a lesser extent, spin modulation amplitudes show some tendency to be stronger during brighter optical states, suggesting that changes in the mass transfer rate may influence the optical emission and modulation amplitudes. Overall, Swift J0614.0+1709 is a comparatively X-ray luminous intermediate polar exhibiting complex optical variability characterised by changes in pulse morphology and recurrent brightening events, making it a valuable target for future simultaneous optical and X-ray studies.
Comments16 pages, 10 figures, accepted for publication in A&A
DOI：10.1051/0004-6361/202661437
