通过高频率测光锐化PSR J1048+2339的质量测量
Sharpening the Mass Measurement of PSR J1048+2339 via High-Cadence Photometry
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- National Cheng Kung University（国立成功大学）
- Chungnam National University（忠南国立大学）
- National Tsing Hua University（国立清华大学）
- Huazhong University of Science and Technology（华中科技大学）
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中文总结 AI 辅助
通过小口径望远镜的高频率光学测光观测脉冲星双星PSR J1048+2339，利用掩食约束轨道倾角和脉冲星质量，实现了对红背系统的高精度质量测量，并估计了伴星磁场强度。
中文摘要 AI 辅助
中子星是宇宙中最致密的天体之一，其质量测量对于理解它们的物态方程至关重要。在紧密双星系统中的脉冲星可以通过动力学方法称重，但精确的质量估计常常受到轨道倾角不确定性的阻碍。本文报告了使用鹿林天文台0.5米RIFT望远镜对脉冲星双星系统PSR J1048+2339进行的多历元光学监测。我们的观测揭示了频繁的光学耀发以及由伴星引起的掩食。利用掩食持续时间、档案测光数据和文献中的轨道星历表，我们将轨道倾角约束为78.0±1.0度，脉冲星质量约束为1.79（+0.09，-0.08）太阳质量。这一测量是迄今为止对任何红背系统最精确的测量之一，展示了使用小口径光学望远镜改进脉冲星质量测量的新颖方法。此外，光学掩食持续时间显著短于在M/GeV伽马射线中测量的持续时间，这可能表明被掩食的伽马射线发射的一部分起源于双星内激波的顶点。基于这些约束，我们估计伴星的磁场强度为30-170高斯。这与观测到的X射线轨道调制所暗示的高场强一致。
英文摘要
Neutron stars are among the densest objects in the universe, and the mass measurements are crucial to the understanding of their equation of state. Pulsars in tight binaries can be weighed dynamically, but accurate mass estimates are often hampered by uncertainties in orbital inclinations. In this paper, we report on multi-epoch optical monitoring of the pulsar binary, PSR J1048+2339, using the 0.5-m RIFT telescope at Lulin Observatory. Our observations reveal frequent optical flares with eclipses caused by the companion. Using the eclipse duration with archival photometric data and orbital ephemeris in the literature, we constrain the inclination to 78.0+/-1.0 degrees and the pulsar mass to 1.79 (+0.09, -0.08) solar masses. This measurement is among the most precise for any redback system to date, demonstrating a novel way to improve the pulsar mass measures with small aperture optical telescopes. Furthermore, the optical eclipse duration is significantly shorter than that measured in M/GeV gamma-rays, possibly suggesting that a fraction of the eclipsed gamma-ray emission originates from the apex of the intrabinary shock. Based on these constraints, we estimate the magnetic field strength of the companion to be 30-170 G. This is consistent with the high field strength implied by the X-ray orbital modulation observed.
