Orbital Dynamics of Candidate Transitional Millisecond Pulsar 3FGL J1544.6-1125: An Unusually Face-on System
Orbital Dynamics of Candidate Transitional Millisecond Pulsar 3FGL J1544.6-1125: An Unusually Face-on System
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DOI：
10.3847/1538-4357/aa8e41
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发表时间：
2017-09
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通讯作者：
C. Britt;J. Strader;L. Chomiuk;E. Tremou;M. Peacock;J. Halpern;Ricardo Salinas Center for Data Intensive;Time Domain Astronomy;D. Physics;Astronomy;M. University;Columbia Astrophysics Laboratory;C. University;Gemini Observatory
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作者：
C. Britt;J. Strader;L. Chomiuk;E. Tremou;M. Peacock;J. Halpern;Ricardo Salinas Center for Data Intensive;Time Domain Astronomy;D. Physics;Astronomy;M. University;Columbia Astrophysics Laboratory;C. University;Gemini Observatory
本文给出了过渡毫秒脉冲星（tMSP）3FGL J1544.6-1125的施主星星的轨道解。其轨道周期为天，完全符合施主星星作为中晚期K矮星的光谱分类。径向速度曲线的半振幅在km/s−1处异常低，意味着在5°-8°范围内有显著的正面倾角，这取决于中子星星和施主质量。在确定了二次星系的面纱之后，我们得出了它与双星的距离为3.8 ± 0.7 kpc，产生了0.3-10 keV的X射线光度，与确认的tMSP相似。由于正面双星很少偶然发生，我们讨论了费米选择的过渡毫秒双星样品在亚发光盘状态的可能性受到光束。通过对光谱星历上的发射线强度进行定相，我们发现了相干变化，并认为这些变化与源自内盘附近的非对称激波的发射最一致。
We present the orbital solution for the donor star of the candidate transitional millisecond pulsar (tMSP) 3FGL J1544.6-1125, currently observed as an accreting low-mass X-ray binary. The orbital period is days, entirely consistent with the spectral classification of the donor star as a mid-to-late K dwarf. The semi-amplitude of the radial velocity curve is exceptionally low at km s−1, implying a remarkably face-on inclination in the range 5°–8°, depending on the neutron star and donor masses. After determining the veiling of the secondary, we derive a distance to the binary of 3.8 ± 0.7 kpc, yielding a 0.3–10 keV X-ray luminosity of , similar to confirmed tMSPs. As face-on binaries rarely occur by chance, we discuss the possibility that Fermi-selected samples of transitional millisecond pulsars in the sub-luminous disk state are affected by beaming. By phasing emission line strength on the spectroscopic ephemeris, we find coherent variations, and argue that these variations are most consistent with emission from an asymmetric shock originating near the inner disk.