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arXiv 2107.09005astro-ph.SRastro-ph.HE
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轨道偏心率的发现和SS433轨道周期增大的证据

Discovery of orbital Eccentricity and Evidence for orbital Period Increase of SS433

A. M. Cherepashchuk, A. A. Belinski, A. V. Dodin, K. A. Postnov

备注：
5 pages, 4 figures + Appendix. Accepted for publication in MNRAS Letters
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摘要：

对SS 433的长期（1979-2020）测光观测的检验使我们能够发现$e=0.05\pm 0.01.$的非零轨道偏心率。我们还发现了轨道周期以$\dot P_\mathrm{b}=(1.0\pm0.3)\times10^{-7}$ s s $^{-1}$的速率长期增加的证据。双星轨道周期增加率使得有可能改进双星质量比$q=M_\mathrm{X}/M_\mathrm{V}>0.8$的估计，其中$M_\mathrm{X}$和$M_\mathrm{V}$分别是相对论天体和光学星的质量。对于质量为10 ${\rm M}_\odot$的光学恒星，相对论性物体（黑洞）的质量是$M_\mathrm{X}>8{\rm M}_\odot$。SS 433中的中子星被可靠地排除在外，因为在这种情况下，轨道周期应该会减少，这与观测结果相矛盾。$\dot P_\mathrm{b}$的导出值设定了来自二进制系统$\gtrsim 7\times 10^{-6} {\rm M}_\odot\mathrm{yr}^{-1}$的Jeans模式中的质量损失率的下限。发现的SS 433轨道椭圆率与从动吸积盘跟踪未对准光学恒星旋转轴的进动的模型一致。

英文摘要：

The examination of long-term (1979-2020) photometric observations of SS433 enabled us to discover a non-zero orbital eccentricity of $e=0.05\pm 0.01.$ We have also found evidence for a secular increase in the orbital period at a rate of $\dot P_\mathrm{b}=(1.0\pm0.3)\times10^{-7}$ s s$^{-1}$. The binary orbital period increase rate makes it possible to improve the estimate of the binary mass ratio $q=M_\mathrm{X}/M_\mathrm{V}>0.8$, where $M_\mathrm{X}$ and $M_\mathrm{V}$ are the masses of the relativistic object and the optical star, respectively. For an optical star mass of 10${\rm M}_\odot$, the mass of the relativistic object (a black hole) is $M_\mathrm{X}>8{\rm M}_\odot$. A neutron star in SS433 is reliably excluded because in that case the orbital period should decrease, in contradiction to observations. The derived value of $\dot P_\mathrm{b}$ sets a lower limit on the mass-loss rate in the Jeans mode from the binary system $\gtrsim 7\times 10^{-6} {\rm M}_\odot\mathrm{yr}^{-1}$. The discovered orbital ellipticity of SS433 is consistent with the model of the slaved accretion disc tracing the precession of the misaligned optical star's rotational axis.

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