1RXS J174320.1-042953：另一个在发射线翼部具有红移吸收成分的极星
1RXS J174320.1-042953: another polar with a red-shifted absorption component in emission line wings
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中文总结 AI 辅助
对磁激变变星1RXS J174320.1-042953的光谱与多波段测光研究确认其为极星，发现发射线翼部存在红移吸收成分，源于吸积流物质穿越视线。
中文摘要 AI 辅助
我们展示了磁激变变星1RXS J174320.1-042953的光谱和多波段测光研究结果。多波段测光确认了轨道周期为$P_{\rm orb}=0.0864 \pm 0.0001$天的周期性调制。利用估计的次星质量$\sim0.15\\,\mathrm{M_\odot}$和基于X射线的白矮星质量$\sim0.75\\,\mathrm{M_\odot}$，我们得到质量比$q\sim0.2$和系统倾角$47^\circ\pm10^\circ$。1RXS J174320.1-042953的光学光谱以巴耳末系、\ion{He}{i}和\ion{He}{ii}的强、复杂、不对称且高度变化的单峰发射线为主，这是极型磁激变变星的特征。多普勒层析成像未发现开普勒吸积盘的证据，支持该系统被分类为极星。H$\beta$和\ion{He}{ii}发射线可分解为至少两个不同的成分。低速成分的半振幅分别约为170 km s$^{-1}$（H$\beta$）和147 km s$^{-1}$（\ion{He}{ii}），而高速成分分别达到约317 km s$^{-1}$和460 km s$^{-1}$。低速成分可能与面向白矮星的次星受照面及/或L$_1$点附近有关，而高速成分与吸积流结构相关。在轨道相位接近$\phi \approx 0.0$时，发射线翼部检测到红移吸收成分，速度高达$\sim1400$ km s$^{-1}$，可能由穿过视线的吸积流物质产生。
英文摘要
We present the results of a spectroscopic and multi-band photometric study of the magnetic cataclysmic variable 1RXS J174320.1-042953. Multi-band photometry confirms a periodic modulation with an orbital period of $P_{\rm orb}=0.0864 \pm 0.0001$ days. Using the estimated secondary mass of $\sim0.15\,\mathrm{M_\odot}$ and, the X-ray-based white dwarf mass of $\sim0.75\,\mathrm{M_\odot}$, we obtain values of $q\sim0.2$ and a system inclination of $47^\circ\pm10^\circ$. The optical spectra of 1RXS J174320.1-042953 are dominated by strong, complex, asymmetric, and highly variable single-peaked emission lines of the Balmer series, \ion{He}{i}, and \ion{He}{ii}, which are characteristic of polar-type magnetic cataclysmic variables. Doppler tomography reveals no evidence of a Keplerian accretion disc, supporting the classification of the system as a polar. The H$β$ and \ion{He}{ii} emission lines can be decomposed into at least two distinct components. The low-velocity components have semi-amplitudes of approximately 170 km s$^{-1}$ (H$β$) and 147 km s$^{-1}$ (\ion{He}{ii}), while the high-velocity components reach about 317 km s$^{-1}$ and 460 km s$^{-1}$, respectively. The low-velocity component is likely associated with the irradiated side of the secondary star facing the white dwarf and/or the vicinity of the L$_1$ point, whereas the high-velocity component is related to the accretion-stream structure. A redshifted absorption component in the emission-line wings is detected at orbital phases near $ϕ\approx 0.0$, reaching velocities up to $\sim1400$ km s$^{-1}$ and likely produced by accretion-stream material crossing the line of sight.
