Abstract

Based on data from the ZTF photometric survey, we have revealed asynchrony of the polar SDSS J085414.02+390537.3. A beat period \(P_{\textrm{beat}}=24.6\pm 0.1\) days, during which the system changes its brightness by \({\approx}3^{m}\), is distinguished in the light curves. Power peaks at the white-dwarf rotation period \(P_{\textrm{spin}}=113.197\pm 0.001\) min and orbital period \(P_{\textrm{orb}}=113.560\pm 0.001\) min are revealed in the periodograms, with the corresponding polar asynchrony being \(1-P_{\textrm{orb}}/P_{\textrm{spin}}=0.3{\%}\). The photometric behavior of the polar points to a change of the main accreting pole during the beat period. Based on the Zeeman splitting of the H\(\beta\) line, we have estimated the mean magnetic field strength of the white dwarf to be \(B=28.5\pm 1.5\) MG. The magnetic field strength near the magnetic pole has been found by modeling the cyclotron spectra to be \(B=34\pm 2\) MG. The Doppler tomograms in the H\(\beta\) line exhibit a distribution of emission sources typical for polars in velocity space with evidence of the transition of the accretion stream from the ballistic trajectory to the magnetic one.

中文翻译：

---

SDSS J085414.02+390537.3—新型异步极性

摘要

根据ZTF光度测量数据，我们揭示了极地SDSS J085414.02+390537.3的异步性。在光变曲线中可以区分节拍周期\(P_{\textrm{beat}}=24.6\pm 0.1\)天，在此期间系统的亮度变化\({\approx}3^{m}\)。白矮星自转周期\(P_{\textrm{spin}}=113.197\pm 0.001\) min 和轨道周期\(P_{\textrm{orb}}=113.560\pm 0.001\) min 处的功率峰值被揭示在周期图中，相应的极异步为\(1-P_{\textrm{orb}}/P_{\textrm{spin}}=0.3{\%}\)。极点的光度行为表明主吸积极在拍频期间发生了变化。根据 H \(\beta\)线的塞曼分裂，我们估算出白矮星的平均磁场强度为\(B=28.5\pm 1.5\) MG。通过将回旋加速器谱建模为\(B=34\pm 2\) MG 可以得到磁极附近的磁场强度。H \(\beta\)线中的多普勒断层图显示了速度空间中极地典型的发射源分布，并有吸积流从弹道轨迹过渡到磁轨迹的证据。