极地的回旋加速器建模相分辨红外光谱学III：AM Herculis和ST Leo Minoris
Cyclotron Modeling Phase-Resolved Infrared Spectroscopy of Polars III: AM Herculis and ST Leo Minoris
摘要：
我们提出了相位分辨低分辨率红外光谱的AM Her和ST LMi，两个低场极化，我们观察到的DAC上的IRTF。光学/近红外光变曲线也被公布，以帮助限制观察时物体的几何形状和亮度。目前，只有有限的红外光谱已公布的这些对象，并没有与相位覆盖在这里提出。在这两种情况下，所产生的光谱都是由近红外光谱中的二级恒星的辐射所主导的。然而，发射区域也是自掩的，允许我们通过减去暗相位谱来分离回旋辐射。我们使用“恒定λ”处方来模拟结果数据中看到的不断变化的回旋特征。对于AM Her，我们找到最佳拟合模型：B = 13.6 MG，kT = 4.0 keV，logLambda = 5.0。回旋加速器导出的吸积几何形状与50度的轨道倾角和85度的磁共纬度是一致的。对于ST LMi，B = 12.1 MG，kT = 3.3 keV，logLambda = 5.7，轨道倾角为55度，磁同纬度为128度。
英文摘要：
We present phase-resolved low resolution infrared spectra of AM Her and ST LMi, two low-field polars that we observed with SPEX on the IRTF. Optical/NIR lightcurves are also published to help constrain the viewing geometry and brightness of the objects at the time they were observed. Currently, only limited IR spectra have been published for these objects, and none with the phase-coverage presented here. In both cases, the resulting spectra are dominated by emission from the secondary star in the NIR. However, the emission regions are also self-eclipsed, allowing us to isolate the cyclotron emission through subtraction of the dim-phase spectrum. We use a ``Constant Lambda'' prescription to model the changing cyclotron features seen in the resulting data. For AM Her, we find a best fit model of: B = 13.6 MG, kT = 4.0 keV, and logLambda = 5.0. The cyclotron derived accretion geometry is consistent with an orbital inclination of 50 degrees and a magnetic co-latitude of 85 degrees. For ST LMi, B = 12.1 MG, kT = 3.3 keV, and logLambda = 5.7 with an orbital inclination of 55 degrees and a magnetic co-latitude of 128 degrees.
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