GALEX和WX LMi、SDSSJ103100 .5+202832.2和SDSSJ121209 .31+013627.7的光学光变曲线
GALEX and Optical Light Curves of WX LMi, SDSSJ103100.5+202832.2 and SDSSJ121209.31+013627.7
摘要：
三个极低吸积率极星的{ \it GALEX}近紫外（NUV）和远紫外（FUV）光变曲线显示出明显的紫外光变曲线调制。虽然这三个系统的磁场范围从13到70 MG，并且是晚型秒速（包括SDSSJ 121209.31 +013627.7中可能存在的棕矮星），但吸积速率是相似的，并且紫外线观测暗示某些机制正在运行以在白矮星上创建增强的发射区。UV变化在相位上与WX LMi中光学观察到的两个磁极相匹配，并且与SDSSJ 1212109.31 +013627.7和SDSSJ 103100.55 +202832.2中光学观察到的单极相匹配。紫外光变曲线的简单点模型表明，如果热点是造成紫外变化的原因，那么温度大约在10，000 - 14，000 K之间。对于单极系统，FUV光斑的尺寸必须小于NUV，并且在所有情况下，几何形状可能比简单的圆形光斑更复杂。
英文摘要：
{\it GALEX} near ultraviolet (NUV) and far-ultraviolet (FUV) light curves of three extremely low accretion rate polars show distinct modulations in their UV light curves. While these three systems have a range of magnetic fields from 13 to 70 MG, and of late type secondaries (including a likely brown dwarf in SDSSJ121209.31+013627.7), the accretion rates are similar, and the UV observations imply some mechanism is operating to create enhanced emission zones on the white dwarf. The UV variations match in phase to the two magnetic poles viewed in the optical in WX LMi and to the single poles evident in the optical in SDSSJ1212109.31+013627.7 and SDSSJ103100.55+202832.2. Simple spot models of the UV light curves show that if hot spots are responsible for the UV variations, the temperatures are on the order of 10,000-14,000K. For the single pole systems, the size of the FUV spot must be smaller than the NUV and in all cases, the geometry is likely more complicated than a simple circular spot.
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