In this paper we test if the ∼0.3–15 keV XMM-Newton EPIC pn spectral continuum of IPs can be described by the thermal Comptonization compTT model. We used publicly observations of 12 IPs (AE Aqr, EX Hya, V1025 Cen, V2731 Oph, RX J2133.7+5107, PQ Gem, NY Lup, V2400 Oph, IGR J00234+6141, IGR J17195-4100, V1223 Sgr, and XY Ari). We find that our modeling is capable of fitting well the average spectral continuum of these sources. In this framework, UV/soft X-ray seed photons (with 〈kT _s〉 of 0.096 0.013 keV) coming presumably from the star surface are scattered off by electrons present in an optically thick plasma (with 〈kT _e〉 of 3.05 0.16 keV and optical depth 〈τ〉 of 9.5 0.6 for plane geometry) located nearby (on top) to the more central seed photon emission regions. A soft blackbody (bbody) component is observed in 5 out of the 13 observations analyzed, with a mean temperature 〈kT _bb 〉 of 0.095 0.004 keV. We observed that the spectra of IPs show in general two photon indices Γ, which are driven by the source luminosity and optical depth. Low luminosity IPs show 〈Γ〉 of 1.83 0.19, whereas high luminosity IPs show lower 〈Γ〉 of 1.34 0.02. Moreover, the good spectral fits of PQ Gem and V2400 Oph indicate that the polar subclass of CVs may be successfully described by the thermal Comptonization as well.

在本文中，我们测试了 0.3-15 keV XMM-Newton EPIC pn 连续谱 IP 是否可以通过热补偿compTT模型来描述。我们使用了 12 个 IP 的公开观察结果（AE Aqr、EX Hya、V1025 Cen、V2731 Oph、RX J2133.7+5107、PQ Gem、NY Lup、V2400 Oph、IGR J00234+6141、IGR J17195-412230、 XY 阿里）。我们发现我们的建模能够很好地拟合这些源的平均光谱连续体。在这个框架中，可能来自恒星表面的UV/软 X 射线种子光子（< kT _s > 为 0.096 0.013 keV）被光学厚等离子体中存在的电子散射掉（< kT _e > 为 3.05 0.16 keV和光学深度< τ＞ 9.5 0.6（对于平面几何）位于更中心的种子光子发射区域附近（顶部）。在分析的 13 个观测中的 5 个中观测到软黑体 ( bbody ) 分量，平均温度 < kT _bb > 为 0.095 0.004 keV。我们观察到 IP 的光谱通常显示两个光子指数 Γ，它们由源光度和光学深度驱动。低光度 IP 显示 <Γ> 为 1.83 0.19，而高光度 IP 显示较低的 <Γ> 为 1.34 0.02。此外，PQ Gem 和 V2400 Oph 的良好光谱拟合表明 CV 的极性子类也可以通过热补偿成功地描述。