Comparing Jupiter's equatorial X-ray emissions with solar X-ray flux over 19 years of the Chandra mission
Comparing Jupiter's equatorial X-ray emissions with solar X-ray flux over 19 years of the Chandra mission
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钱德拉任务 19 年来木星赤道 X 射线发射与太阳 X 射线通量的比较
DOI：
10.1002/essoar.10512649.2
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发表时间：
2022
期刊：
影响因子：
--
通讯作者：
McEntee S
中科院分区：
文献类型：
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作者：
McEntee S
我们利用钱德拉X射线天文台（CXO） 19年的观测数据对木星盘X射线发射进行了统计研究。先前的研究表明，这些辐射与从木星上层大气中弹性散射的太阳X射线一致。我们展示了一种新的脉冲不变量（PI）滤波方法，该方法可以最大限度地减少仪器效应，这些仪器效应可能会在近20年的观测期间产生光子计数的非物理趋势。我们将CXO的结果与地球静止运行环境卫星X射线传感器的波长波段1-8 Å（长通道）的太阳X射线通量数据进行比较，以量化太阳活动与木星盘数之间的相关性。我们发现统计上显著的Pearson相关系数为0.9，这证实了发射的木星盘X射线主要受太阳活动的控制。我们还利用CXO上的高分辨率相机的高空间分辨率来绘制圆盘光子在木星表面的位置。通过覆盖朱诺参考模型和Perijove 9内部场模型，构建了Voronoi镶嵌图，以识别赤道光子的空间偏好。在考虑了行星曲面的面积和散射后，我们发现木星的圆盘发射在2-3.5高斯的表面磁场强度下是优先的。这表明磁盘X射线的一部分可能与太阳散射以外的过程有关：与磁场强度相关的空间偏好可能意味着来自辐射带的降水增加，正如先前假设的那样。
We present a statistical study of Jupiter’s disk X‐ray emissions using 19 years of Chandra X‐Ray Observatory (CXO) observations. Previous work has suggested that these emissions are consistent with solar X‐rays elastically scattered from Jupiter’s upper atmosphere. We showcase a new pulse invariant (PI) filtering method that minimizes instrumental effects which may produce unphysical trends in photon counts across the nearly two‐decade span of the observations. We compare the CXO results with solar X‐ray flux data from the Geostationary Operational Environmental Satellites X‐ray Sensor for the wavelength band 1–8 Å (long channel), to quantify the correlation between solar activity and Jovian disk counts. We find a statistically significant Pearson’s Correlation Coefficient of 0.9, which confirms that emitted Jovian disk X‐rays are predominantly governed by solar activity. We also utilize the high spatial resolution of the High Resolution Camera Instrument on‐board the CXO to map the disk photons to their positions on Jupiter’s surface. Voronoi tessellation diagrams were constructed with the Juno Reference Model through Perijove 9 internal field model overlaid to identify any spatial preference of equatorial photons. After accounting for area and scattering across the curved surface of the planet, we find a preference of Jovian disk emission at 2–3.5 Gauss surface magnetic field strength. This suggests that a portion of the disk X‐rays may be linked to processes other than solar scattering: the spatial preference associated with magnetic field strength may imply increased precipitation from the radiation belts, as previously postulated.