We present ALMA 1.3 mm observations of the HD~53143 debris disk - the first infrared or millimeter image produced of this ~1 Gyr-old solar-analogue. Previous HST STIS coronagraphic imaging did not detect flux along the minor axis of the disk which could suggest a face-on geometry with two 'clumps' of dust. These ALMA observations reveal a disk with a strikingly different structure. In order to fit models to the millimeter visibilities and constrain the uncertainties on the disk parameters, we adopt an MCMC approach. This is the most eccentric debris disk observed to date with a forced eccentricity of $0.21\pm0.02$, nearly twice that of the Fomalhaut debris disk, and also displays apocenter glow. Although this eccentric model fits the outer debris disk well, there are significant interior residuals remaining that may suggest a possible edge-on inner disk, which remains unresolved in these observations. Combined with the observed structure difference between HST and ALMA, these results suggest a potential previous scattering event or dynamical instability in this system. We also note that the stellar flux changes considerably over the course of our observations, suggesting flaring at millimeter wavelengths. Using simultaneous TESS observations, we determine the stellar rotation period to be $9.6\pm0.1$ days.

中文翻译：

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ALMA 成像偏心 HD 53143 碎片磁盘

我们展示了对 HD~53143 碎片盘的 ALMA 1.3 mm 观测结果——这是这个 ~1 Gyr-old 太阳模拟产生的第一张红外或毫米图像。以前的 HST STIS 日冕成像未检测到沿圆盘短轴的通量，这可能表明具有两个“团块”尘埃的正面几何形状。这些 ALMA 观测揭示了一个结构截然不同的圆盘。为了使模型适应毫米级能见度并约束磁盘参数的不确定性，我们采用了 MCMC 方法。这是迄今为止观测到的最偏心的碎片盘，强制偏心率为 $0.21\pm0.02$，几乎是北落师门碎片盘的两倍，并且还显示出远心辉光。虽然这个偏心模型很适合外部碎片盘，剩余的大量内部残差可能表明可能存在内盘边缘，在这些观察中仍未解决。结合观察到的 HST 和 ALMA 之间的结构差异，这些结果表明该系统中可能存在先前的散射事件或动态不稳定性。我们还注意到，在我们的观测过程中，恒星通量发生了很大变化，这表明在毫米波长处有耀斑。使用同时 TESS 观测，我们确定恒星自转周期为 $9.6\pm0.1$ 天。我们还注意到，在我们的观测过程中，恒星通量发生了很大变化，这表明在毫米波长处有耀斑。使用同时 TESS 观测，我们确定恒星自转周期为 $9.6\pm0.1$ 天。我们还注意到，在我们的观测过程中，恒星通量发生了很大变化，这表明在毫米波长处有耀斑。使用同时 TESS 观测，我们确定恒星自转周期为 $9.6\pm0.1$ 天。