Studies^1,2 have shown that the remnants of destroyed planets and debris-disk planetesimals can survive the volatile evolution of their host stars into white dwarfs^3,4, but few intact planetary bodies around white dwarfs have been detected^5,6,7,8. Simulations predict^9,10,11 that planets in Jupiter-like orbits around stars of ≲8 M_☉ (solar mass) avoid being destroyed by the strong tidal forces of their stellar host, but as yet, there has been no observational confirmation of such a survivor. Here we report the non-detection of a main-sequence lens star in the microlensing event MOA-2010-BLG-477Lb¹² using near-infrared observations from the Keck Observatory. We determine that this system contains a 0.53 ± 0.11 M_☉ white-dwarf host orbited by a 1.4 ± 0.3 Jupiter-mass planet with a separation on the plane of the sky of 2.8 ± 0.5 astronomical units, which implies a semi-major axis larger than this. This system is evidence that planets around white dwarfs can survive the giant and asymptotic giant phases of their host’s evolution, and supports the prediction that more than half of white dwarfs have Jovian planetary companions¹³. Located at approximately 2.0 kiloparsecs towards the centre of our Galaxy, it is likely to represent an analogue to the end stages of the Sun and Jupiter in our own Solar System.

研究^1,2表明，被摧毁的行星和碎片盘星子的残余物可以在它们的主恒星不断演变成白矮星^3,4中幸存下来，但几乎没有发现围绕白矮星的完整行星体^{5,6,7, 8} . 模拟预测^{9,10,11围绕}≲ 8  M _☉ （太阳质量）恒星的类木星轨道中的行星避免被其恒星宿主的强大潮汐力摧毁，但到目前为止，还没有观测证实这种情况一个幸存者。在这里，我们报告了在微透镜事件 MOA-2010-BLG-477Lb ^{12中未检测到主序透镜星}使用凯克天文台的近红外观测。我们确定该系统包含一个 0.53 ± 0.11  M _☉白矮星宿主，由一颗 1.4 ± 0.3 木星质量的行星绕行，在天空平面上的间隔为 2.8 ± 0.5 个天文单位，这意味着半长轴更大比这个。该系统证明白矮星周围的行星可以在其宿主演化的巨星和渐近巨星阶段幸存下来，并支持超过一半的白矮星拥有木星行星伴星的预测¹³。它位于我们银河系中心约 2.0 千秒差距处，很可能代表了我们太阳系中太阳和木星末期的类似物。