Magnetized quark nuggets (MQNs) are a recently proposed dark-matter candidate consistent with the Standard Model and with Tatsumi’s theory of quark-nugget cores in magnetars. Previous publications have covered their formation in the early universe, aggregation into a broad mass distribution before they can decay by the weak force, interaction with normal matter through their magnetopause, and a first observation consistent MQNs: a nearly tangential impact limiting their surface-magnetic-field parameter B_o from Tatsumi’s ~10^12+/−1 T to 1.65 × 10¹² T +/− 21%. The MQN mass distribution and interaction cross section strongly depend on B_o. Their magnetopause is much larger than their geometric dimensions and can cause sufficient energy deposition to form non-meteorite craters, which are reported approximately annually. We report computer simulations of the MQN energy deposition in water-saturated peat, soft sediments, and granite, and report the results from excavating such a crater. Five points of agreement between observations and hydrodynamic simulations of an MQN impact support this second observation being consistent with MQN dark matter and suggest a method for qualifying additional MQN events. The results also redundantly constrain B_o to ≥ 4 × 10¹¹ T.

中文翻译：

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通过径向撞击地球搜索磁化的夸克-金块暗物质的结果

磁化夸克块（MQN）是最近提出的暗物质候选对象，与标准模型以及Tatsumi的磁星中的夸克块核理论相一致。先前的出版物涵盖了它们在早期宇宙中的形成，在它们可以被弱力衰减之前聚集成广泛的质量分布，通过其磁更年期与正常物质相互作用以及首次观察到一致的MQN：几乎切线的影响限制了它们的表面磁性场参数B _o从Tatsumi的〜10 ^{12 +/- 1} T到1.65×10 ¹² T +/- 21％。MQN的质量分布和相互作用截面在很大程度上取决于B _o。它们的绝磁远大于其几何尺寸，并且可以引起足够的能量沉积以形成非陨石陨石坑，这种陨石坑大约每年都有报道。我们报告了在含水饱和泥炭，软质沉积物和花岗岩中MQN能量沉积的计算机模拟，并报告了开挖此类火山口的结果。观测与MQN冲击的流体动力学模拟之间的五个共识点支持第二次观测与MQN暗物质相一致，并提出了限定其他MQN事件的方法。结果还多余地将B _o约束为≥4×10 ^11T。