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优先级 40　·　高能暂现天体　·　引力波电磁对应体

Gardening on the Moon: An Advection-Diffusion Model to Guide the Search for Supernova Debris in the Lunar Regolith

月球翻耕：指导在月壤中搜寻超新星碎屑的平流-扩散模型

✉ Emily S. Costello (Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa), John Ellis (Theoretical Particle Physics and Cosmology Group, Department of Physics, King’s College London; Theoretical Physics Department, CERN), Brian D. Fields (Department of Astronomy, University of Illinois) et al.

原文摘要Abstract

The vertical redistribution of materials in the lunar regolith—ranging from continuously produced space-weathering products to sporadic pulses of supernova- or kilonova-derived isotopes—remains a fundamental problem in planetary science. We present a unified stochastic model of regolith gardening induced by the impact flux. Treating gardening as a competition between impact-driven advection and diffusion predicts the maturity profiles of Apollo cores over more than 2 orders of magnitude in time (<inline-formula><mml:math><mml:mrow><mml:mn>1.4</mml:mn><mml:mo>×</mml:mo><mml:msup><mml:mrow><mml:mn>10</mml:mn></mml:mrow><mml:mrow><mml:mn>7</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> to <inline-formula><mml:math><mml:mrow><mml:mn>4.5</mml:mn><mml:mo>×</mml:mo><mml:msup><mml:mrow><mml:mn>10</mml:mn></mml:mrow><mml:mrow><mml:mn>8</mml:mn></mml:mrow></mml:msup><mml:mtext> </mml:mtext><mml:mtext> </mml:mtext><mml:mi>yr</mml:mi></mml:mrow></mml:math></inline-formula>). This model describes well the depth profiles of live <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Fe</mml:mi></mml:mrow><mml:mrow><mml:mn>60</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula> in Apollo regolith samples, suggesting that supernova dust capture is independent of native iron abundance, and is consistent with a uniform influx at the latitudes of the Apollo landing sites. We extend our model to predict lunar signals for live <inline-formula><mml:math><mml:mrow><mml:mi>r</mml:mi></mml:mrow></mml:math></inline-formula>-process species that might originate from supernovae or kilonovae: <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Pu</mml:mi></mml:mrow><mml:mrow><mml:mn>244</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula> tied to terrestrial detections, and <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>I</mml:mi></mml:mrow><mml:mrow><mml:mn>129</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula>, <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Hf</mml:mi></mml:mrow><mml:mrow><mml:mn>182</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula>, and <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Cm</mml:mi></mml:mrow><mml:mrow><mml:mn>247</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula> based on <inline-formula><mml:math><mml:mrow><mml:mi>r</mml:mi></mml:mrow></mml:math></inline-formula>-process calculations. The <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Pu</mml:mi></mml:mrow><mml:mrow><mml:mn>244</mml:mn></mml:mrow></mml:mmultiscripts><mml:mo>/</mml:mo><mml:mmultiscripts><mml:mrow><mml:mi>Fe</mml:mi></mml:mrow><mml:mrow><mml:mn>60</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula> depth profile can probe the origin of <inline-formula><mml:math><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi>Pu</mml:mi></mml:mrow><mml:mrow><mml:mn>244</mml:mn></mml:mrow></mml:mmultiscripts></mml:mrow></mml:math></inline-formula>, motivating searches in Artemis regolith samples down to depths <inline-formula><mml:math><mml:mrow><mml:mi>O</mml:mi><mml:mo>(</mml:mo><mml:mn>100</mml:mn><mml:mo>)</mml:mo><mml:mtext> </mml:mtext><mml:mtext> </mml:mtext><mml:mi>cm</mml:mi></mml:mrow></mml:math></inline-formula>.

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AI 综述 AI-generated · 以原文为准

亮点

将撞击 gardening 首次统一为平流-扩散解析模型，并用 Apollo 成熟度和 Fe-60 剖面双重验证；提出 Pu-244/Fe-60 深度比值可区分近邻超新星与持续/更早 r-过程来源，为 Artemis 采样深度提供定量依据。

脉络与展望

自 Ellis+ 1996 提出近邻超新星可在月球留下 Fe-60 等活同位素、并由 Knie+ 1999 在深海证实以来，月壤成为独立记录站；但经典月壤翻耕模型多把混合视为纯扩散 Gault+ 1974，难以解释 Apollo 剖面中的尖锐梯度。本文将 Costello+ 2021 的次级撞击埋藏-挖掘几何升级为质量守恒的 ADE，成功复现成熟度与 Fimiani+ 2016 的 Fe-60 剖面，并与 Wallner+ 2021 深海 Pu-244/Fe-60 约束衔接。随后扩展 Wang+ 2023 的月球 r-过程核素测量思路，预测 Pu-244、I-129、Hf-182、Cm-247 深度分布。展望上，该 ADE 方法可推广至月球挥发分与 He-3，Artemis 更深岩心和南极点采样有望通过纬度杠杆及深部 Pu-244/Fe-60 比值区分超新星/千新星来源。

预印本 2026-04-10 · 刊出 2026-08-14 · 收录 2026-08-22

ADS:2026PhRvL.137g1005C ↗arXiv:2604.09524 ↗DOI ↗

边缘相关 1 篇 · 低相关性展开＋

优先级 20　·　引力波电磁对应体　·　多信使触发与联合09-06 补录

Gravitational memory from hairy binary black hole mergers

Gasparotto, Silvia, Zosso, Jann, Saló, Llibert Aresté, et al.

原文摘要Abstract

Gravitational-wave memory is a low-frequency, nonoscillatory component of the radiation field that provides a potentially powerful but as yet undetected probe of strong-field gravity. We present the first calculation of gravitational memory from full inspiral-merger-ringdown waveforms in a theory beyond general relativity, focusing on scalar-Gauss-Bonnet gravity as a theoretically well-motivated and numerically accessible extension of GR. Starting from the general memory formulas in Horndeski gravity, we derive explicit spin-weighted spherical-harmonic expressions for the tensor null memory in scalar-Gauss-Bonnet theory and evaluate them on existing numerical-relativity waveforms for both shift-symmetric and dynamically scalarizing binary black hole mergers. We find that the dominant effect is an indirect modification of the tensor memory through changes in the nonlinear merger dynamics, while the direct scalar contribution to the tensor memory remains suppressed by orders of magnitude for the systems considered in this work. For the largest deviations in our dataset, the final memory amplitude differs from the corresponding GR prediction by a few percent and by up to <inline-formula><mml:math><mml:mrow><mml:mo>~</mml:mo><mml:mn>4</mml:mn><mml:mo>%</mml:mo></mml:mrow></mml:math></inline-formula> when compared to the GR template that minimizes the waveform mismatch in a detector-oriented analysis. We further show that including memory increases the mismatch between GR and scalar-Gauss-Bonnet waveforms by more than an order of magnitude, indicating that memory can provide complementary information for testing gravity with third-generation detectors, especially for low-mass binaries.

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带毛黑洞并合产生的引力记忆　·　本文首次在标量-高斯-博内引力中计算了完整旋近-并合-铃宕波形的引力记忆，发现主要效应来自非线性并合动力学对张量记忆的间接修正，直接标量贡献被压制，但记忆可显著增大与广义相对论的波形失配，为第三代探测器检验引力提供补充信息。

预印本 2026-04-10 · 刊出 2026-08-26 · 收录 2026-09-06

ADS:2026PhRvD.114d4094G ↗arXiv:2604.09350 ↗DOI ↗