近地小行星主要源自主帶小行星，其演化過程是透過亞爾科夫斯基效應與平均運動共振的共同作用所驅動。熱漂移將小行星推入共振區域，隨後引力攝動會放大其軌道離心率，進而產生穿越火星軌道的路徑並注入近地小行星區域。本次研究探討瑪利亞星小行星家族成員的長期軌道演化，該星族為部位於強烈的 3:1 木星平均運動共振附近的主帶星族。我們透過對所選瑪利亞星族成員的克卜勒軌道要素進行數值積分，並追蹤其從主帶進入內太陽系軌道的動力學路徑。我們的模擬證實，與 3:1 平均運動共振的相互作用會大幅增加離心率（$e$），從而高效地驅動天體穿越火星軌道並進入近地小行星空間。至關重要的是，數值積分結果揭示了部分逃逸成員經歷了極端的軌道傾角（$i$）激發，超過 $90^\circ$ 並從順行運動轉變為逆行運動。我們分析了這些劇烈的傾角倒轉究竟是與高偏心率階段解耦，抑或是由高偏心率階段所驅動（例如在共振內部透過古薩-利多夫機制所致）。此外，我們也將這些由動力學產生的逆行天體與本質上即擁有逆行軌道的小行星進行了比較。這些結果表明，瑪利亞星族不僅是典型順行近地小行星的來源，同時也是不尋常的高傾角或逆行近地天體的源頭。透過繪製 3:1 平均運動共振附近偏心率激增與傾角驟升之間的耦合關係，也在本次研究為共振輸送機制以及內太陽系極端傾角天體的起源提供了關鍵見解。;Near-Earth Asteroids (NEAs) predominantly originate from Main-Belt Asteroids (MBAs) through the combined action of the Yarkovsky effect and mean-motion resonances (MMRs). Thermal drift pushes asteroids into resonant regions， where gravitational perturbations amplify eccentricities， leading to Mars-crossing trajectories and NEA injection. This study investigates the long-term orbital evolution of members of the Maria family， a main-belt family situated near the strong 3:1 Jupiter MMR. By numerically integrating the Keplerian elements of selected Maria members， we trace their dynamical pathways from the main belt into inner Solar System orbits.
Our simulations confirm that interaction with the 3:1 MMR dramatically increases eccentricity ($e$)， efficiently driving objects across the Martian orbit and into NEA space. Crucially， the integrations reveal that a subset of escaping members undergoes extreme inclination ($i$) excitation， exceeding $90^\circ$ and transitioning from prograde to retrograde motion. We analyze whether these dramatic inclination inversions are decoupled from or driven by high-eccentricity phases， such as through Kozai-Lidov dynamics within the resonance. Furthermore， we compare these dynamically generated retrograde bodies with asteroids that possess intrinsically retrograde orbits.
These results demonstrate that the Maria family serves as a source for both typical prograde NEAs and unusual， high-inclination or retrograde Near-Earth Objects. By mapping the coupling between eccentricity pump-up and inclination spikes near the 3:1 MMR， this work offers key insights into resonant transport mechanisms and the origin of extreme-inclination bodies in the inner Solar System.
