本論文以Chyba（1990）由月球隕石坑所得的碰撞歷史，以及Melosh與Vickery（1989）對大氣演化的模型為基礎，並加以改良，重新建構太陽系內各行星或衛星受到LHBE影響的模型。
而泰坦是太陽系內除了火星外，我們很有興趣的一顆衛星，因為它濃厚的N2大氣層與今日的地球頗為相似，泰坦是否成為下一個可能有生命存在的星球，我們除了可以利用新建構的模型推算泰坦生命起源的可能時間，同時也可以應用到其他行星或衛星上去。尤其是火星，目前太陽系最具爭議性的行星，以LHBE推論的結果，可能在39.5億年前（比地球早1∼2億年）就有機會產生生命。而利用LHBE這種碰撞消滅大氣的機制（Collisional Destruction Mechanism），可以用來建構星球大氣演化的模型，同時也可以應用到泰坦的大氣上。利用模型推算的結果，泰坦的原始N2大氣可能為今天的10∼200倍。
論文中除了利用蒙地卡羅法（Monte Carlo Method）探討星球受到LHBE的撞擊情形，並對於太陽系內幾個主要具有大氣層的行星（如金星、地球、火星）以及衛星（如泰坦），模擬LHBE在碰撞過程中可能發生的情形。除此之外，還以同位素分析的方法根據LHBE對星球大氣的影響來推算泰坦的原始大氣質量。

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