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- The Chamberlin–Moulton planetesimal hypothesis was proposed in 1905 by geologist Thomas Chrowder Chamberlin and astronomer Forest Ray Moulton to describe the formation of the Solar System. It was proposed as a replacement for the Laplacian version of the nebular hypothesis that had prevailed since the 19th century. The hypothesis was based on the idea that a star passed close enough to the sun early in its life to cause tidal bulges to form on its surface, which along with the internal process that leads to solar prominences, caused material to be ejected repeatedly from the sun. Due to the gravitational effects of the passing star, two spiral-like arms would have extended from the sun, and while most of the material would have fallen back, part of it would remain in orbit. This orbiting material would cool and condense into numerous small bodies that they termed planetesimals and a few larger protoplanets. Their theory proposed that as these objects collided over time, the planets and their moons were built up, with comets and asteroids being the leftover debris. The "spiral nebulae" photographed at Lick Observatory were thought to possibly be views of other suns undergoing this process. These nebulae are now known to be galaxies rather than developing solar systems. In 1917, James Hopwood Jeans argued that only a very close approach of a second star was necessary to eject material, instead of requiring solar prominences. In 1939, Lyman Spitzer showed that a column of material drawn out from the sun would dissipate rather than condense. By this time the theory had mostly fallen out of favor, and in the 1940s, the work of Henry Norris Russell showed that if the solar material had been pulled away from the sun with the force necessary to account for the angular momentum of Jupiter, the material would have continued out of the solar system entirely. Though the Chamberlin–Moulton hypothesis is no longer accepted, the idea of planetesimals remains in modern theory. (en)
- 張伯倫莫頓假說是地質學家TC张柏伦和天文學家弗雷斯·雷·莫頓在1905年提出，用來描述太陽系形成的假說。它被提出來做為替換在19世紀以來已經佔了上風的拉普拉斯星雲假說。 理論基於恆星在以足夠接近的距離經過太陽的附近，可以讓早期的太陽從表面產生潮汐隆起，這種延續導致內部過程形成日珥，使得物質從太陽彈射出去。由於經過的恆星的引力效應，將會有兩條螺旋臂從太陽向外擴展，大部分的物質會落回太陽，但有一部分將留在軌道上。這些在軌道上環繞的物質會冷卻，凝結成許多小團塊，較小的被稱為微行星（星子），幾顆較大的稱為原行星。他們的理論提出，因為這些物體隨著時間的推移而相互的碰撞，行星和他們的衛星逐漸建立起來，剩下的碎片就形成彗星和小行星。在利克天文台拍攝到的"螺旋星雲"被認為可能是其它的太陽正在經過這樣的歷程。現在已經知道這些星雲是星系，而不是在發展中的太陽系。 在1917年，詹姆士·金斯爭論只有第二顆恆星非常接近太陽才是必要的，而不必要求太陽有日珥彈出。在1939年，萊曼·史匹哲表明從太陽抽出的一系列物質會消散而不是凝結。此刻，這個理論已經不受歡迎而失寵，亨利·諾利斯·羅素在1940年代的工作顯示，計算出如果將物質從太陽拉扯出來，所需要的力量將形成有如木星一樣大的角動量，因而這些物質將繼續向外，完全逃離出太陽系。 雖然，張伯倫莫頓假說已經被摒棄，但微行星的想法依然留存在現在的理論中。 (zh)
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- 張伯倫莫頓假說是地質學家TC张柏伦和天文學家弗雷斯·雷·莫頓在1905年提出，用來描述太陽系形成的假說。它被提出來做為替換在19世紀以來已經佔了上風的拉普拉斯星雲假說。 理論基於恆星在以足夠接近的距離經過太陽的附近，可以讓早期的太陽從表面產生潮汐隆起，這種延續導致內部過程形成日珥，使得物質從太陽彈射出去。由於經過的恆星的引力效應，將會有兩條螺旋臂從太陽向外擴展，大部分的物質會落回太陽，但有一部分將留在軌道上。這些在軌道上環繞的物質會冷卻，凝結成許多小團塊，較小的被稱為微行星（星子），幾顆較大的稱為原行星。他們的理論提出，因為這些物體隨著時間的推移而相互的碰撞，行星和他們的衛星逐漸建立起來，剩下的碎片就形成彗星和小行星。在利克天文台拍攝到的"螺旋星雲"被認為可能是其它的太陽正在經過這樣的歷程。現在已經知道這些星雲是星系，而不是在發展中的太陽系。 在1917年，詹姆士·金斯爭論只有第二顆恆星非常接近太陽才是必要的，而不必要求太陽有日珥彈出。在1939年，萊曼·史匹哲表明從太陽抽出的一系列物質會消散而不是凝結。此刻，這個理論已經不受歡迎而失寵，亨利·諾利斯·羅素在1940年代的工作顯示，計算出如果將物質從太陽拉扯出來，所需要的力量將形成有如木星一樣大的角動量，因而這些物質將繼續向外，完全逃離出太陽系。 雖然，張伯倫莫頓假說已經被摒棄，但微行星的想法依然留存在現在的理論中。 (zh)
- The Chamberlin–Moulton planetesimal hypothesis was proposed in 1905 by geologist Thomas Chrowder Chamberlin and astronomer Forest Ray Moulton to describe the formation of the Solar System. It was proposed as a replacement for the Laplacian version of the nebular hypothesis that had prevailed since the 19th century. Though the Chamberlin–Moulton hypothesis is no longer accepted, the idea of planetesimals remains in modern theory. (en)
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- Chamberlin–Moulton planetesimal hypothesis (en)
- 張伯倫莫頓假說 (zh)
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