碎片轨道的变化：太阳质量为1-3的主序星在30-150 AU的冰行星形成
Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 Solar Mass Main Sequence Stars
摘要：
我们描述了在30-150 AU的1-3太阳质量的恒星周围的冰行星和碎片盘的形成的计算。碎片盘的形成与行星系统的形成相一致。随着原行星的成长，它们将剩余的星子搅拌到很大的速度。一系列的碰撞将剩余的碎片碾成粉末，形成了一个可观察到的碎片盘。恒星的寿命和碰撞级联限制了原行星的生长。冰质行星的最大半径约为1750公里，与初始盘质量、恒星质量和恒星年龄无关。这些物体包含的固体物质不超过初始质量的3%至4%。碰撞级联产生的碎片盘的最大亮度约为恒星亮度的0.002倍。峰值24微米的过量变化从大约1%的恒星光球通量为1太阳质量的恒星到大约50倍的恒星光球通量为3太阳质量的恒星。峰值70-850微米的过量大约是恒星光球通量的30-100倍。对于所有的恒星，24-160微米的过剩在恒星年龄为5-20百万年时上升，在10-50百万年时达到峰值，然后下降。下降大致呈幂律，其中f propto t^{-n}且n = 0.6-1.0。这一预测的演化与已发表的A型和太阳型恒星的观测结果一致。观测到的A型恒星的远红外颜色演化也与模型预测相匹配。
英文摘要：
We describe calculations for the formation of icy planets and debris disks at 30-150 AU around 1-3 solar mass stars. Debris disk formation coincides with the formation of planetary systems. As protoplanets grow, they stir leftover planetesimals to large velocities. A cascade of collisions then grinds the leftovers to dust, forming an observable debris disk. Stellar lifetimes and the collisional cascade limit the growth of protoplanets. The maximum radius of icy planets, roughly 1750 km, is remarkably independent of initial disk mass, stellar mass, and stellar age. These objects contain no more than 3% to 4% of the initial mass in solid material. Collisional cascades produce debris disks with maximum luminosity of roughly 0.002 times the stellar luminosity. The peak 24 micron excess varies from roughly 1% of the stellar photospheric flux for 1 solar mass stars to roughly 50 times the stellar photospheric flux for 3 solar mass stars. The peak 70-850 micron excesses are roughly 30-100 times the stellar photospheric flux. For all stars, the 24-160 micron excesses rise at stellar ages of 5-20 Myr, peak at 10-50 Myr, and then decline. The decline is roughly a power law, with f propto t^{-n} and n = 0.6-1.0. This predicted evolution agrees with published observations of A-type and solar-type stars. The observed far-IR color evolution of A-type stars also matches model predictions.
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