The maximum temperature and radial temperature profile in a protoplanetary disc are important for the condensation of different elements in the disc. We simulate the evolution of a set of protoplanetary discs from the collapse of their progenitor molecular cloud cores as well as the dust decoupling within the discs as they evolve. We show how the initial properties of the cloud cores affect the thermal history of the protoplanetary discs using a simple viscous disc model. Our results show that the maximum mid-plane temperature in the disc occurs within 0.5 au. It increases with the initial cloud temperature and decreases with its angular velocity and the viscosity of the disc. From the observed properties of the molecular cloud cores, we find the median value of the maximum temperature is around 1250 K, with roughly 90 per cent of them being less than 1500 K – a value that is lower than the 50 per cent condensation temperatures of most refractory elements. Therefore, only cloud cores with high initial temperatures or low-angular velocities and/or low viscosities within the planet-forming discs will result in refractory-rich planetesimals. To reproduce the volatile depletion pattern of CM, CO, and CV chondrites and the terrestrial planets in Solar system, one must either have rare properties of the initial molecular cloud cores like high core temperature, or other sources of energy to heat the disc to sufficiently high temperatures. Alternatively, the volatile depletion observed in these chondrites may be inherited from the progenitor molecular cloud.

中文翻译：

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演化的原行星盘的最高温度和行星构件的组成

原行星盘中的最高温度和径向温度分布对于盘中不同元素的凝结很重要。我们模拟了一组原行星圆盘的演化，这些圆盘的前身分子云核心坍塌，以及圆盘内的尘埃随着它们的演化而解耦。我们使用简单的粘性盘模型展示了云芯的初始特性如何影响原行星盘的热历史。我们的结果表明，圆盘中的最大中间平面温度发生在 0.5 au 范围内。它随着初始云温度而增加，并随着其角速度和圆盘的粘度而降低。从观察到的分子云核的性质，我们发现最高温度的中值在 1250 K 左右，其中大约 90% 的温度低于 1500 K——这个值低于大多数耐火元素 50% 的冷凝温度。因此，只有在行星形成盘内具有高初始温度或低角速度和/或低粘度的云芯才会产生富含耐火材料的星子。要重现太阳系中 CM、CO 和 CV 球粒陨石和类地行星的挥发性耗尽模式，必须要么具有初始分子云核心的稀有特性，如高核心温度，要么具有其他能源来将圆盘加热到足够高温。或者，在这些球粒陨石中观察到的挥发性消耗可能是从祖分子云继承而来的。