Photoevaporation of protoplanetary discs with PLUTO+PRIZMO I. Lower X-ray-driven mass-loss rates due to enhanced cooling

Andrew D. Sellek, Tommaso Grassi, Giovanni Picogna, Christian Rab, Cathie J. Clarke, Barbara Ercolano
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Abstract

Context: Photoevaporation is an important process for protoplanetary disc dispersal but there has so far been a lack of consensus from simulations over the mass-loss rates and the most important part of the high-energy spectrum for driving the wind. Aims: We aim to isolate the origins of these discrepancies through carefully-benchmarked hydrodynamic simulations of X-ray photoevaporation with time-dependent thermochemistry calculated on the fly. Methods: We conduct hydrodynamic simulations with pluto where the thermochemistry is calculated using prizmo. We explore the contribution of certain key microphysical processes and the impact of using different spectra used previously in literature studies. Results: We find that additional cooling results from the excitation of O by neutral H, which leads to dramatically reduced mass-loss across the disc compared to previous X-ray photoevaporation models, with an integrated rate of 10^-9 Msun/yr. Such rates would allow for longer-lived discs than previously expected from population synthesis. An alternative spectrum with less soft X-ray produces mass-loss rates around a factor of 2-3 times lower. The chemistry is significantly out of equilibrium, with the survival of H2 into the wind aided by advection. This leads to its role as the dominant coolant at 10s au - thus stabilising a larger radial temperature gradient across the wind - as well as providing a possible wind tracer.
利用 PLUTO+PRIZMO I 实现原行星盘的光蒸发。
背景:光蒸发是原行星盘分散的一个重要过程,但迄今为止,模拟结果在质量损失率和驱动风的高能谱最重要部分上缺乏共识。目的:我们的目标是通过仔细基准化的 X 射线光蒸发流体力学模拟,以及实时计算的随时间变化的热化学过程,来分离出这些差异的根源:我们对冥王星进行了流体力学模拟,其中的热化学是用 prizmo 计算的。我们探索了某些关键微物理过程的贡献,以及使用文献研究中使用的不同光谱的影响。结果:我们发现额外的冷却来自于中性 H 对 O 的激发,与之前的 X 射线光蒸发模型相比,这导致整个圆盘的质量损失显著降低,综合速率为 10^-9 Msun/年。这样的速率将使圆盘的寿命比之前的种群合成所预期的更长。使用较少软 X 射线的替代光谱产生的质量损失率大约低 2-3 倍。化学反应明显失去平衡,H2 在平流的帮助下进入风中。这导致它成为 10s au 处的主要冷却剂--从而稳定了整个风的较大径向温度梯度--并提供了一种可能的风向跟踪器。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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