Radiative Transfer on Perturbations in Protoplanetary Disks
Radiative Transfer on Perturbations in Protoplanetary Disks
复制标题
原行星盘中扰动的辐射传输
DOI：
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发表时间：
2003
期刊：
影响因子：
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通讯作者：
D. Sasselov
中科院分区：
文献类型：
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作者：
H. Jang;D. Sasselov
提出了一种计算受原行星扰动的原行星盘面上辐射传递的方法。我们应用这种方法来确定在一颗质量不超过20个地球的小原行星附近，一个被动的环绕恒星盘对光球内温度结构的影响。原行星的引力势会导致其附近的盘状物质受到压缩，导致盘状表面的密度降低。因此，光球层高度的等密度等高线呈现出井的形状。当这样的井被掠入射的恒星照射时，它会导致阴影区的冷却和裸露区域的加热。对于与行星形成时期相关的典型恒星和盘参数，我们发现，对于1个地球质量的行星来说，由于原行星与其母恒星相距1AU而引起的温度变化大约是4%(5K)，对于10个地球质量的行星大约是14%(19K)，对于20个地球质量的行星大约是18%(25K)。我们得出结论，即使是这样小的原行星也可以在被动盘中引起温度变化。因此，行星形成过程中的许多过程不应该用局部等温状态方程来模拟。
We present a method for calculating the radiative transfer on a protoplanetary disk perturbed by a protoplanet. We apply this method to determine the effect on the temperature structure within the photosphere of a passive circumstellar disk in the vicinity of a small protoplanet of up to 20 Earth masses. The gravitational potential of a protoplanet induces a compression of the disk material near it, resulting in a decrement in the density at the disk's surface. Thus, an isodensity contour at the height of the photosphere takes on the shape of a well. When such a well is illuminated by stellar irradiation at grazing incidence, it results in cooling in a shadowed region and heating in an exposed region. For typical stellar and disk parameters relevant to the epoch of planet formation, we find that the temperature variation due to a protoplanet at 1 AU separation from its parent star is about 4% (5 K) for a planet of 1 Earth mass, about 14% (19 K) for planet of 10 Earth masses, and about 18% (25 K) for planet of 20 Earth masses, We conclude that even such relatively small protoplanets can induce temperature variations in a passive disk. Therefore, many of the processes involved in planet formation should not be modeled with a locally isothermal equation of state.