Collisional modelling of the debris disc around HIP 17439
Collisional modelling of the debris disc around HIP 17439
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HIP 17439 周围碎片盘的碰撞建模
DOI：
10.1051/0004-6361/201423523
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发表时间：
2014
影响因子：
6.5
通讯作者：
C. Eiroa
中科院分区：
文献类型：
--
作者：
Ch. Schüppler;T. Löhne;A. V. Krivov;S. Ertel;J. P. Marshall;C. Eiroa
我们对附近K2 V星星HIP 17439周围的碎片盘进行了分析。在HerschelDUNES关键计划的背景下，使用HerschelPACS和SPIRE仪器在远红外中观察和空间分辨盘。在以前的研究中，我们假设星周尘埃的大小和径向分布是独立的幂律。在探讨了非常广泛的可能模型参数之后，提出了能够解释这些观测结果的几种设想。在本文中，我们对这些场景进行了后续的深入碰撞建模，以进一步区分它们。在我们的模型中，我们考虑碰撞，直接辐射压力，和阻力，这是实际的物理过程中运作的碎片盘。我们发现，在第一篇论文中讨论的所有方案在物理上是合理的，可以重现所观察到的光谱能量分布沿着与PACS表面亮度配置文件合理。在一个模型中，尘埃是在一个狭窄的小行星带中产生的，超过120 Au，并通过坡印廷-罗伯逊和恒星风阻力向内输送。要与观测到的径向剖面吻合，需要恒星风比太阳风强一个数量级，这一点没有得到观测的证实，尽管没有被排除。另一个模型由两个空间分离的微行星带组成，一个温暖的内部和一个寒冷的外部。这种情况可能意味着行星的存在清除了两个组件之间的差距。最后，我们定性地表明，可以解释的意见，假设尘埃是在一个单一的，但广泛的星子盘与固体的表面密度向外上升，预期为一个扩展的磁盘，经历了一个自然的内-外碰撞耗尽。讨论了通过未来观测区分竞争情景的前景。
We present an analysis of the debris disc around the nearby K2 V star HIP 17439. In the context of theHerschelDUNES key programme, the disc was observed and spatially resolved in the far-IR with theHerschelPACS and SPIRE instruments. In a previous study, we assumed that the size and radial distribution of the circumstellar dust are independent power laws. There, several scenarios capable of explaining the observations were suggested after exploring a very broad range of possible model parameters. In this paper, we perform a follow-up in-depth collisional modelling of these scenarios to further distinguish between them. In our models we consider collisions, direct radiation pressure, and drag forces, which are the actual physical processes operating in debris discs. We find that all scenarios discussed in the first paper are physically reasonable and can reproduce the observed spectral energy distribution along with the PACS surface brightness profiles reasonably well. In one model, the dust is produced beyond 120 au in a narrow planetesimal belt and is transported inwards by Poynting-Robertson and stellar wind drag. Good agreement with the observed radial profiles would require stellar winds by about an order of magnitude stronger than the solar value, which is not confirmed – although not ruled out – by observations. Another model consists of two spatially separated planetesimal belts, a warm inner and a cold outer one. This scenario would probably imply the presence of planets clearing the gap between the two components. Finally, we show qualitatively that the observations can be explained by assuming the dust is produced in a single, but broad planetesimal disc with a surface density of solids rising outwards, as expected for an extended disc that experiences a natural inside-out collisional depletion. Prospects of distinguishing between the competing scenarios by future observations are discussed.
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