Modelling the huge, Herschel-resolved debris ring around HD 207129
Modelling the huge, Herschel-resolved debris ring around HD 207129
复制标题
对 HD 207129 周围巨大的、赫歇尔解析的碎片环进行建模
DOI：
10.1051/0004-6361/201117731
复制
发表时间：
2012
影响因子：
6.5
通讯作者：
S. Wolf
中科院分区：
文献类型：
--
作者：
T. Löhne;J.-C. Augereau;S. Ertel;J. P. Marshall;C. Eiroa;A. Mora;O. Absil;K. Stapelfeldt;P. Thébault;C. del Burgo;W. Danchi;A.V. Krivov;J. Lebreton;G. Letawe;P. Magain;J. Maldonado;B. Montesinos;G. L. Pilbratt;G. J. White;S. Wolf
碎片盘是恒星系统的共同特征，从观测到的红外线过剩推断，碎片盘是尘埃、岩石和可能的星子的集合体。由于它们的形成和演化机制与行星体的形成和演化机制相联系，它们提供了宝贵的信息。为数不多的分辨率很好的碎片盘甚至更有价值，因为它们可以作为建模基准，并有助于解决建模方面的退化问题，如典型的粒度和距离。在这里，我们提出了一个分析的HD 207129碎片盘，其覆盖的光谱能量分布andHerschel/PACS图像的框架下获得的沙丘（尘埃周围的近地恒星）计划。我们使用经验的幂律方法的灰尘的分布，然后我们通过碰撞，直接辐射压力和阻力的灰尘的生产和去除模型。由此产生的最佳拟合模型包含的尘埃总质量接近10- 2个地球质量，微行星带的典型颗粒尺寸在4至7μm之间。我们将动力学激发限制在较低的水平，这将导致非常长的碰撞寿命和明显填充内部间隙的阻力，特别是在70μm处。放射状分布从100 Au以内以一个不寻常的向外上升的斜坡延伸到大约170-190 Au的一个相当尖锐的外缘。因此，内边缘比北落师门报告的更平滑，但来自几乎没有结合的颗粒的扩展晕的贡献同样很小。缓慢的自搅动和行星扰动都可能形成并塑造了这个圆盘。
Debris disks, which are inferred from the observed infrared excess to be ensembles of dust, rocks, and probably planetesimals, are common features of stellar systems. As the mechanisms of their formation and evolution are linked to those of planetary bodies, they provide valuable information. The few well-resolved debris disks are even more valuable because they can serve as modelling benchmarks and help resolve degeneracies in modelling aspects such as typical grain sizes and distances. Here, we present an analysis of the HD 207129 debris disk, based on its well-covered spectral energy distribution andHerschel/PACS images obtained in the framework of the DUNES (DUst around NEarby Stars) programme. We use an empirical power-law approach to the distribution of dust and we then model the production and removal of dust by means of collisions, direct radiation pressure, and drag forces. The resulting best-fit model contains a total of nearly 10-2Earth masses in dust, with typical grain sizes in the planetesimal belt ranging from 4 to 7μm. We constrain the dynamical excitation to be low, which results in very long collisional lifetimes and a drag that notably fills the inner gap, especially at 70μm. The radial distribution stretches from well within 100 AU in an unusual, outward-rising slope towards a rather sharp outer edge at about 170–190 AU. The inner edge is therefore smoother than that reported for Fomalhaut, but the contribution from the extended halo of barely bound grains is similarly small. Both slowly self-stirring and planetary perturbations could potentially have formed and shaped this disk.
登录
查看更多内容
附近恒星周围的柯伊伯带
影响因子：
6.5
作者：
R. Nilsson;R. Liseau;A. Brandeker;G. Olofsson;G. Pilbratt;C. Risacher;J. Rodmann;J. Augereau;P. Bergman;C. Eiroa;M. Fridlund;P. Th'ebault;G. P. D. O. Astronomy;S. University;Stockholm;Sweden.;O. Observatory;C. Technology;Onsala;E. A. Division;Estec;Noordwijk;The Netherlands.;Sron;Groningen;Esaestec Space Environment;Effects Section;U. J. Fourier;L. D. D. Grenoble;Grenoble;France.;Dpto. de F'isica Te'orica;F. Ciencias;U. A. D. Madrid;Madrid;Spain.;O. Paris;S. Meudon;D. Physics;Astronomy;Open University;M. Keynes;UK.;Science;Technology Facilities Council;R. Laboratory;Didcot
通讯作者：
Didcot
碰撞和破碎粒子的开普勒盘的演化：应用于埃奇沃斯-柯伊伯带的动力学模型
影响因子：
3.2
作者：
A. Krivov;M. Sremčević;F. Spahn
通讯作者：
F. Spahn
作为北落师门尘埃带结构起源的行星系统
影响因子：
64.8
作者：
P. Kalas;J. Graham;M. Clampin
通讯作者：
M. Clampin
DOI：
--
发表时间：
2009
期刊：
影响因子：
--
作者：
K. Heng;S. Tremaine
通讯作者：
S. Tremaine
DOI：
10.1088/0004-637x/691/2/l133
发表时间：
2009-02
期刊：
The Astrophysical Journal
影响因子：
--
作者：
S. Stewart;Z. Leinhardt
通讯作者：
S. Stewart;Z. Leinhardt