Potential multi-component structure of the debris disk around HIP 17439 revealed by Herschel/DUNES ⋆
Potential multi-component structure of the debris disk around HIP 17439 revealed by Herschel/DUNES ⋆
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Herschel/DUNES 揭示了 HIP 17439 周围碎片盘的潜在多组分结构 â
DOI：
10.1051/0004-6361/201219945
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发表时间：
2014
影响因子：
6.5
通讯作者：
S. Wolf
中科院分区：
文献类型：
--
作者：
S. Ertel;J. P. Marshall;J.-C. Augereau;A. V. Krivov;T. Löhne;C. Eiroa;A. Mora;C. Del Burgo;B. Montesinos;G. Bryden;W. Danchi;F. Kirchschlager;R. Liseau;J. Maldonado;G. L. Pilbratt;Ch. Schüppler;Ph. Thébault;G. J. White;S. Wolf
在碎片盘中观察到的尘埃是由行星/微行星形成过程中遗留下来的较大天体碰撞产生的。在空间上解决这些磁盘允许限制其架构，从而底层的行星/星子system.AimsOurHerschelopen时间关键程序DUNES旨在检测和表征碎片磁盘附近，太阳般的恒星。除了数据的统计分析，通过空间分辨的磁盘和详细的建模的单个对象的详细研究的数据是一个主要目标的project.MethodsWe获得的第一个观测空间分辨碎片盘周围的太阳一样的星星HIP 17439（HD 23484）使用仪器PACS和SPIRE上theHerschel空间天文台。同时多波长建模这些数据连同辅助数据从literatures.ResultsA标准的单组分磁盘模型无法重现主轴径向分布在70μm，100μm，和160μm的同时。此外，从这样一个模型得出的最佳拟合参数表明，从星星的几个Au到几百个Au，具有几乎恒定的表面密度，这在物理上是不可能的。然而，来自数据和我们有限的理论研究的约束还不足以完全排除这个模型。另一种更合理、更适合的系统模型是由两个尘埃环组成的，其高度约为100米。30 Au和90 Au，而这个模型的参数的约束是弱的，由于其复杂性和内在的degenerations.ConclusionsThe磁盘可能是由至少两个组件具有不同的空间位置（但不一定分离），而一个单一的，广泛的磁盘是可能的，但可能性较小。在我们的最佳拟合模型中，两个空间上分离良好的尘埃环表明至少存在一个高质量行星或几个低质量行星，这些行星清除了两个环之间的星子和尘埃。
ContextThe dust observed in debris disks is produced through collisions of larger bodies left over from the planet/planetesimal formation process. Spatially resolving these disks permits to constrain their architecture and thus that of the underlying planetary/planetesimal system.AimsOurHerschelopen time key program DUNES aims at detecting and characterizing debris disks around nearby, sun-like stars. In addition to the statistical analysis of the data, the detailed study of single objects through spatially resolving the disk and detailed modeling of the data is a main goal of the project.MethodsWe obtained the first observations spatially resolving the debris disk around the sun-like star HIP 17439 (HD 23484) using the instruments PACS and SPIRE on board theHerschelSpace Observatory. Simultaneous multi-wavelength modeling of these data together with ancillary data from the literature is presented.ResultsA standard single component disk model fails to reproduce the major axis radial profiles at 70μm, 100μm, and 160μm simultaneously. Moreover, the best-fit parameters derived from such a model suggest a very broad disk extending from few au up to few hundreds of au from the star with a nearly constant surface density which seems physically unlikely. However, the constraints from both the data and our limited theoretical investigation are not strong enough to completely rule out this model. An alternative, more plausible, and better fitting model of the system consists of two rings of dust at approx. 30 au and 90 au, respectively, while the constraints on the parameters of this model are weak due to its complexity and intrinsic degeneracies.ConclusionsThe disk is probably composed of at least two components with different spatial locations (but not necessarily detached), while a single, broad disk is possible, but less likely. The two spatially well-separated rings of dust in our best-fit model suggest the presence of at least one high mass planet or several low-mass planets clearing the region between the two rings from planetesimals and dust.
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观察碎片盘中的行星盘相互作用
影响因子：
6.5
作者：
S. Ertel;S. Wolf;J. Rodmann
通讯作者：
J. Rodmann
波江座 ε 周围温暖尘埃的冷起源
DOI：
--
发表时间：
2010
期刊：
影响因子：
--
作者：
Martin Reidemeister;A. Krivov;C. Stark;J. Augereau;T. Loehne;S. Mueller
通讯作者：
S. Mueller
碎片盘是自搅拌的吗？
DOI：
10.1111/j.1365-2966.2010.16528.x
发表时间：
2010
影响因子：
4.8
作者：
Grant M. Kennedy;M. Wyatt
通讯作者：
M. Wyatt
DOI：
10.1086/379854
发表时间：
2003
期刊：
The Astronomical Journal
影响因子：
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作者：
S. Kenyon;B. Bromley
通讯作者：
B. Bromley
影响因子：
3.5
作者：
C. Engelbracht;M. Blaylock;Kate Y. L. Su;Jeonghee Rho;G. Rieke;J. Muzerolle;D. Padgett;D. Hines;K. D. Gordon;Dario Fadda;A. Noriega-Crespo;D. Kelly;W. Latter;J. Hinz;K. Misselt;J. Morrison;J. Stansberry;D. Shupe;S. Stolovy;W. Wheaton;E. Young;G. Neugebauer;Stefanie Wachter;P. Pérez-González;P. Pérez-González;D. Frayer;F. Marleau
通讯作者：
C. Engelbracht;M. Blaylock;Kate Y. L. Su;Jeonghee Rho;G. Rieke;J. Muzerolle;D. Padgett;D. Hines;K. D. Gordon;Dario Fadda;A. Noriega-Crespo;D. Kelly;W. Latter;J. Hinz;K. Misselt;J. Morrison;J. Stansberry;D. Shupe;S. Stolovy;W. Wheaton;E. Young;G. Neugebauer;Stefanie Wachter;P. Pérez-González;P. Pérez-González;D. Frayer;F. Marleau