DISK RADII AND GRAIN SIZES IN HERSCHEL-RESOLVED DEBRIS DISKS
DISK RADII AND GRAIN SIZES IN HERSCHEL-RESOLVED DEBRIS DISKS
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赫歇尔解析碎片盘中的盘半径和晶粒尺寸
DOI：
10.1088/0004-637x/792/1/65
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
C. Eiroa
中科院分区：
文献类型：
--
作者：
N. Pawellek;A. V. Krivov;J.-P. Marshall;B. Montesinos;P. Abrahám;A. Moór;G. Bryden;C. Eiroa
碎片盘的半径及其尘埃颗粒的大小是这些系统中运行的小行星形成机制和物理过程的重要示踪物。在这里，我们使用在不同的赫歇尔空间天文台(赫歇尔空间天文台是欧空局空间天文台，由欧洲领导的主要调查者财团提供科学仪器，NASA也有重要参与)计划中分解的34个碎片盘的代表性样本，以限制盘半径及其尘埃的尺寸分布。虽然我们模拟了具有热和冷成分的盘，并确定了大约三分之二的恒星周围的热内盘，但我们的分析只集中在冷的外盘上，即柯伊伯带类似物。我们从分解的图像中得到了圆盘半径，发现任何光谱类别的主星都有很大的色散，但恒星的光度没有明显的变化趋势。这与冰线在设置碎片盘大小方面的主导作用相抵触，因为冰线的位置随着中央恒星的光度而变化。将圆盘半径固定为从分辨率图像推断的半径，我们对光谱能量分布进行建模，以确定每个目标的尘埃温度和颗粒尺寸分布。当尘埃温度朝着较早的光谱类型有系统地升高时，尘埃温度与圆盘半径处的黑体温度之比随着恒星光度的增加而减小。这是由一个明显的趋势来解释的，即典型的恒星大小越来越接近更明亮的恒星。典型的颗粒大小与S的辐射压力爆发极限进行了比较，后者与恒星光度质量比成正比，因此也随着早期光谱类别的增加而增加。G星到A星的星盘中的颗粒尺寸在所有恒星光度下都是S爆炸的数倍，这与碎片盘的碰撞模型是一致的。以S吹气为单位测量的大小似乎随着光度的增加而减小，这可能暗示着圆盘的搅动水平朝着较早类型的恒星增加。样品中所有圆盘的粉尘不透明度指数β在0到2之间，粒度分布指数Q在3到5之间变化。
The radii of debris disks and the sizes of their dust grains are important tracers of the planetesimal formation mechanisms and physical processes operating in these systems. Here we use a representative sample of 34 debris disks resolved in various Herschel Space Observatory (Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA) programs to constrain the disk radii and the size distribution of their dust. While we modeled disks with both warm and cold components, and identified warm inner disks around about two-thirds of the stars, we focus our analysis only on the cold outer disks, ie, Kuiper-belt analogs. We derive the disk radii from the resolved images and find a large dispersion for host stars of any spectral class, but no significant trend with the stellar luminosity. This argues against ice lines as a dominant player in setting the debris disk sizes, since the ice line location varies with the luminosity of the central star. Fixing the disk radii to those inferred from the resolved images, we model the spectral energy distribution to determine the dust temperature and the grain size distribution for each target. While the dust temperature systematically increases toward earlier spectral types, the ratio of the dust temperature to the blackbody temperature at the disk radius decreases with the stellar luminosity. This is explained by a clear trend of typical sizes increasing toward more luminous stars. The typical grain sizes are compared to the radiation pressure blowout limit s blow that is proportional to the stellar luminosity-to-mass ratio and thus also increases toward earlier spectral classes. The grain sizes in the disks of G-to A-stars are inferred to be several times s blow at all stellar luminosities, in agreement with collisional models of debris disks. The sizes, measured in the units of s blow, appear to decrease with the luminosity, which may be suggestive of the disk's stirring level increasing toward earlier-type stars. The dust opacity index β ranges between zero and two, and the size distribution index q varies between three and five for all the disks in the sample.
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发表时间：
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期刊：
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发表时间：
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