The dust around Vega-like stars: A bridge from YSOS to comets

被引：0

作者：

Butner, HM ^{[1
]}

Walker, HJ ^{[1
]}

Wooden, DH ^{[1
]}

机构：

[1] SMTO, Steward Observ, Tucson, AZ 85721 USA

来源：

FORMATION AND EVOLUTION OF SOLIDS IN SPACE | 1999年 / 523卷

关键词：

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Vega-like stars are infrared excess stars either nearing or already on the main sequence. The infrared excess is interpreted as evidence for the presence of extended dusty disks surrounding the stars. In a few cases, the disks have been directly imaged. While most of the disks are difficult to observe at optical and near-infrared wavelengths, a few disks are bright enough to study at 10 microns. Mid-infrared spectra from several of these mid-infrared bright Vega-like stars reveals a range of silicate emission features. Such features arise from the thermal emission of silicate grains in the disks. In some cases, the silicate features seen are similar to those seen towards some solar-system comets and interplanetary dust particles.

引用

页码：505 / 512

页数：8

共 22 条

[1]

Artymowicz P., 1996, Role of Dust in the Formation of Stars. Proceedings of the ESO Workshop, P137

[2]

Backman D. E., 1993, Protostars and Planets III, P1253

[3] COMBINED INFRARED AND ANALYTICAL ELECTRON-MICROSCOPE STUDIES OF INTERPLANETARY DUST PARTICLES [J].