The composition of circumstellar gas and dust in 51 Oph

被引：29

作者：

van den Ancker, ME

Meeus, G

Cami, J

Waters, LBFM

Waelkens, C

机构：

[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[2] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands

[3] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium

[4] SRON, NL-9700 AV Groningen, Netherlands

来源：

ASTRONOMY & ASTROPHYSICS | 2001年 / 369卷 / 02期

关键词：

circumstellar matter; stars : emission-line; stars : evolution; stars : 51 Oph; infrared : stars;

D O I：

10.1051/0004-6361:20010245

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyze ISO archive data of the nearby bright emission-line star 51 Oph, previously classified as a proto-planetary system similar to P Pie. The infrared spectrum reveals the presence of gas-phase emission bands of hot (similar to 850 K) CO, CO(2), H(2)O and NO. In addition to this, partially crystalline silicate dust is present. The solid-state bands and the energy distribution are indicative of dust that has: formed recently, rather than of debris dust. The presence of hot molecular gas and the composition of the circumstellar dust are highly unusual for a young star and are reminiscent of what is found around evolved (AGB) stars, although we exclude the possibility of 51 Oph belonging to this group. We suggest several explanations for the nature of 51 Oph, including a recent episode of mass loss from a Be star, and the recent destruction of a planet-sized body around a young star.

引用

页码：L17 / L21

页数：5

共 35 条

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