SPATIAL STRUCTURE OF THE CYGNUS LOOP IN THE X-RAY REGION ABOVE 1.5 KEV

被引：11

作者：

HATSUKADE, I ^{[1
]}

TSUNEMI, H ^{[1
]}

机构：

[1] OSAKA UNIV,FAC SCI,DEPT PHYS,TOYONAKA,OSAKA 560,JAPAN

来源：

ASTROPHYSICAL JOURNAL | 1990年 / 362卷 / 02期

关键词：

Nebulae: individual (Cygnus Loop); Nebulae: structure; Nebulae: supernovae remnants; X-rays: sources;

D O I：

10.1086/169294

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We observed the Cygnus Loop with the large area counter on board Ginga in the energy range above 1.5 keV. The observation was performed in a scanning mode along two different directions: one parallel to and the other perpendicular to the Galactic plane. The spatial structure shows that the emission region above 1.5 keV is narrower than that below 1 keV while their centers coincide well with each other. Furthermore, it shows a center-filled structure (plerion-type) rather than a shell structure. The emission above 1.5 keV is not well correlated with the optical nebula. Our data show that a high-temperature, low-density plasma fills the interior of the Cygnus Loop and is surrounded by a low-temperature, high-density plasma shell. The luminosity above 1.5 keV from the plasma filled inside the Loop is 2 × 1033 ergs s-1 which is about 40 times stronger than that predicted with the strong shock model.

引用

页码：566 / 571

页数：6