Constraints on cosmic-ray efficiency in the supernova remnant RCW 86

被引：1

作者：

Renaud, M. ^{[1
]}

Lemoine-Goumard, M. ^{[1
]}

Vink, J. ^{[1
]}

Allen, G. E. ^{[1
]}

Bamba, A. ^{[1
]}

Giordano, F. ^{[1
]}

Uchiyama, Y. ^{[1
]}

机构：

[1] Univ Montpellier 2, CNRS, LUPM, IN2P3, F-34095 Montpellier 5, France

来源：

HIGH ENERGY GAMMA-RAY ASTRONOMY | 2012年 / 1505卷

关键词：

Supernova remnants (individual: RCW 86); Astronomical observations: gamma-ray; RX J1713.7-3946; X-RAY; GAMMA-RAYS; EMISSION; ACCELERATION; RADIATION; TEV;

D O I：

10.1063/1.4772239

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Several young supernova remnants (SNRs) have recently been detected in the high-and very-high energy gamma-ray domains, and the nature of this emission is still hotly debated. We have studied the broadband nonthermal emission from one of these SNRs, namely RCW 86, by analyzing similar to 40 months of Fermi/LAT data in the high-energy domain, and the archival X-ray data from several instruments. The derived Fermi/LAT upper limits, together with the H. E. S. S. measurements, are incompatible with a standard E-p(-2) hadronic emission arising from p-p interactions, and can only be accommodated by a particle spectrum harder than E-p(-1.8). In such hadronic scenario, the total energy in hadrons eta(CR) = E-CR/E-SN is similar to 0.07 d(2.5)(2)/(n) over bar (cm-3) (with d(2.5) = d/2.5 kpc and (n) over bar (cm-3) equivalent to (n) over bar /1 cm(-3)), and the average magnetic field B must be larger than 50 mu G in order to significantly suppress any leptonic contribution. On the other hand, the interpretation of the gamma-ray emission by inverse Compton scattering reproduces the multi-wavelength data using a reasonable value for B of 15-25 mu G. In this leptonic scenario, we derive a conservative upper limit to eta(CR) of 0.04 d(2.5)(2)/(n) over bar (cm-3).

引用

页码：229 / 232

页数：4

共 23 条

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