Search for very high energy gamma radiation from the radio bright region DR4 of the SNR G78.2+2.1

被引：0

作者：

Prosch, C

Feigl, E

Plaga, R

Arqueros, F

Cortina, J

Fernandez, J

Fernandez, P

Fonseca, V

Funk, B

Gonzalez, JC

Haustein, V

Heinzelmann, G

Karle, A

Krawczynski, H

Krennrich, F

Kuhn, M

Lindner, A

Lorenz, E

Magnussen, N

Martinez, S

Matheis, V

Merck, M

Meyer, H

Mirzoyan, R

Moller, H

Moralejo, A

Muller, N

Padilla, L

Prahl, J

Rhode, W

Samorski, M

Sanchez, JA

Sander, H

Schmele, D

Stamm, W

Wahl, H

Westerhoff, S

WiebelSooth, B

Willmer, M

机构：

[1] MAX PLANCK INST PHYS & ASTROPHYS, D-80805 MUNICH, GERMANY

[2] UNIV COMPLUTENSE MADRID, FAC CIENCIAS FIS, E-28040 MADRID, SPAIN

[3] BUGH WUPPERTAL, FACHBEREICH PHYS, D-42119 WUPPERTAL, GERMANY

[4] CHRISTIAN ALBRECHTS UNIV KIEL, INST KERNPHYS, D-24118 KIEL, GERMANY

[5] UNIV HAMBURG, INST EXPT PHYS 2, D-22761 HAMBURG, GERMANY

[6] MAX PLANCK INST KERNPHYS, D-69029 HEIDELBERG, GERMANY

来源：

ASTRONOMY & ASTROPHYSICS | 1996年 / 314卷 / 01期

关键词：

gamma rays; observations; cosmic rays; ISM; supernova remnants; G; 78.2+2.1;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Data from the HEGRA air shower array are used to set an upper limit on the emission of gamma-radiation above 25 (18) TeV from the direction of the radio bright region DR4 within the SNR G78.2 + 2.1 of 2.5 (7.1). 10(-13) cm(-2) sec(-1). The shock front of SNR G78.2 + 2.1 probably recently overtook the molecular cloud Gong 8 which then acts as a target for the cosmic rays produced within the SNR, thus leading to the expectation of enhanced gamma-radiation. Using a model of Drury, Aharonian and Volk which assumes that SNRs are the sources of galactic cosmic rays via first order Fermi acceleration, we calculated a theoretical prediction for the gamma-ray flux from the DR4 region and compared it with our experimental flux limit. Our 'best estimate' value for the predicted flux lies a factor of about 18 above the upper limit for gamma-ray energies above 25 TeV. Possible reasons for this discrepancy are discussed.

引用

页码：275 / 280

页数：6

共 15 条

[1]

AHARONIAN F, 1993, 23RD P INT COSM RAY, V4, P291

[2]

AHARONIAN FA, 1994, ASTRON ASTROPHYS, V285, P645

[3] VERY-HIGH-ENERGY GAMMA-RAY ASTRONOMY AND THE ORIGIN OF COSMIC-RAYS [J].

AHARONIAN, FA .

NUCLEAR PHYSICS B, 1995, :193-206

[4] A SEARCH FOR ULTRA-HIGH-ENERGY GAMMA-RAY EMISSION FROM 5 SUPERNOVA-REMNANTS [J].

ALLEN, GE ;

BERLEY, D ;

BILLER, S ;

BURMAN, RL ;

CAVALLISFORZA, M ;

CHANG, CY ;

CHEN, ML ;

CHUMNEY, P ;

COYNE, D ;

DION, CL ;

DORFAN, D ;

ELLSWORTH, RW ;

GOODMAN, JA ;

HAINES, TJ ;

HOFFMAN, CM ;

KELLEY, L ;

KLEIN, S ;

SCHMIDT, DM ;

SCHNEE, R ;

SHOUP, A ;

SINNIS, C ;

STARK, MJ ;

WILLIAMS, DA ;

WU, JP ;

YANG, T ;

YODH, GB .

ASTROPHYSICAL JOURNAL, 1995, 448 (01) :L25-L28

[5]

Axford W. I., 1981, 17th International Cosmic Ray Conference, P155

[6] Numerical investigation of cosmic ray acceleration in supernova remnants [J].

Berezhko, E. G. ;

Yelshin, V. K. ;

Ksenofontov, L. T. .

ASTROPARTICLE PHYSICS, 1994, 2 (02) :215-227

[7] Diffuse radiation from cosmic ray interactions in the galaxy [J].

Berezinsky, V. S. ;

Gaisser, T. K. ;

Halzen, F. ;

Stanev, Todor .

ASTROPARTICLE PHYSICS, 1993, 1 (03) :281-287

[8]

Berezinsky V.S., 1990, Astrophysics of cosmic rays

[9] THE ACCELERATION OF COSMIC-RAYS IN SUPERNOVA-REMNANTS .1. GAMMA-RAY EVIDENCE FOR COSMIC-RAY INTENSITY VARIATIONS ON THE SCALE OF 0.1-3 KILOPARSECS [J].

BHAT, CL ;

ISSA, MR ;

MAYER, CJ ;

WOLFENDALE, AW ;

ZAN, M .

JOURNAL OF PHYSICS G-NUCLEAR AND PARTICLE PHYSICS, 1986, 12 (10) :1067-1086

[10]

BIERMANN PL, 1993, ASTRON ASTROPHYS, V271, P649

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