2006A&A...459..519A


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.08CET02:35:04

2006A&A...459..519A - Astronomy and Astrophysics, volume 459, 519-533 (2006/11-4)

Radio emission from shell-type supernova remnants.

ASVAROV A.I.

Abstract (from CDS):

The evolution of the radio emission of shell-type Supernova remnants (SNRs) is modeled within the framework of the simple and commonly used assumptions that the mechanism of diffusive shock acceleration (DSA) is responsible for generating radio emitting electrons and that the magnetic field is the typical interstellar field compressed at the shock. It is considered that electrons are injected into the mechanism in test-particle regime directly from the high energy tail of the downstream Maxwellian distribution function. The model can be applied to most of the observed SNRs because the majority of detected SNRs are shell-types and have a more or less spherical shape and are sources of nonthermal radio emission. It is shown that the model successfully explains the many averaged observational properties of evolved shell-type SNRs. In particular, the radio surface brightness (Σ) evolves with diameter as ∼D–(0.3/0.5), while the bounding shock is strong (Mach number is M ≥10), followed by steep decrease (steeper than ∼D–4.5) for M<10. Such evolution of the surface brightness with diameter and its strong dependence on the environmental parameters strongly reduce the usefulness of Σ-D relations as a tool for determining the distances to SNRs. The model predicts no radio emission from SNRs in the late radiative stage of evolution and the existence of radio-quiet but relatively active SNRs is possible. Our model easily explains very large-diameter radio sources such as the Galactic Loops and the candidates for Hypernova radio remnants. The model predicts that most of the observed SNRs with Σ1GHz≲10–20W/m2/sr/Hz are located in a tenuous phase of the ISM. The model also predicts the existence of a population of 150-250pc SNRs with Σ1GHz≲10–22W/m2/sr/Hz if the kinetic energy of the explosion is ∼1051erg. From the comparison of the model results with the statistics of evolved shell-type SNRs, we were able to estimate the fraction of electrons accelerated from the thermal pool in the range (3/11)x10–4. If acceleration takes place directly from the high energy tail of the downstream Maxwellian distribution function, then the corresponding injection momentum is estimated as pinj~(2.7-3).pth.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - acceleration of particles - shock waves

Simbad objects: 29

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Number of rows : 29

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1092 1
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11217 1
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9710 1
4 NGC 300 GiG 00 54 53.4460065856 -37 41 03.182962667 8.83 8.69 8.13 7.46   ~ 1350 2
5 IC 1613 GiC 01 04 54.2 +02 08 00   10.42 10.01 9.77   ~ 1122 2
6 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5253 1
7 SNR G160.8+02.6 SNR 05 01 00.000 +46 40 00.00           ~ 195 0
8 SNR G166.2+02.5 SNR 05 19.0 +41 53           ~ 70 0
9 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15214 1
10 SNR B0535-66.0 SNR 05 35 43.1 -66 01 59           ~ 160 1
11 SNR G180.0-01.7 SNR 05 39 00.000 +27 50 00.00           ~ 218 2
12 SNR B0547-69.7 SNR 05 47 17.5 -69 41 38           ~ 92 1
13 IC 443 SNR 06 18 02.7 +22 39 36     10.11     ~ 1121 1
14 NAME MONOCEROS NEB SNR 06 38 43 +06 30.2           ~ 222 0
15 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1135 2
16 NAME MSH 11-61A SNR 10 59 25.36 -61 18 42.6           ~ 158 0
17 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1228 1
18 SNR G349.7+00.2 SNR 17 18 10.160 -37 18 53.80           ~ 171 0
19 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           ~ 725 4
20 SNR G018.8+00.3 SNR 18 24.0 -12 23           ~ 94 0
21 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 846 2
22 W 49b SNR 19 11 09.000 +09 06 24.00           ~ 408 1
23 SNR G068.8+02.6 SNR 19 52 55 +32 54.2           ~ 331 1
24 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2296 2
25 [FT87] NGC 6946 1 SNR 20 35 00.74 +60 11 30.6           ~ 92 0
26 NAME Cyg Loop SNR 20 51.0 +30 40           ~ 837 0
27 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2476 1
28 NGC 7793 GiG 23 57 49.7533807411 -32 35 27.708304655 10.26 9.74 9.28 9.06 9.7 ~ 957 2
29 [BL97] N7793-S26 SNR 23 58 00.27 -32 33 22.1           ~ 48 0

    Equat.    Gal    SGal    Ecl

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2021.03.08-02:35:04

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