# 2010A&A...509A..34B

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 Query : 2010A&A...509A..34B

2010A&A...509A..34B - Astronomy and Astrophysics, volume 509, A34-34 (2010/1-1)

A statistical approach to radio emission from shell-type SNRs. I. Basic ideas, techniques, and first results.

BANDIERA R. and PETRUK O.

Abstract (from CDS):

Shell-type supernova remnants (SNRs) exhibit correlations between radio surface brightness, SNR diameter, and ambient medium density, that between the first two quantities being the well known Σ-D relation. We investigate these correlations, to extract useful information about the typical evolutionary stage of radio SNRs, as well as to obtain insight into the origin of the relativistic electrons and magnetic fields responsible for the synchrotron emission observed in radio. We propose a scenario, according to which the observed correlations are the combined effect of SNRs evolving in a wide range of ambient conditions, rather than the evolutionary track of a typical'' SNR. We then develop a parametric approach to interpret the statistical data, and apply it to the data sample previously published by Berkhuijsen, as well as to a sample of SNRs in the galaxy M 33. We find that SNRs cease to emit effectively in radio at a stage near the end of their Sedov evolution, and that models of synchrotron emission with constant efficiencies in particle acceleration and magnetic field amplification do not provide a close match to the data. We discuss the problem of the cumulative distribution in size, showing that the slope of this distribution does not relate to the expansion law of SNRs, as usually assumed, but only to the ambient density distribution. This solves a long-standing paradox: the almost linear cumulative distribution of SNRs led several authors to conclude that these SNRs are still in free expansion, which also implies very low ambient densities. Within this framework, we discuss the case of the starburst galaxy M82. Statistical properties of SNR samples may be used to shed light on both the physics of electron acceleration and the evolution of SNRs. More precise results could be obtained by combining data of several surveys of SNRs in nearby galaxies.

Journal keyword(s): ISM: supernova remnants - methods: statistical - radiation mechanisms: non-thermal - acceleration of particles - galaxies: individual: M 33 - galaxies: individual: M 82

Full paper

 Number of rows : 41
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1158 1
2 SNR B0045-73.4 SNR 00 47 32.9 -73 07 46           ~ 50 1
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10600 1
4 SNR B0102-72.3 SNR 01 04 01.2 -72 01 52           ~ 384 1
5 SNR B0103-72.6 SNR 01 05 05.6 -72 23 20           ~ 80 1
6 M 33 GiG 01 33 50.8965749232 +30 39 36.630403128 6.17 6.27 5.72     ~ 5637 1
7 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 6630 1
8 SNR B0453-68.5 SNR 04 53 36.00 -68 29 30.0           ~ 77 1
9 SNR J045447-662528 SNR 04 54 48.00 -66 25 42.0           ~ 109 0
10 NAME LMC B0455-6843 SNR 04 55 55.9 -68 38 29           ~ 65 1
11 DEM L 34 HII 04 56 34.3 -66 26 52           ~ 101 0
12 SNR J045949-700835 SNR 04 59 54.00 -70 08 06.0           ~ 56 0
13 SNR B0505-67.9 SNR 05 05 42.0 -67 52 29           ~ 138 0
14 SNR J050555-680150 SNR 05 05 55.00 -68 01 54.0           ~ 83 0
15 SNR B0509-67.5 SNR 05 09 31 -67 31.3           ~ 217 0
16 NGC 1918 SNR 05 19 04.50 -69 38 56.0           ~ 100 0
17 SNR B0519-69.0 SNR 05 19 35.14 -69 02 00.5           ~ 152 0
18 SNR J051945-692600 SNR 05 19 45.00 -69 26 00.0           ~ 45 0
19 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16636 1
20 SNR J052501-693842 SNR 05 25 02.20 -69 38 39.0           ~ 387 1
21 SNR B0525-66.0 SNR 05 25 27.1 -65 59 11           ~ 98 1
22 SNR J052559-660453 SNR 05 26 00.4 -66 05 02     12.71     ~ 430 2
23 SNR J052741-691207 SNR 05 27 39.00 -69 12 12.0           ~ 38 0
24 SNR B0527-65.8 SNR 05 27 57.00 -65 49 54.0           ~ 37 0
25 NGC 2018 As* 05 31 24.00 -71 04 24.0   10.91 10.89     ~ 103 1
26 SNR J053400-695508 SNR 05 33 59.00 -69 55 00.0           ~ 64 0
27 SNR B0534-70.5 SNR 05 34 08.80 -70 34 28.0           ~ 65 0
28 SNR B0535-66.0 SNR 05 35 43.1 -66 01 59           ~ 171 1
29 SNR J053605-703826 SNR 05 36 07.00 -70 38 48.0           ~ 59 0
30 SNR B0543-68.9 SNR 05 43 08 -68 58.3           ~ 56 0
31 SNR B0547-69.7 SNR 05 47 17.5 -69 41 38           ~ 93 1
32 SNR B0548-70.4 SNR 05 47 50.00 -70 24 54.0           ~ 84 0
33 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1201 2
34 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5700 6
35 ESO 134-11 HII 14 40 29 -62 38.7           ~ 551 1
36 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1298 1
37 AJG 44 Psr 16 17 33.000 -51 02 00.00           ~ 492 3
38 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           ~ 774 4
39 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 931 2
40 W 49b SNR 19 11 09.000 +09 06 24.00           ~ 445 1
41 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2683 1

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2023.03.26-14:18:34