2013MNRAS.429.2945T


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.11CEST06:58:12

2013MNRAS.429.2945T - Mon. Not. R. Astron. Soc., 429, 2945-2952 (2013/March-2)

Properties of young pulsar wind nebulae: TeV detectability and pulsar properties.

TANAKA S.J. and TAKAHARA F.

Abstract (from CDS):

Among dozens of young pulsar wind nebulae (PWNe), some have been detected in TeV γ-rays (TeV PWNe), while others have not (non-TeV PWNe). The TeV emission detectability is not correlated with either the spin-down power or the characteristic age of the central pulsars and it is an open question as to what determines the detectability. To study this problem, we investigate the spectral evolution of five young non-TeV PWNe: 3C 58, G310.6-1.6, G292.0+1.8, G11.2-0.3 and SNR B0540-69.3. We use a spectral evolution model that was developed in our previous works to be applied to young TeV PWNe. The TeV γ-ray flux upper limits of non-TeV PWNe give upper or lower limits on parameters such as the age of the PWN and the fraction of spin-down power going into magnetic energy injection (the fraction parameter). Combined with other independent observational and theoretical studies, we can guess a plausible value of the parameters for each object. For 3C 58, we prefer parameters with an age of 2.5 kyr and fraction parameter of 3.0x10–3, although the spectral modelling alone does not rule out a lower age and a higher fraction parameter. The fraction parameter of 3.0x10–3 is also consistent for other non-TeV PWNe and thus the value is regarded as common to young PWNe, including TeV PWNe. Moreover, we find that the intrinsic properties of the central pulsars are similar: 1048–50erg for the initial rotational energy and 1042–44erg for the magnetic energy (2x1012-3x1013G for the dipole magnetic field strength at the surface). The TeV detectability is correlated with the total injected energy and the energy density of the interstellar radiation field around PWNe. Except for the case of G292.0+1.8, broken power-law injection of the particles reproduces the broad-band emission from non-TeV PWNe well.

Abstract Copyright: © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)

Journal keyword(s): radiation mechanisms: non-thermal - ISM: individual objects: 3C 58 - ISM: individual objects: G310.6-1.6 - ISM: individual objects: G292.0+1.8 - ISM: individual objects: G11.2-0.3 - ISM: individual objects: SNR B0540-69.3

Simbad objects: 16

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Number of rows : 16

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 SNR G130.7+03.1 SNR 02 05 37.0 +64 49 42           ~ 573 4
2 PSR J0205+6449 Psr 02 05 37.92 +64 49 42.8           ~ 219 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15283 1
4 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5721 4
5 NGC 2060 SNR 05 37 51.4470067818 -69 10 23.957283532   9.69 9.59     ~ 327 2
6 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 810 3
7 PSR J1124-5916 Psr 11 24 39.1 -59 16 20           ~ 138 1
8 SNR G292.0+01.8 SNR 11 24 59 -59 19.1           ~ 295 1
9 SNR G310.6-01.6 SNR 14 00 45.69 -63 25 42.6           ~ 28 1
10 SNR G000.9+00.1 SNR 17 47.3 -28 09           ~ 174 1
11 HESS J1809-193 gam 18 10 31 -19 18.0           ~ 44 1
12 SNR G011.2-00.3 SNR 18 11 28.9 -19 25 29           ~ 260 1
13 PSR J1811-1926 Psr 18 11 29.15 -19 25 25.4           ~ 113 1
14 SNR G021.5-00.9 SNR 18 33 33.612 -10 34 07.69           ~ 405 1
15 SNR G029.7-00.2 SNR 18 46 25.5 -02 59 14           ~ 304 2
16 SNR G054.1+00.3 SNR 19 30 31 +18 52.0           ~ 198 1

    Equat.    Gal    SGal    Ecl

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