2017MNRAS.464.4895G


Query : 2017MNRAS.464.4895G

2017MNRAS.464.4895G - Mon. Not. R. Astron. Soc., 464, 4895-4926 (2017/February-1)

Learning about the magnetar Swift J1834.9-0846 from its wind nebula.

GRANOT J., GILL R., YOUNES G., GELFAND J., HARDING A., KOUVELIOTOU C. and BARING M.G.

Abstract (from CDS):

The first wind nebula around a magnetar was recently discovered in X-rays around Swift J1834.9-0846. We study this magnetar's global energetics and the properties of its particle wind or outflows. At a distance of ∼4 kpc, Swift J1834.9-0846 is located at the centre of the supernova remnant (SNR) W41 whose radius is ∼19 pc, an order of magnitude larger than that of the X-ray nebula (∼2 pc). The association with SNR W41 suggests a common age of ∼5-100 kyr, while its spin-down age is 4.9 kyr. A small natal kick velocity may partly explain why a wind nebula was detected around this magnetar but not around other magnetars, most of which appear to have larger kick velocities and may have exited their birth SNR. We find that the GeV and TeV source detected by Fermi/Large Area Telescope (LAT) and High Energy Spectroscopic System (H.E.S.S.), respectively, of radius ∼11 pc is most likely of hadronic origin. The dynamics and internal structure of the nebula are examined analytically to explain the nebula's current properties. Its size may naturally correspond to the diffusion-dominated cooling length of the X-ray emitting e+e pairs. This may also account for the spectral softening of the X-ray emission from the nebula's inner to outer parts. The analysis of the X-ray synchrotron nebula implies that (i) the nebular magnetic field is >= 11 µG (and likely <= 30 µG), and (ii) the nebula is not powered predominantly by the magnetar's quiescent spin-down-powered MHD wind, but by other outflows that contribute most of its energy. The latter are most likely associated with the magnetar's bursting activity, and possibly dominated by outflows associated with its past giant flares. The energy source for the required outflows cannot be the decay of the magnetar's dipole field alone, and is most likely the decay of its much stronger internal magnetic field.

Abstract Copyright: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): diffusion - hydrodynamics - magnetic fields - stars: magnetars - stars: winds, outflows - ISM: supernova remnants - ISM: supernova remnants

Simbad objects: 28

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Number of rows : 28
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 G160.8+02.6 SNR 05 01 00.000 +46 40 00.00           ~ 197 0
2 2XMM J050106.5+451634 X 05 01 08.0 +45 16 31           ~ 112 0
3 SNR J052559-660453 SNR 05 26 00.4 -66 05 02     12.71     ~ 414 2
4 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 524 1
5 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5767 4
6 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 386 0
7 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 356 1
8 SNR G327.2-00.1 SNR 15 50 55 -54 18.0           ~ 61 1
9 PSR J1622-4950 Psr 16 22 44.80 -49 50 54.4           ~ 114 0
10 SNR G333.9+00.0 SR? 16 23 -49.7           ~ 10 0
11 SNR G337.0-00.1 SNR 16 35 06.9 -47 47 25           ~ 124 1
12 GRB 980618A gB 16 35 52 -47 35.2           ~ 244 0
13 SNR G348.7+00.3 SNR 17 13 43.0 -38 10 12           ~ 112 2
14 [AAB2008] 1 X 17 14 05.758 -38 10 31.32           ~ 52 1
15 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1141 2
16 SNR G023.3-00.3 SNR 18 34 51.80 -08 44 38.2           ~ 197 0
17 SWIFT J1834.9-0846 N*? 18 34 52.768 -08 45 40.83           ~ 66 0
18 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 242 1
19 4C -04.71 Rad 18 41 19.8 -04 56 06           ~ 309 3
20 SNR G029.6+00.1 Rad 18 44 52 -02 56.5           ~ 49 1
21 AX J1844.8-0258 HXB 18 44 53 -02 56.0           ~ 113 0
22 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 314 2
23 SNR G029.7-00.2 SNR 18 46 25.5 -02 59 14           ~ 309 2
24 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 803 0
25 NAME Sgr 1935+2154 * 19 34 55.68 +21 53 48.2           ~ 232 1
26 SNR G057.2+00.8 SNR 19 35.0 +21 57           ~ 77 0
27 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 599 1
28 SNR G109.1-01.0 SNR 23 01 35 +58 53.0           ~ 326 0

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2021.08.06-06:08:16

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