2012MNRAS.422.2878D


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.18CEST11:49:19

2012MNRAS.422.2878D - Mon. Not. R. Astron. Soc., 422, 2878-2903 (2012/June-1)

Magnetic field decay in neutron stars: from soft gamma repeaters to `weak-field magnetars'.

DALL'OSSO S., GRANOT J. and PIRAN T.

Abstract (from CDS):

The recent discovery of the `weak-field, old magnetar' soft gamma repeater (SGR) J0418+5729, whose dipole magnetic field, Bdip, is less than 7.5 {x} 1012 G, has raised perplexing questions: how can the neutron star produce SGR-like bursts with such a low magnetic field? What powers the observed X-ray emission when neither the rotational energy nor the magnetic dipole energy is sufficient? These observations, which suggest either a much larger energy reservoir or a much younger true age (or both), have renewed the interest in the evolutionary sequence of magnetars. We examine here a phenomenological model for the magnetic field decay: {img} and compare its predictions with the observed period, P, the period derivative, {img}, and the X-ray luminosity, LX, of magnetar candidates. We find a strong evidence for a dipole field decay on a time-scale of ∼103 yr for the strongest (Bdip∼ 1015 G) field objects, with a decay index within the range 1 ≤ α < 2 and more likely within 1.5 ≲ α ≲ 1.8. The decaying field implies a younger age than what is implied by {img}. Surprisingly, even with the younger age, the energy released in the dipole field decay is insufficient to power the X-ray emission, suggesting the existence of a stronger internal field, Bint. Examining several models for the internal magnetic field decay, we find that it must have a very large ( ≳ 1016 G) initial value. Our findings suggest two clear distinct evolutionary tracks - the SGR/anomalous X-ray pulsar branch and the transient branch, with a possible third branch involving high-field radio pulsars that age into low-luminosity X-ray dim isolated neutron stars.

Abstract Copyright: 2012 The Authors Monthly Notices of the Royal Astronomical Society2012 RAS

Journal keyword(s): magnetic fields - stars: magnetars - stars: neutron - X-rays: stars

CDS comments: T.1 : Objects RX JHHMM not identified

Simbad objects: 23

goto Full paper

goto View the reference in ADS

Number of rows : 23

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 PSR J0100-7211 Psr 01 00 42.86 -72 11 33.3   17.69 17.82     B3V 87 0
2 PSR J0146+6145 Psr 01 46 22.21 +61 45 03.8   28.100 25.620     ~ 520 0
3 NAME Sgr J0418+5729 gam 04 18 33.867 +57 32 22.91           ~ 192 0
4 RX J0420.0-5022 N*? 04 20 02.2 -50 22 46     25.5     ~ 82 0
5 PSR B0525-66 Psr 05 26 00.7 -66 04 35           ~ 524 1
6 PSR B0656+14 Psr 06 59 48.1960 +14 14 19.400   24.85 24.90     ~ 780 1
7 RX J0720.4-3125 N* 07 20 24.961 -31 25 50.21   26.1   27.0   ~ 285 0
8 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 385 0
9 RX J1308.8+2127 N*? 13 08 48.7 +21 27 08   28.6 28.6     ~ 146 1
10 2MASX J15180915+0433468 GiC 15 18 09.1798495480 +04 33 46.920661510           ~ 14 0
11 PSR J1550-5418 Psr 15 50 54.18 -54 18 23.9           ~ 353 1
12 PSR J1622-4950 Psr 16 22 44.80 -49 50 54.4           ~ 114 0
13 GRB 980618A gB 16 35 52 -47 35.2           ~ 243 0
14 PSR J1647-4552 Psr 16 47 10.18 -45 52 16.7           ~ 180 1
15 PSR J1708-4008 Psr 17 08 49.0 -40 09 10           ~ 269 0
16 [AAB2008] 1 X 17 14 05.758 -38 10 31.32           ~ 51 1
17 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1138 2
18 AX J1809.8-1943 Psr 18 09 51.07 -19 43 51.8           ~ 385 0
19 NAME Sgr 1833-0832 gam 18 33 46.0 -08 32 13           ~ 68 0
20 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 239 1
21 PSR J1846-0258 Psr 18 46 24.94 -02 58 30.1           ~ 310 2
22 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 801 0
23 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 597 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2012MNRAS.422.2878D and select 'bookmark this link' or equivalent in the popup menu


2021.04.18-11:49:19

© Université de Strasbourg/CNRS

    • Contact