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Query : 2008MNRAS.389L..66F |
2008MNRAS.389L..66F - Mon. Not. R. Astron. Soc., 389, L66-L70 (2008/September-1)
Origin and evolution of magnetars.
FERRARIO L. and WICKRAMASINGHE D.
Abstract (from CDS):
The high value of γ can be interpreted in one of two ways. It may indicate that the magnetic flux distribution on the main sequence is a strong function of mass and that this is reflected in the magnetic fluxes of the neutron stars that form from this mass range (the fossil field hypothesis). The recent evidence for magnetic fluxes similar to those of the magnetars in a high fraction (∼25 per cent) of massive O-type stars lends support to such a hypothesis. Another possibility is that the spin of the neutron star is a strong function of the progenitor mass, and it is only for stars that are more massive than ∼20M☉ that magnetar-type fields can be generated by the α-ω dynamo mechanism (the convective dynamo hypothesis). In either interpretation, it has to be assumed that all or a subset of stars in the mass range ∼20-45M☉, which on standard stellar evolution models lead to black holes via the formation of a fall-back disc, must give rise to magnetars.
Unlike with the radio pulsars, the magnetars only weakly constrain the birth spin period, due to their rapid spin-down. Our model predicts a birthrate of ∼1.5-3x10–3/yr for the magnetars.
Abstract Copyright: © 2008 The Authors. Journal compilation © 2008 RAS
Journal keyword(s): stars: early-type - stars: magnetic fields - stars: neutron - pulsars: general
Simbad objects: 11
Number of rows : 11 |
N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2024 |
#notes |
---|---|---|---|---|---|---|---|---|---|---|---|---|
1 | NAME SMC | BL? | 00 52 38.0 | -72 48 01 | 2.79 | 2.2 | ~ | 11103 | 1 | |||
2 | PSR J0100-7211 | Psr | 01 00 42.86 | -72 11 33.3 | 17.69 | 17.82 | B3V | 94 | 0 | |||
3 | NAME LMC | G | 05 23 34.6 | -69 45 22 | 0.4 | ~ | 17359 | 1 | ||||
4 | PSR B0525-66 | Psr | 05 26 00.7 | -66 04 35 | ~ | 542 | 1 | |||||
5 | NAME Orion Nebula Cluster | OpC | 05 35.0 | -05 29 | ~ | 2323 | 0 | |||||
6 | PSR J1550-5418 | Psr | 15 50 54.18 | -54 18 23.9 | ~ | 407 | 1 | |||||
7 | GRB 980618A | gB | 16 35 52 | -47 35.2 | ~ | 262 | 0 | |||||
8 | Cl Westerlund 1 | Cl* | 16 47 02.4 | -45 51 07 | ~ | 561 | 0 | |||||
9 | PSR J1647-4552 | Psr | 16 47 10.18 | -45 52 16.7 | ~ | 197 | 1 | |||||
10 | NAME 1806-20 Star Cluster | OpC | 18 08 39.0 | -20 24 39 | ~ | 35 | 1 | |||||
11 | W 31 | SFR | 18 10 28.6 | -19 55 51 | ~ | 259 | 0 |
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