2004A&A...415..305U


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.14CEST14:27:02

2004A&A...415..305U - Astronomy and Astrophysics, volume 415, 305-311 (2004/2-3)

Convection in protoneutron stars and the structure of surface magnetic fields in pulsars.

URPIN V. and GIL J.

Abstract (from CDS):

We consider generation and evolution of small-scale magnetic fields in neutron stars. These fields can be generated by small-scale turbulent dynamo action soon after the collapse when the protoneutron star is subject to convective and neutron finger instabilities. After instabilities stop, small-scale fields should be frozen into the crust that forms initially at high density ∼ 1014g/cm3 and then spreads to the surface. Because of high crustal conductivity, magnetic fields with the lengthscale ∼1-3 km can survive in the crust as long as 10-100Myr and form a sunspot-like structure at the surface of radiopulsars.

Abstract Copyright:

Journal keyword(s): stars: pulsars: general - stars: neutron - magnetic fields

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 PSR B0943+10 Psr 09 46 07.31 +09 51 57.3           ~ 302 1
2 PSR J1210-5226 Psr 12 10 00.88 -52 26 28.4           ~ 204 1
3 PSR J1824-2452A Psr 18 24 32.009 -24 52 11.10           ~ 432 2
4 PSR J2144-3939 Psr 21 44 12.10 -39 33 55.2           ~ 95 0

    Equat.    Gal    SGal    Ecl

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2020.08.14-14:27:02

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