2004ApJ...615L.133L

Query : 2004ApJ...615L.133L

2004ApJ...615L.133L - Astrophys. J., 615, L133-L136 (2004/November-2)

Radio pulsars as progenitors of anomalous X-ray pulsars and soft gamma-ray repeaters: magnetic field evolution through pulsar glitches.

LIN J.R. and ZHANG S.N.

Abstract (from CDS):

Glitches are common phenomena in pulsars. After each glitch, there is often a permanent increase in the pulsar's spin-down rate. Therefore, a pulsar's present spin-down rate may be much higher than its initial value and the characteristic age of a pulsar based on its present spin-down rate and period may be shorter than its true age. At the same time, the permanent increase of its spin-down rate implies that the pulsar's surface magnetic field is increased after each glitch. Consequently, after many glitches some radio pulsars may evolve into magnetars, i.e., strongly magnetized and slowly rotating neutron stars.

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Journal keyword(s): Stars: Pulsars: General - Stars: Pulsars: Individual: Name: Crab Pulsar - Stars: Pulsars: Individual: Alphanumeric: PSR B1757-24 - Stars: Pulsars: Individual: Name: Vela Pulsar

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
3 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1
4 PSR B1757-24 Psr 18 01 00.016 -24 51 27.50           ~ 258 1
5 NAME Milne 56 SNR 18 02 10.000 -24 54 00.00           ~ 182 3

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