2006ApJ...637.1010L

Query : 2006ApJ...637.1010L

2006ApJ...637.1010L - Astrophys. J., 637, 1010-1015 (2006/February-1)

On the nature of radio pulsars with long periods.

LOMIASHVILI D., MACHABELI G. and MALOV I.

Abstract (from CDS):

We show that the drift waves near the light cylinder can cause modulation of the emission with periods of the order of several seconds. These periods explain the intervals between successive pulses observed in ``magnetars'' and radio pulsars with long periods. The model under consideration makes it possible to calculate the real rotation periods of the host neutron stars. They are less than 1 s for the investigated objects. The magnetic fields at the surface of the neutron star are of the order of 1011-1013 G and equal to the usual fields for known radio pulsars.

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Journal keyword(s): Stars: Pulsars: Individual: Alphanumeric: PSR J1119-6127 - Stars: Pulsars: Individual: Alphanumeric: PSR J1814-1744 - Stars: Pulsars: Individual: Alphanumeric: PSR J1847-0130 - Stars: Pulsars: Individual: Alphanumeric: PSR J2144-3933 - Stars: Magnetic Fields

Simbad objects: 8

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Number of rows : 8
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 PSR J1119-6127 Psr 11 19 14.30 -61 27 49.5           ~ 439 1
2 PSR B1642-03 Psr 16 45 02.0330 -03 17 57.200           ~ 394 0
3 PSR B1811-17.7 Psr 18 14 43.10 -17 44 48.0           ~ 77 0
4 PSR B1828-10 Psr 18 30 47.566 -10 59 27.90           ~ 190 1
5 PSR J1847-0130 Psr 18 47 35.2 -01 30 46           ~ 44 0
6 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 906 0
7 PSR J2144-3939 Psr 21 44 12.01000 -39 33 58.4000           ~ 145 0
8 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 673 1

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