The Impact of Magnetic Dipole Radiation and Decay on the Variation of Period and Inclination Angle of Pulsars
School of Physics, Northeast Normal University, Changchun, China
Received: October 30, 2019 Accepted: November 25, 2019 Published: December 3, 2019
Citation: Li LS. The Impact of Magnetic Dipole Radiation and Decay on the Variation of Period and Inclination Angle of Pulsars. Int J Phys Stud Res. 2019; 2(1): 78-80. doi: 10.18689/ijpsr-1000111
Copyright: © 2019 The Author(s). This work is licensed under a Creative Commons Attribution 4.0 International License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
The change of pulsar period and inclination angle under the braking of magnetic radiation and magnetic decay is studied. The system of equations of evolution of period and inclination angle is given and solves it. The solution shows that the period increases and inclination angle decreases with time under the braking of magnetic radiation and decay. The numerical results for the change of period and inclination angle of PSR0531+21 are given. The discussions are drawn.
Keywords: Pulsar; Period and inclination angle; Braking of magnetic radiation and Decay; Change.
When pulsar was born, the gravitational radiation plays a leading role in 81 year . Afterward, the magnetic radiation plays a second role in a life of pulsar. In this stage pulsar rotation is very fast and its rotational energy is very large and its magnetic field is very stronger, but the rotational energy and the magnetic field also are small and weakness with time gradually. It is well known that the rotational energy may transforms to pulsar radiation energy and the weakness of magnetic field may result in the magnetic moment decay. Other hand the magnetic radiation and magnetic decay result in prolong of period and decrease of obliquity angle with time.
In the past years some authors researched these topics, such as, Ostriker and Gunn , Davns & Goltstein , Wang et al. , Heansel et al. , Mira et al. , Urpin & Gil , Philippov et al. . The research of these authors is very desirable and devisable. Based on these researches, the present paper combines concrete pulsar for researching the evolution of the period and obliquity angle under braking of magnetic radiation and magnetic decay.
The Change of Pulsar Period and Inclination Angle under the Braking of Magnetic Dipolar Radiation
Philippov et al. provided a method for studding the evolution of period and obliquity angle of pulsar under braking of magnetic radiation and decay. This paper cited the system of equations with angular velocity Ω and inclination angle α .
where I dettes the moment of inertia. The Z-compo net of toque, Kz, act opposite to Ω , Kx component act perpendicular to Ω .
According to Philippov et al. 
μ is magnetic moment
Substitution of (3), (4) and (5) into (1) and (2), we obtain
By letting . P is period of pulsar.
The equations (6) and (7) become as
The equations (9)-(10) can be given
Integrating the above equation
The equation (10) can be written by using (12):
Integrating the above equation
Substituting the above expression into the first expression of (12), we obtain the change of period of pulsar
The expressions (14) and (15) are that the change of period and inclination angle with time under the braking of the magnetic radiation.
The Change of the Period and Inclination Angle under the Braking of the Magnetic Decay
We assume that the magnetic moment of pulsar decays with the exponent, i. e
ξ is the coefficient of the magnetic decay. μ0=R3B0. Substituting (16) into the equation (13) and integrating it
Substituting the above expression into the first expression of (12), we obtain
The expressions of (17) and (18) are that the change of period and obliquity angle with time under their braking of the magnetic decay.
This paper uses the formulae (14)–(15) and (17)–(18) to calculate the change of the period and magnetic inclination angle under the braking of magnetic radiation and magnetic decay for PSR0531+21 (Crab pulsar) . Its period P0=0.033058(s), and magnetic field B0=3.78 × 1012G cited from Manchestefer et al. . Itʼs obliquity angle α0=59°.2 cited from Davis and Goldstein . I=1.4 × 1045 (g.cm2) , R=1.2 × 106 cm. , ξ=1.1111 × 10-6/yr .
Discussion and Conclusion for Numerical Results
(1) It can be seen from tables 1 and 2 that the period increases and inclination angle decreases with time under the magnetic radiation and magnetic decay.
(2) However the increase of period and decrease of inclination angle under the braking of magnetic decay are larger than that under the braking of magnetic radiation.
(3) The decrease of magnetic radiation is due to the rotational energy loss and the magnetic decay is due to the weakness of magnetic field with time. Hence the increase of period and decrease of the magnetic inclination angle are due to the rotational energy loss and the weakness of the magnetic field of pulsar.
(4) The pulsar PSR0531+21 speeds up suddenly due to stellar quake (glitches) in three years . However it is temporary happening and it is not secular happening. It does not influence the secular variation of period and inclination angle due to the braking of magnetic radiation and magnetic decay.
- Ostriker JP, Gunn JE. On the Nature of Pulsars I Theory. The Astrophysical Journal. 1969; 157: 1395. doi: 10.1086/150160
- Davis L, Goldstein M. Magnetic-dipole alignment in pulsars. The Astrophysical Journal. 1970; 159: L81-L86.
- Wang ZR, Qu QR, Lu T, Lu LF. Statistical analysis of the radio luminosity of pulsars. Acta Astronomical Sonica. 1979; 10: 199.
- Haensel P, Urpin VA, Vakovlev DG. Ohmic decay of internal magnetic fields in neutron stars. Astron Astrophysics. 1990; 229(1): 133-137.
- Mitra D, Konar S, Bhattacharya D. Evolution of the multipolar magnetic field in isolated neutron stars. Monthly Notices of the Royal Astronomical Society (MNRAS). 1999; 307(2): 459-462. doi: 10.1046/j.1365-8711.1999.02654.x
- Urpin V, Gil J. Convection in protoneutron stars and the structure of surface magnetic fields in pulsars. Astron Astrophys. 2004; 415: 305-311. doi: 10.1051/0004-6361:20034447
- Philippov A, Tchek hovskov A, Li JG. Time evolution of pulsar obliquity angle from 3D simulations of magnetospheres. Monthly Notices of the Royal Astronomical Society. 2014; 441: 1879-1887.
- Shapiro SL, Teukolsky SA. Black holes, white dwarfs and neutron stars: the physics of compact objects. A Wiley Interscience publishing, John Wiley & sons, New York chi Chester; 1983.
- Manchester RN, Hobbs GB, Teoh A, Hobbs M. The Australia Telescope National Facility Pulsar Catalog. The Astronomical Journal. 2005; 129(4): 1993-2006. doi: 10.1086/428488
- Dʼalessandro F. Rotational irregularities in pulsars — A review. Astrophys Space Sci. 1996; 246: 73-106.