Speaker
Description
Neutron stars are very dense objects found in the universe. These neutron stars can have very high angular velocity about their axis, such fast-spinning neutron stars are also known as pulsars. The rotation axis of a pulsar is defined as the axis around which a star rotates, similarly, we can define an axis called a magnetic axis, which is the axis along which the magnetic field lines originate. In an idealistic scenario, these two axes are not pointed in the same direction, thus forming a finite angle between them. Such stars are called oblique rotators. Pulsars having very high angular velocity can also result in the deformation of the shape of the star thus forming a spheroid. In this talk, I will present how we can model such stars considering general relativistic effects. I will also explain how the magnetic fields, charge density at the surface of the star, and power-loss of such a star varies
References:
1. Chatterjee, S., et. al., 2022. JHEAp. 34, 10-18
2. Goldreich, P., 1970. Astrophys. J. 160, L11.
3. Konno, K., et al., 1999. Astron. Astrophys. 352
4. Konno, K., Kojima, Y., 2000. Prog. Theor. Phys. 104.
5. Pacini, F., 1968. Nature 219, 145–146
6. Cook, G., et al., 1994. Astrophys. J. 422.
7. Komatsu, H., et al., 1989. Mon. Not. R. Astron. Soc. 237
