Abstract
In this chapter, we present a brief and non-exhaustive review of the developments of theoretical models for accretion flows around neutron stars. A somewhat chronological summary of crucial observations and modelling of timing and spectral properties are given in Sects. 2 and 3. In Sect. 4, we argue why and how the Two-Component Advective Flow (TCAF) solution can be applied to the cases of neutron stars when suitable modifications are made for the NSs. We showcase some of our findings from Monte Carlo and Smoothed Particle Hydrodynamic simulations which further strengthens the points raised in Sect. 4. In summary, we remark on the possibility of future works using TCAF for both weakly magnetic and magnetic Neutron Stars.
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Acknowledgements
I would like to acknowledge the constant support and motivation provided by Prof. Sandip K. Chakrabarti. The work we have been doing for the past 2 years on the numerical simulation of spectral and timing properties of accreting neutron stars, was inspired by his work in the domain of stellar mass and supermassive black holes; conceived by him for the cases of neutron stars due to his unparalleled physical insight into the subject and flexibility to adapt in the face of new observations; implemented by his steadfast approach in supervising our work. I would personally like to thank him for tolerating and answering any and all of my academic questions, irrespective of time or place, for the past 4 years, I have worked under his supervision.
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Bhattacharjee, A. (2018). Generalized Flows Around Neutron Stars. In: Mukhopadhyay, B., Sasmal, S. (eds) Exploring the Universe: From Near Space to Extra-Galactic. Astrophysics and Space Science Proceedings, vol 53. Springer, Cham. https://doi.org/10.1007/978-3-319-94607-8_8
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