Published in Journal 1, 2009
This paper is about the number 1. The number 2 is left for future work.
Recommended citation: Your Name, You. (2009). "Paper Title Number 1." Journal 1. 1(1). http://academicpages.github.io/files/paper1.pdf
Published in Journal 1, 2010
This paper is about the number 2. The number 3 is left for future work.
Recommended citation: Your Name, You. (2010). "Paper Title Number 2." Journal 1. 1(2). http://academicpages.github.io/files/paper2.pdf
Published in Journal 1, 2015
This paper is about the number 3. The number 4 is left for future work.
Recommended citation: Your Name, You. (2015). "Paper Title Number 3." Journal 1. 1(3). http://academicpages.github.io/files/paper3.pdf
Neutron stars are probably the most compact and extreme magnetised astrophysical objects in the universe. The unbelievably intense magnetic fields they carry are known to be responsible for many astrophysical phenomena. Therefore, understanding the astrophysics of these extreme compact objects are the key to solve many puzzling problems on highly energetic astrophysical phenomena. 
To describe such extreme astrophysical systems, proper physics needs to be taken into account. For example, general relativity is required to account for the extremely strong gravitational fields, relativistic magnetohydrodynamics is necessary to describe the dynamics of plasma. Since the corresponding equations are highly non-linear and fully coupled with each other, they cannot be described analytically. First-principles numerical simulation is probably the only possible way to accurately model the evolution of these extreme compact objects. To accurately model these astrophysical systems, I develop and implement large-scale high-performance computing general-relativistic simulation codes. 
Published:
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Published:
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Undergraduate course, University 1, Department, 2014
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Workshop, University 1, Department, 2015
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