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I’m a theoretical and computational astrophysicist originally from Lebanon, currently based in Spain. My research delves into the extraordinary physics of neutron stars—exotic cosmic laboratories where immense magnetic fields, ultra-dense nuclear matter, and quantum anomalies converge.

After earning my Bachelor’s degree in Physics in Lebanon, I pursued advanced studies across Italy, France, and Spain through the Erasmus Mundus Joint Master in Nuclear Physics, supported by a competitive European scholarship. I completed my PhD at the Autonomous University of Barcelona, developing MATINS, a pioneering 3D magneto-thermal simulation code tailored for isolated neutron stars. This work was driven by my deep passion for coding and computational problem-solving, especially the challenge of designing and debugging complex numerical physics models.

Currently, as a Juan de la Cierva Fellow—awarded through a competitive national research program—I investigate how magnetic helicity and chiral anomalies influence neutron star magnetic field evolution. Building on this, I show how a newborn neutron star can reorganize a tangle of small magnetic knots into the strong, ordered dipole seen in magnetars—without any external power source. For years, ideas focused on the first moments after collapse struggled to build a large dipole and mostly produced short-lived, small-scale turbulence. My results explain how that turbulence later self-organizes. The key is magnetic helicity—the twist and linkage of field lines. A subtle quantum link between particle spin and magnetic fields (a chiral effect) lets the field use its own helicity as a catalyst to rearrange itself. Modern particle-physics calculations show that any initial particle imbalance decays quickly, and I include that damping. Even so, a tiny residual is enough when a neutron star has what earlier stages don’t: time. Over roughly 50–100 years, my 3D simulations show the field coalescing into a large-scale dipole of a few ×10¹⁴ gauss—matching observations of mature magnetars. This closes a long-standing gap between early “dynamo” ideas and observed magnetars, and highlights the often overlooked role of helicity: small twists, patiently guided over decades, can build the giant magnetic structures that power these stars.