I work on binary systems made of Neutron Stars (NS) and NS/ White Dwarfs
(WD)/Black Holes (BH), as well as double WD systems, and core-collapse of massive, rapidly rotating stars. I study how compact objects form, evolve, and merge, and which transient events they produce. Also, I am interested in the magnetic helicity which plays a major role in suppressing the kinematic large scale dynamo and driving the large scale dynamo through the magnetic helicity flux.
In double WD system, I am resolving the critical conditions for deflagration and detonation shock waves once type Ia Supernova occurs. Hypotheses are tested using extensive hydrodynamical, thermonuclear, AMR, and multidimensional simulations coupled with detailed nuclear reaction networks (The computational requirements for these use MESA and FLASH). The results of these simulations are followed by an analysis of composition using a large-scale nucleosynthetic network – (PPN). These enable us just to calculate the detailed properties of SN’s ejecta.
I study turbulent nuclear burning, which can largely enhance nuclear burning rates and may serve as an additional mechanism for stellar explosions. Moreover, it may power thermonuclear and pair-instability supernovae, liberate the neutrinos in core-collapse supernovae, and synthesize r-process heavy nuclei in kilonovae and collapsars.
Currently, I'm studying the dynamical ejecta of binary Neutron Stars like evolution, properties and the end results by using 3D GRMHD simulation (e.x, HARM3DNUC).
Furthermore, I'm studying the low mass BH formation from Dark Matter (DM) triggered collapse.
The Ca-rich SNe: evolution of the debris disk from the 0.55 𝑀⊙ CO-WD disk around the HeCO-WD of mass 𝑀 = 0.63𝑀⊙. The panels show the color coded density distribution throughout the simulation. We show the initial model followed by several snapshots. Significant nuclear burning begins already at ∼30 sec, and The detonation occurs at 𝑡_𝑑𝑒𝑡 ≃ 46 𝑠𝑒𝑐, which is about 88% of t_visc0 .
The Ca-rich SNe: Left panel: The bolometric light curve of fca1 (green curve), fca2 (blue curve), fca3 (red curve) compared to Ca-rich SNe 2019ehk (squares), 2021gno (circles) and 2021inl (polygons). Right panel: comparison of the three models in the r-band Mr to type Ib/IIb SNe and SN 2019ehk relative to maximum light in the AB magnitude system.
BNS simulation: Left panel: The density distribution of the BNS until 90 msec. Right panel: the radial profile of mass weighted in whole grid between 5-190 msec. The gray curve is the fit curve as you can see how close to Keplerian r^(-3/2).
Background Fluctuation: Log-log plot of the dimensionless fractional turbulent enhancement in the nuclear burning rate, as a function of the RMS temperature fluctuation on length scale r, normalized to the mean temperature, in the distributed burning regime. The curves shown are for neutrino cooling via the URCA process (solid line), C12 -C12 burning (dashed), and triple-alpha reaction (dot dashed). The inset figure shows the same three curves on the same set of axes, compensated by the factor (1/[n*(n - 1)]). For weak enhancement, the compensated enhancement collapses onto a single curve, demonstrating its universal nature.