Speaker
Description
In this work, we investigate the Oscillating Asymmetric Dark Matter (OADM) model as a potential solution to the core-cusp problem, a well-known discrepancy between the predictions of the ΛCDM (Lambda Cold Dark Matter) cosmological model and the observed dark matter density profiles in dwarf spheroidal galaxies. While ΛCDM simulations typically predict a steep, cusp-like increase in dark matter density toward the centers of galaxies, observations often reveal flatter, core-like profiles. To address this issue, we analyze a mechanism in which dark matter annihilation is reactivated during the structure formation epoch, facilitated by a small Majorana mass term that breaks the conservation of dark matter particle number. This leads to oscillations between dark matter particles and their antiparticles, altering the density profiles of dark matter halos.
We analyze the impact of this annihilation mechanism on galaxy rotation curves using data from the SPARC (Spitzer Photometry and Accurate Rotation Curves) and LITTLE THINGS (Local Irregulars That Trace Luminosity Extremes, The HI Nearby Galaxy Survey) catalogs. By identifying the specific characteristics of the OADM model that best fit the observed data, we demonstrate that the model successfully converts cusp-type halos—predicted by ΛCDM—into core-type halos, consistent with the observed profiles in our data sample. Our results suggest that the OADM model provides a compelling explanation for the core-cusp problem, offering a dynamic mechanism to reconcile theoretical predictions with observational data. This work highlights the potential of the OADM framework to advance our understanding of dark matter dynamics and its role in shaping galactic structures.
