Atomic and Nuclear Physics

Biography

Biography: Ushasi Datta

Abstract

Even after 100 years of discovery of the atomic nucleus by Rutherford, the limits of the existence of the nuclei are still uncertain. This is due to lack of proper understanding of the nature of interactions that bind atomic nuclei. The atomic nucleus is a complex quantum many-body system but it's simple behavior can be explained by a mean nuclear field, containing many ingredients of the nucleon-nucleon interactions. The characteristics of that are the shell gaps at magic numbers, explained by Mayer and Jensen. The study of Nuclear Shell structure around the drip line and validation of theoretical  prediction with the data may provide important information on nucleon-nucleon interaction. This may play key role in understanding the limits of its existence. The Coulomb breakup is an exclusive tool for probing the quantum states of valence nucleon. We have investigated the ground-state properties of neutron-rich nuclei around N~20 using this method via kinematical complete measurement at GSI, Darmstadt. Very clear evidences have been observed for the breakdown and merging of long cherished magic shell gaps at N=20, 28. The nuclei around the drip-line are short lived and naturally do not exist on the earth. But surprisingly, evanescent rare isotopes imprint their existence in supernovae and other stellar explosive scenarios (rp, r-process etc.). To understand those processes and evaluation of elements, one has to create those nuclei in the laboratory to explore specific-properties. Due to their fleeting existence, indirect measurements are often only possible access to the information which are valuable inputs to the model for star evaluation process. Neutron star, remnant of supernovae is the densest matter, observed in cosmos. To understand that state of matter, some valuable properties of neutron-rich nuclei are key issues. I shall discuss our achievements related to above  mentioned facts using RIB in worldwide scenario.