Analysis of planetary nebular in the milky way: Physicalproperties, chemical abundances, and galactic distributions

This thesis examines the physical and chemical properties of planetary nebulae in the Milky Way and their distribution among the structural components of the Galaxy, such as the disk, bulge, and halo. For this purpose, 1449 "True Planetary Nebula" data selected from the HASH (The Hong Kong/AAO/Strasbourg Hα Planetary Nebula Database) database were used. It was determined that the majority of planetary nebulae are located in the Galactic disk and that planetary nebulae in the halo have relatively larger angular dimensions. Physical parameters derived from approximately 16,500 emission line measurements obtained from the spectral data of planetary nebulae; the attenuation coefficient, electron temperature, and electron density were observed to form Gaussian-like distributions with median values of 1.5, 9,900 K, and 1,200 cm⁻³, respectively. Additionally, the abundance of elements obtained from 7,200 different measurements revealed that Helium, Nitrogen, Oxygen, Neon, Sulfur, Chlorine, and Argon elements show different distributions among galactic components, and that the abundance of all elements is at its lowest level, particularly in planetary nebulae in the halo. However, a strong correlation (r=0.87) has been detected between the abundance of sulfur and nitrogen elements in all galactic components.