Study of Galactic Star Forming Regions and Related Instrumentation

Abstract

Star formation is a process by which dilute gas converted to stellar systems forming stars, which are the potential cradles of life. Almost all the radiant mass in the Galaxy is in the form of the star that formed billions of years ago. To understand the star formation process and its evolutionary sequences observations of many star-forming regions have been performed over the last few decades but many questions remain unanswered. Pre-stellar cores form due to the gravitational collapse of dense cloud core in the interstellar medium (ISM), which consist of di use clouds, hot and warm clouds, molecular clouds etc. These clouds show a large range of temperature (10ð€€€104 K) and densities (100ð€€€108 H atoms cmð€€€3). The possible sites of star formation are various molecular clouds e.g., giant molecular clouds (GMCs), dark molecular clouds (DMCs) and Bok globules (BGs), which are further classi ed into cometary globules (CGs) and bright-rimmed clouds (BRCs) etc. The stars are formed in mainly two ways: spontaneous star formation mode and triggered star formation mode. Study of these processes is crucial to gain insights into the formation of stars and the evolution of molecular clouds. In this thesis, we have studied the triggered star formation mode using magnetic eld geometry, molecular line studies and spectroscopic studies.