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 (10104 K) and densities (100108 H atoms
cm3). 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.
