The Effect of Gaseous Discharge on Star Formation

Krishna Bulchandani; Saptarshi Ghosh; Manisha Chowdhury; Pooja Thakur; Sharry

doi:10.34256/famr2323

Krishna Bulchandani Department of Physics, St. Xavier's College (Autonomous), Mumbai, Maharashtra 400001, India
Saptarshi Ghosh Department of Physics, Ramakrishna Mission Residential College, Narendrapur, Kolkata, West Bengal 700103, India
Manisha Chowdhury Department of Physics, University of Calcutta, Kolkata, West Bengal 700073, India
Pooja Thakur Department of Physics, D.A.V. University, Jalandhar, Punjab 144012, India
Sharry School of Physics, The University of Sydney, Camperdown NSW 2050, Australia

Keywords: Collapse, Molecular clouds, Protostellar, Shockwaves

Abstract

This paper examines how gaseous discharge affects molecular clouds and how that affects star formation. In the magnetic field of the star, electrons, positrons, and ions interact to form the majority of the plasma's chemical makeup. The ZK equations are used for the study of gaseous discharge effects in the presence of shocks and solitons. According to the study, shockwaves produced by gaseous discharge are crucial in creating molecular clouds, which in turn affect the evolution of stars. Within molecular clouds, denser regions develop as a result of the compression of the interstellar medium caused by shockwaves. The gravitational collapse of these squeezed regions promotes the creation of protostellar cores and starts the star-formation process as a result. Shockwaves also affect the motion and turbulence of molecular clouds and improve the amplification of magnetic fields. Clarifying the basic principles regulating star formation and the ensuing creation of stellar populations inside galaxies requires an understanding of the complex interplay between shockwaves and molecular clouds.

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