Abstract
The study of protoplanetary disk formation and its connection with Solar system’s origin is considered to be one of the longest-standing problems in astronomy and astrophysics. To the current human understanding, planets are believed to be the hosts of life. Therefore, understanding the dynamic process affecting the formation of protoplanetary disk leads to predicting the origin of our Solar system. The fundamental question we raise here is how the properties of the surrounding gas and dust, which provide mass for the disk and central protostar formations, affect the properties of the protoplanetary disk. This paper investigates how the infalling core’s magnetic field, rotation and turbulence govern the protoplanetary disk formation. The theoretical model we have developed and the numerical results generated from the theoretical model show that a strongly magnetized and rotating core results in a relatively massive protoplanetary disk. Moreover, most of the disk’s angular momentum is removed outwards due to the infalling core’s magnetic field and its rotation speed.
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Notes
Zhang et al. (2014) defined molecular clump as an entity of 1 pc that forms massive stars with a population of lower mass stars, and dense cores as an entity of 0.01–0.1 pc that forms one or a group of stars.
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Acknowledgements
We gratefully acknowledge Space Science and Geospatial Institute (SSGI), Entoto Observatory and Research Center (EORC), Department of Astronomy and Astrophysics. East African Astrophysics Research Network (EAARN) and International Science Programme (ISP)-Uppsala University are also gratefully recognized for their support this research.
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Kumssa, G.M., Tessema, S.B. Protoplanetary disk formation in rotating, magnetized and turbulent molecular cloud. J Astrophys Astron 44, 70 (2023). https://doi.org/10.1007/s12036-023-09960-w
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DOI: https://doi.org/10.1007/s12036-023-09960-w