International Journal of Astrophysics and Space Science

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Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud

Received: 19 October 2023    Accepted: 2 November 2023    Published: 30 November 2023
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Abstract

The formation of the protoplanetary disc is a crucial step in planetary system formation. The study of protoplanetary disk formation is important for understanding the origins of our solar system as well as planets orbiting other stars. Many studies of protoplanetary disc formation focus on the initial properties of the planetary disc, such as mass, radius, and density, rather than the parent cloud properties. As a result, we’re looking into the formation of the protoplanetary disc in the context of the central star-forming core and the parent cloud parameters. Thus we derive numerical results from the theoretical model using boundary conditions, confirming the presence of a correct link between the features of the developing disk, parent cloud, and central core. In theory, we model the disc’s mass, density, and temperature in terms of the parent cloud and the center core’s attributes. In addition, using the mass-momentum transfer method in conjunction with the newly formulated disc mass and the associated host star, we determine the masses of the disk and core. We also explain how the magnetic field affects disc formation by formulating the mass of the disc formed from a magnetized cloud. The findings reveal that the properties of the parental cloud and the host star have a significant impact on the formation of a protoplanetary disc and its essential dynamic parameters, such as mass, surface density, and mass density.

DOI 10.11648/j.ijass.20231102.12
Published in International Journal of Astrophysics and Space Science (Volume 11, Issue 2, June 2023)
Page(s) 23-37
Creative Commons

This is an Open Access article, distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution and reproduction in any medium or format, provided the original work is properly cited.

Copyright

Copyright © The Author(s), 2024. Published by Science Publishing Group

Keywords

Molecular Cloud, Self-gravitating, Protostellar Core, Protostar, Protoplanetary Disk, Planetary System, Accretion

References
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Cite This Article
  • APA Style

    Muleta Kumssa, G., Belay Tessema, S. (2023). Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud. International Journal of Astrophysics and Space Science, 11(2), 23-37. https://doi.org/10.11648/j.ijass.20231102.12

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    ACS Style

    Muleta Kumssa, G.; Belay Tessema, S. Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud. Int. J. Astrophys. Space Sci. 2023, 11(2), 23-37. doi: 10.11648/j.ijass.20231102.12

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    AMA Style

    Muleta Kumssa G, Belay Tessema S. Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud. Int J Astrophys Space Sci. 2023;11(2):23-37. doi: 10.11648/j.ijass.20231102.12

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  • @article{10.11648/j.ijass.20231102.12,
      author = {Gemechu Muleta Kumssa and Solomon Belay Tessema},
      title = {Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud},
      journal = {International Journal of Astrophysics and Space Science},
      volume = {11},
      number = {2},
      pages = {23-37},
      doi = {10.11648/j.ijass.20231102.12},
      url = {https://doi.org/10.11648/j.ijass.20231102.12},
      eprint = {https://article.sciencepublishinggroup.com/pdf/10.11648.j.ijass.20231102.12},
      abstract = {The formation of the protoplanetary disc is a crucial step in planetary system formation. The study of protoplanetary disk formation is important for understanding the origins of our solar system as well as planets orbiting other stars. Many studies of protoplanetary disc formation focus on the initial properties of the planetary disc, such as mass, radius, and density, rather than the parent cloud properties. As a result, we’re looking into the formation of the protoplanetary disc in the context of the central star-forming core and the parent cloud parameters. Thus we derive numerical results from the theoretical model using boundary conditions, confirming the presence of a correct link between the features of the developing disk, parent cloud, and central core. In theory, we model the disc’s mass, density, and temperature in terms of the parent cloud and the center core’s attributes. In addition, using the mass-momentum transfer method in conjunction with the newly formulated disc mass and the associated host star, we determine the masses of the disk and core. We also explain how the magnetic field affects disc formation by formulating the mass of the disc formed from a magnetized cloud. The findings reveal that the properties of the parental cloud and the host star have a significant impact on the formation of a protoplanetary disc and its essential dynamic parameters, such as mass, surface density, and mass density.},
     year = {2023}
    }
    

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  • TY  - JOUR
    T1  - Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud
    AU  - Gemechu Muleta Kumssa
    AU  - Solomon Belay Tessema
    Y1  - 2023/11/30
    PY  - 2023
    N1  - https://doi.org/10.11648/j.ijass.20231102.12
    DO  - 10.11648/j.ijass.20231102.12
    T2  - International Journal of Astrophysics and Space Science
    JF  - International Journal of Astrophysics and Space Science
    JO  - International Journal of Astrophysics and Space Science
    SP  - 23
    EP  - 37
    PB  - Science Publishing Group
    SN  - 2376-7022
    UR  - https://doi.org/10.11648/j.ijass.20231102.12
    AB  - The formation of the protoplanetary disc is a crucial step in planetary system formation. The study of protoplanetary disk formation is important for understanding the origins of our solar system as well as planets orbiting other stars. Many studies of protoplanetary disc formation focus on the initial properties of the planetary disc, such as mass, radius, and density, rather than the parent cloud properties. As a result, we’re looking into the formation of the protoplanetary disc in the context of the central star-forming core and the parent cloud parameters. Thus we derive numerical results from the theoretical model using boundary conditions, confirming the presence of a correct link between the features of the developing disk, parent cloud, and central core. In theory, we model the disc’s mass, density, and temperature in terms of the parent cloud and the center core’s attributes. In addition, using the mass-momentum transfer method in conjunction with the newly formulated disc mass and the associated host star, we determine the masses of the disk and core. We also explain how the magnetic field affects disc formation by formulating the mass of the disc formed from a magnetized cloud. The findings reveal that the properties of the parental cloud and the host star have a significant impact on the formation of a protoplanetary disc and its essential dynamic parameters, such as mass, surface density, and mass density.
    VL  - 11
    IS  - 2
    ER  - 

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Author Information
  • Space Science and Geospatial Institute (SSGI), Entoto Observatory and Research Center (EORC), Astronomy and Astrophysics Research and Development, Addis Ababa, Ethiopia; Department of Physics, College of Natural Sciences, Jimma University, Jimma, Ethiopia

  • Space Science and Geospatial Institute (SSGI), Entoto Observatory and Research Center (EORC), Astronomy and Astrophysics Research and Development, Addis Ababa, Ethiopia

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