Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud

Gemechu Muleta Kumssa; Solomon Belay Tessema

doi:doi:10.11648/j.ijass.20231102.12

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Protoplanetary Disk Formation in a Self-gravitating Molecular Cloud

Gemechu Muleta Kumssa^*, Solomon Belay Tessema

Published in International Journal of Astrophysics and Space Science (Volume 11, Issue 2)

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.

Published in	International Journal of Astrophysics and Space Science (Volume 11, Issue 2)
DOI	10.11648/j.ijass.20231102.12
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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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

Gemechu Muleta Kumssa

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

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Solomon Belay Tessema

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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Plain Text BibTeX RIS

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}
}

Copy | Download

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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