Determination of Orbital Time Period of Revolution Dwarf Planets Around the Sun using Kepler’s Third Law of Planetary Motion and Python - Pluto, Eris, Haumea, Makemake, Gonggong, Quaoar, Sedna, Orcus and Salacia

International Journal of Applied Physics

© 2024 by SSRG - IJAP Journal

Volume 11 Issue 2

Year of Publication : 2024

Authors : Shobhini Khanna

10.14445/23500301/IJAP-V11I2P103

How to Cite?

Shobhini Khanna, "Determination of Orbital Time Period of Revolution Dwarf Planets Around the Sun using Kepler’s Third Law of Planetary Motion and Python - Pluto, Eris, Haumea, Makemake, Gonggong, Quaoar, Sedna, Orcus and Salacia," SSRG International Journal of Applied Physics, vol. 11,  no. 2, pp. 1-5, 2024. Crossref, https://doi.org/10.14445/23500301/IJAP-V11I2P103

Abstract:

Dwarf Planets do not classify as planets as most of them do not clear the neighborhood around their orbit, for example, Pluto. Some of the biggest dwarf planets are found farther than Neptune’s distance, which is 30 AU. This makes it hard for an observational study of these dwarf planets the determination their orbital period around the sun. In this paper, we use Kepler’s third law of motion to determine the theoretical orbital period of some of the biggest dwarf planets. Firstly, using the orbital time and semi-major axis of the eight planets in the solar system, namely, Mercury, Venus, Earth, Mars, Jupiter, Saturn and Neptune, the mass of the sun using average and graphical methods is calculated, the results were 2.0355 ∗ 10 30 Kg and 2.2289 ∗ 10 30Kg, respectively. Using Kepler’s third law, T = √(4Π²/GM)R³, where R is the semi-major axis, G is the universal constant of gravity, M is the mass of the sun, and the orbital time period(T) of dwarf planets is determined. This paper suggests the orbital time period of the dwarf planets Pluto, Eris, Haumea, Makemake, Gonggong, Quaoar, Sedna, Orcus and Salacia are about 236, 910, 213, 310, 794, 261, 736, 320, 265 years.

Keywords:

Dwarf planets, Planets, Kepler’s Law, Orbital period, Semi-major axis.

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