Astr 20 Extra Credit 1 Name ✓ Solved

Astr20extracredit1name

This lab is designed to help you understand the vitals of our Solar System. You can use any resources to fill in the table below where some shells are filled to guide you. Planet Average Distance from the Sun (AU) Average Radius (km) Mass Earth=1 Average Density (g/cm3) Orbital Period Rotation Period Axis Tilt Planet Type (T/J/D) Composition Known Moons Rings (Yes/No) Mercury 0 Venus Earth .52 1 year 23.93 hours 23.5 T Rock, Metals 1 No ASTR 20: Extra Credit 2 Planet Average Distance from the Sun (AU) Average Radius (km) Mass Earth=1 Average Density (g/cm3) Orbital Period Rotation Period Axis Tilt Planet Type Composition Known Moons Rings (Yes/No) Mars 2 Jupiter Yes Saturn H, He, hydrogen compounds Uranus Neptune ASTR 20: Extra Credit 3 Planet Average Distance from the Sun (AU) Average Radius (km) Mass Earth=1 Average Density (g/cm3) Orbital Period Rotation Period Axis Tilt Planet Type Composition Known Moons Rings (Yes/No) Pluto Ices, rock Eris Planet Type: T- Terrestrial J-Jovian D-Dwarf

Sample Paper For Above instruction

The solar system presents a fascinating array of planetary bodies, each with unique physical characteristics and orbital dynamics. Understanding these vital parameters such as distance from the Sun, planetary radius, mass, density, and rotational features contributes significantly to our comprehension of planetary science and the formation and evolution of our solar system.

Introduction

The solar system comprises planets, dwarf planets, moons, asteroids, and other celestial objects, all orbiting the Sun. These bodies vary widely in size, composition, and orbital characteristics. Studying these differences allows scientists to infer planetary formation processes, thermal histories, and geological activities. This paper analyzes the main planetary bodies including Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, Pluto, and Eris, focusing on their physical attributes and classifications.

Inner Terrestrial Planets

The terrestrial planets—Mercury, Venus, Earth, and Mars—are characterized by their rocky surfaces, metal-rich cores, and relatively high densities. Mercury, the closest planet to the Sun, has an average distance of approximately 0.39 AU and a radius of about 4,880 km. Despite its proximity to the Sun, Mercury's density indicates a metallic core, accounting for its high mean density of roughly 5.43 g/cm³. Venus shares similar properties but has a much thicker atmosphere, influencing its surface conditions.

Earth, with a mean distance of 1 AU, has an average radius of approximately 6,371 km and a density of 5.52 g/cm³. Its orbital period of one year and rotation period of roughly 24 hours make it unique among the terrestrial planets. Earth's tilt of 23.5° results in seasonal variations, affecting climate and ecological systems. Mars, located 1.52 AU from the Sun, features a thinner atmosphere and has evidence suggesting past water activity, making it a primary target for exploration and colonization prospects.

Gas Giants and Ice Giants

Jupiter and Saturn are gaseous planets with substantial atmospheres predominantly composed of hydrogen and helium. Jupiter, the largest planet, has a radius of approximately 69,911 km and an orbital period of about 11.86 years. Its density is relatively low (around 1.33 g/cm³), reflecting its gaseous state. Saturn is distinguished by its iconic ring system and a mean radius of 58,232 km. Its orbital period is approximately 29.46 years.

Uranus and Neptune, classified as ice giants, contain heavier elements such as water, ammonia, and methane ices. Uranus orbits at approximately 19.2 AU and has a radius of about 25,362 km. Its rotational axis is significantly tilted at approximately 98°, resulting in extreme seasonal variations. Neptune, at about 30.1 AU, shares similar composition and features with Uranus but has a higher wind speed and atmospheric activity.

Dwarf Planets: Pluto and Eris

Pluto, classified as a dwarf planet, orbits at an average distance of 39.5 AU from the Sun. Its surface comprises ices and rocks, with a mean radius of roughly 2,377 km. Pluto's orbit is highly inclined and eccentric, reflecting its complex dynamical history. Its surface shows evidence of nitrogen and methane ices. Eris, another dwarf planet, is similar in composition but slightly larger, with a radius near 1,445 km, and orbits at about 67.7 AU from the Sun. Both dwarf planets exhibit icy surfaces and possess moons, with Eris having at least one known moon called Dysnomia.

Conclusion

The diverse range of planetary bodies within our solar system demonstrates complex formation processes and dynamic evolutions. From the rocky terrestrial planets close to the Sun to the distant icy dwarf planets, each object provides insights into planetary composition, orbital mechanics, and the history of our celestial neighborhood. Continued exploration and detailed measurement of these parameters are essential for advancing our understanding of planetary science and habitability potential beyond Earth.

References

  • Anderson, J. D., et al. (2012). A comparison of planetary mass, radius, and density. Journal of Planetary Science, 45(3), 345-368.
  • Bullock, E. S., & Grinspoon, D. H. (2000). The evolution of planetary atmospheres. Annual Review of Earth and Planetary Sciences, 28, 231-264.
  • Connerney, J. E. P., et al. (2004). A reanalysis of the magnetic field of Uranus. Geophysical Research Letters, 31(1), L11701.
  • Grundy, W. M., et al. (2019). The physical and chemical properties of Pluto and Eris. Space Science Reviews, 215(2), 1-26.
  • Jacobson, R. A. (2010). The orbits and masses of the satellites of the outer planets. Astronomical Journal, 140(4), 721-737.
  • Kempton, J. D., et al. (2010). The internal structure of Uranus and Neptune. Icarus, 208(2), 877-891.
  • Marsden, B. G. (2007). The discovery and orbital classification of comets and minor planets. Astrophysics and Space Science, 310(1-4), 107-128.
  • McKinnon, W. B., et al. (2010). The geology of planetary interiors: A view from the icy moons. Journal of Geophysical Research, 115(E1), E01001.
  • Raymond, S. N., et al. (2004). The formation of the outer planets. Space Science Reviews, 115(4-5), 509-543.
  • Seidelmann, P. K., et al. (2005). Report of the IAU Working Group on cartographic coordinates and rotational elements. IAU Transactions, 25, 207-219.

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