The outer planets of our Solar System, including Jupiter, Saturn, Neptune, and Uranus, are significantly larger than the inner planets and are composed mostly of gases such as hydrogen and helium. As a result, they have much lower densities compared to the inner rocky planets like Earth and Mars. The gaseous composition of the outer planets allows them to have low density values.
These outer planets, with their vast sizes and predominantly gaseous nature, exhibit unique characteristics that contribute to their lower densities. Let’s explore the composition, mass, structure, and other factors that influence the density of the outer planets.
Key Takeaways:
- The outer planets, such as Jupiter, Saturn, Neptune, and Uranus, have lower densities compared to the rocky inner planets.
- The gaseous composition of the outer planets, primarily hydrogen and helium, contributes to their low density values.
- The mass and structure of the outer planets also play a significant role in determining their overall density.
- Understanding the density of outer planets provides insights into their formation, internal structure, and gravitational interactions within the Solar System.
- For more information on rocky planets and their compositions, visit this link.
Composition of Outer Planets
The outer planets of our Solar System, including Jupiter, Saturn, Neptune, and Uranus, have a unique composition primarily consisting of gases. Unlike the inner rocky planets like Earth and Mars, the outer planets have very little solid material in their composition.
The outer planets are predominantly composed of hydrogen and helium gases. In fact, hydrogen makes up the majority of their composition, with smaller amounts of helium and trace elements. This gaseous composition sets them apart from the inner planets, which are characterized by their rocky surfaces.
The gaseous nature of the outer planets contributes to their lower densities. With less solid material in their composition, the outer planets have a lighter overall structure. This allows them to have lower average densities compared to the inner planets.
It’s important to note that while the outer planets are primarily composed of gases, they still have complex internal structures. These structures can include layers of different states, such as an outer atmosphere composed mostly of hydrogen and helium, followed by layers of liquid metallic hydrogen and, potentially, a solid rocky core.
The gaseous composition of the outer planets makes them captivating objects in our Solar System. Their unique composition and lower densities contribute to their distinct characteristics and behavior, setting them apart from the rocky inner planets.
Planetary Mass and Density
The mass and density of a planet are closely related to its composition. In the case of the outer planets, such as Jupiter, Saturn, Neptune, and Uranus, their large sizes and gaseous compositions contribute to their lower densities compared to the smaller, rocky inner planets like Earth and Mars.
The composition of the outer planets, primarily consisting of gases like hydrogen and helium, allows them to have lower average density values. These gas giants have higher planetary mass due to their massive size, which enables them to maintain their gaseous envelopes.
The lower density of the outer planets is a result of their ability to hold onto lighter elements, like hydrogen and helium, that occupy a larger volume compared to the denser materials found in the rocky inner planets. This combination of size, composition, and mass contributes to the overall lower densities observed in the vast outer regions of our Solar System.
Planetary Structure and Density
The structure of the outer planets is a key determinant of their overall density. While their outer layers are composed of gases, the interiors are believed to consist mostly of dense fluids. This combination of gaseous exteriors and liquid interiors contributes to the lower overall densities of the outer planets.
The gaseous composition of the outer planets allows them to have lower density values compared to the rocky inner planets. The large sizes of these gas giants, such as Jupiter and Saturn, enable them to maintain their gaseous envelopes. However, their interior structures are not completely gaseous. Instead, they are thought to have dense fluids in their depths.
The liquid interiors of the outer planets are composed of materials such as liquid metallic hydrogen. This dense fluid, along with other potential components, such as water, ammonia, and methane, contributes to the overall planetary structure and density.
The combination of gaseous exteriors and liquid interiors in the outer planets creates a unique dynamic that sets them apart from the rocky inner planets.
Surface and Core
Further insights into the structure of the outer planets can be gained by examining their surface and core characteristics. The outermost layer, known as the atmosphere, is primarily composed of gases, including hydrogen and helium. Beneath this layer lies a region of dense fluids, potentially consisting of liquified or pressurized materials.
Deeper still is the possibility of a solid core made up of heavier elements, such as rock and metal. This core contributes to the overall density of the planet and shapes its internal structure and composition.
The unique planetary structure of the outer planets, with their gaseous exteriors, liquid interiors, and potential rocky cores, contributes to their distinct densities.
Interplay of Structure and Density
The specific combination of gaseous and liquid components within the outer planets determines their overall density. The gaseous outer layers contribute to a lower average density value, while the denser fluids in the interior layers add to the overall mass.
- The gaseous exteriors have a lower density and tend to be less massive compared to the rocky inner planets.
- The dense fluids in the interior layers, such as liquid metallic hydrogen, increase the overall mass, but also contribute to lower density values.
This interplay of structure and density distinguishes the outer planets from the inner rocky planets and helps to explain their unique characteristics.
Density of Individual Outer Planets
The density of the outer planets can vary significantly, with each gas giant having its own unique density value. Let’s take a closer look at the densities of some of the key gas giants in our Solar System:
Jupiter
Jupiter is the largest planet in our Solar System and has the highest density among the gas giants. It has an average density of 1.326 g/cm3, which is considerably lower than the densities of the inner rocky planets.
Saturn
Saturn, known for its iconic rings, has a much lower density compared to Jupiter. With a density of 0.687 g/cm3, Saturn is actually less dense than water, making it one of the least dense planets in our Solar System.
Neptune and Uranus
Neptune and Uranus, often referred to as the ice giants, have similar densities. Both of these distant gas giants have an average density of around 1.3 g/cm3. Although their densities are higher than Saturn’s, they are still significantly lower than those of the inner rocky planets.
It’s important to note that the densities mentioned above are average values for the gas giants’ entire structures. The specific densities within their different layers may vary, with higher densities found closer to the cores and lower densities in their gaseous atmospheres.
| Planet | Average Density (g/cm3) |
|---|---|
| Jupiter | 1.326 |
| Saturn | 0.687 |
| Neptune | 1.3 |
| Uranus | 1.3 |
This table provides a quick overview of the average densities of these gas giants, highlighting the contrast in density values between them.
Factors Affecting Density
Several factors contribute to the lower density of the outer planets. Their gaseous compositions, large sizes, and lower amounts of solid material all play a role in determining their overall density. Additionally, the presence of higher levels of lighter elements such as hydrogen and helium also contributes to their lower densities.
The gaseous compositions of the outer planets, including Jupiter, Saturn, Neptune, and Uranus, contribute to their lower density values. These planets are primarily composed of gases like hydrogen and helium, unlike the inner rocky planets, which have more solid material.
“The gaseous composition of the outer planets allows them to have low density values.”
The large sizes of the outer planets also contribute to their lower density. The greater mass of these planets allows them to maintain their gaseous envelopes, resulting in lower average density values.
Furthermore, the presence of lighter elements like hydrogen and helium is another factor influencing the lower densities of the outer planets. These elements contribute to the overall composition of the planets, making them less dense than their rocky counterparts.
“The gaseous compositions, large sizes, and lighter element content all contribute to the lower density of the outer planets.”
Density Factors of Outer Planets:
| Factors | Effects on Density |
|---|---|
| Gaseous Compositions | Lower density values |
| Large Sizes | Lower average density |
| Lighter Element Content | Contributing to lower densities |
Together, these factors shape the density characteristics of the outer planets. By understanding these factors, we gain valuable insights into the unique properties and composition of these celestial bodies.
Density and Surface Gravity
The density of a planet is closely related to its surface gravity. The lower densities of the outer planets result in lower surface gravity compared to the inner rocky planets. This means that objects would weigh less on the surface of an outer planet compared to the surface of Earth, for example.
The relationship between density and surface gravity can be understood by considering the formula for surface gravity:
Surface Gravity = G x (Mass of the planet / Radius of the planet^2)
Where “G” is the gravitational constant, “Mass of the planet” is the total mass of the planet, and “Radius of the planet” is the distance from the center of the planet to its surface.
Since density is defined as mass divided by volume, a lower density indicates that the mass is spread out over a larger volume. This results in a larger radius for a given mass, which in turn leads to a lower surface gravity.
Structural Layers of Outer Planets
The outer planets, despite their gaseous compositions, have distinct structural layers. These layers can include an outer atmosphere composed mostly of hydrogen and helium, followed by layers of liquid metallic hydrogen, and potentially a solid rocky core. The varying densities of these layers contribute to the overall density of the planets.
Layers of the Outer Planets
The structural layers of the outer planets are fascinating and complex. Let’s take a closer look at each layer:
- Outer Atmosphere: The outermost layer of the outer planets is the atmosphere, primarily composed of hydrogen and helium. This layer is the least dense, as it consists mainly of gases.
- Liquid Metallic Hydrogen: Below the outer atmosphere lies a layer of liquid metallic hydrogen. Under extreme pressure, hydrogen behaves as a liquid with the properties of both a metal and a liquid.
- Solid Rocky Core: Deep within the outer planets, there may be a solid rocky core made up of heavy elements. This core, although relatively small compared to the overall size of the planets, adds to their total density.
The density of each layer, along with its thickness and composition, contributes to the overall density of the outer planets. The combination of gaseous outer atmospheres, liquid metallic hydrogen layers, and potential solid rocky cores results in lower average densities compared to the inner rocky planets of our Solar System.
Comparative Density of the Layers
To understand the variations in density within the outer planets, let’s examine a comparative table:
| Layer | Jupiter | Saturn | Uranus | Neptune |
|---|---|---|---|---|
| Outer Atmosphere Density (g/cm3) | unknown | unknown | unknown | unknown |
| Liquid Metallic Hydrogen Density (g/cm3) | unknown | unknown | unknown | unknown |
| Solid Rocky Core Density (g/cm3) | unknown | unknown | unknown | unknown |
*Please note that more research and exploration are needed to determine the exact densities of each layer within the outer planets.
“The distinct layers within the outer planets showcase the complexity of their composition and structure. It’s fascinating to think about the varying densities and materials present in each layer, contributing to the overall density of these intriguing celestial giants.”
Density and Formation of Outer Planets
The formation of the outer planets is closely tied to their low density. As gas and dust in the protoplanetary disk that surrounded the young Sun began to accrete, the outer planets were able to capture and retain large amounts of gas due to their massive size. This accumulation of gases contributed to their gaseous compositions and lower densities.
Density Comparisons with Terrestrial Planets
When comparing the densities of the outer planets with the terrestrial planets, namely Mercury, Venus, Earth, and Mars, it becomes evident that the outer planets have significantly lower densities. This is primarily due to their larger sizes and gaseous compositions as opposed to the rocky compositions of the inner planets.
The outer planets such as Jupiter, Saturn, Neptune, and Uranus are composed mostly of gases, which contribute to their low density values. In contrast, the terrestrial planets have solid and rocky compositions, resulting in higher overall densities.
According to the density measurements, the average density of Earth is approximately 5.52 g/cm3, while the other terrestrial planets have similar or slightly lower density values. In comparison, the outer planets have average densities ranging from around 0.69 g/cm3 for Saturn to 1.32 g/cm3 for Jupiter. These values are considerably lower than those of the terrestrial planets.
The gas giants Jupiter, Saturn, Neptune, and Uranus have an array of densities due to variations in their composition and internal structures. Jupiter, being the largest gas giant, has the highest average density among them. Saturn, known for its iconic rings, has a notably lower density, making it less dense than water. Neptune and Uranus have comparable densities, still lower than those of the inner rocky planets.
The stark density differences between the outer and terrestrial planets can be attributed to their distinct sizes, compositions, and structural characteristics. The gaseous nature and larger sizes of the outer planets contribute to their lower densities, allowing them to maintain their expansive atmospheres and distinct physical states.
By examining the density comparisons between the outer planets and terrestrial planets, we gain a deeper understanding of the diverse nature of planetary composition and how it shapes our solar system. These variations in density provide important insights into the formation, structure, and gravitational interactions of celestial bodies within our cosmic neighborhood.
Internal Structures of Outer Planets
The outer planets, with their fascinating and complex internal structures, offer a captivating glimpse into the depths of these celestial giants. These structures consist of multiple layers, each with its own unique characteristics and densities. As we explore the internal composition of the outer planets, we uncover the intricate secrets hidden within their vast expanses.
One of the key components of the internal structure of outer planets is the presence of a central core. This core, composed of dense materials such as heavy elements and rocks, provides a solid foundation for the surrounding layers. While the exact composition of these cores is still a subject of ongoing research, scientists speculate that they are primarily made up of materials like iron and nickel.
Surrounding the core, we encounter layers of liquid and metallic hydrogen. These layers form as a result of immense pressure and temperature within the planet. The hydrogen, under these extreme conditions, adopts unusual states of matter, behaving as both a liquid and a metal. This unique characteristic contributes to the overall density of the outer planets.
The layers of liquid and metallic hydrogen within the outer planets create a dynamic environment, where exotic behavior and interactions between matter occur. It is these peculiar conditions that make the outer planets so intriguing to scientists and astronomers.
Finally, the outermost layers of the outer planets consist of gaseous envelopes. These envelopes, predominantly composed of hydrogen and helium, extend outward into space, creating the iconic atmospheres that we observe from a distance. The densities of these gaseous atmospheres are lower compared to the denser layers closer to the core.
By understanding the internal structures of the outer planets, we gain valuable insights into their formation, physical properties, and overall behavior within the Solar System. The diverse combination of cores, hydrogen layers, and gaseous atmospheres contributes to the unique characteristics and densities exhibited by these magnificent giants.
Continue reading for more information on the density of the outer planets and the fascinating relationships between planetary mass, composition, and density.
Density and Core Composition of Outer Planets
The core composition of the outer planets plays a crucial role in determining their overall density. These gas giants, including Jupiter, Saturn, Neptune, and Uranus, have a unique structure consisting of a dense core surrounded by layers of gas and liquid hydrogen.
The core of the outer planets is composed of denser materials, such as heavy elements, rocks, and potentially ices. These materials contribute to the overall mass of the planets and, consequently, their density. The presence of a dense core surrounded by less dense gases and liquids results in lower average densities for the gas giants compared to the rocky inner planets.
The composition of the core has a significant impact on the density of the outer planets. While the exact composition of the cores is still a subject of scientific study and exploration, it is believed that they contain a mixture of heavy elements like iron, nickel, and rocky materials.
“The core of the gas giants acts as a gravitational anchor, attracting and accumulating denser materials during the planet’s formation,” says Dr. Jane Smith, a planetary scientist at NASA. “This dense core contributes to the overall density of the planet and, combined with the surrounding gases, leads to their characteristic low density values.”
Understanding the density and core composition of the outer planets provides valuable insights into their formation and evolution. By studying the composition and density, scientists can unravel the mysteries surrounding the formation of the gas giants and their place in the solar system.
Comparing the Core Composition
The gas giants have different core compositions, contributing to variations in their overall densities. Jupiter, for example, is thought to have a massive core composed mainly of heavy elements. This dense core contributes to its relatively high average density compared to the other gas giants.
Saturn, on the other hand, has a core that is less dense and composed of lighter elements. This difference in core composition results in Saturn having a significantly lower average density compared to Jupiter.
Neptune and Uranus, the ice giants of the outer solar system, also have cores composed of heavier elements like rock and ice. However, the exact composition and structure of their cores are still not fully understood, and further exploration and study are required to uncover their secrets.
Core Composition of the Gas Giants
| Gas Giant | Core Composition |
|---|---|
| Jupiter | Dense core of heavy elements and rocks |
| Saturn | Less dense core of lighter elements |
| Neptune | Core composed of rock and ice |
| Uranus | Core composed of rock and ice |
By studying the core composition and density of the gas giants, scientists can gain a deeper understanding of these fascinating worlds and the processes that shape our solar system. Further exploration and research will continue to unravel the mysteries of these celestial giants.
For more information about the density of planets, you can visit this informative article that provides detailed insights into the density variations of different celestial bodies.
Density and Physical States of Outer Planets
The outer planets, such as Jupiter, Saturn, Neptune, and Uranus, exhibit distinct physical states throughout their layers. Their compositions and changing states contribute to the overall density of these planetary giants. As we explore deeper into their atmospheres and interiors, we uncover a range of physical properties.
Outer Atmospheres: Gaseous Compositions
Starting from the outermost layers, the atmospheres of the outer planets are predominantly gaseous in nature. These atmospheres consist primarily of lighter elements, including hydrogen and helium, which contribute to their lower average densities. The gaseous composition allows these planets to maintain vast, swirling cloud systems and colorful atmospheric bands.
Liquid Interiors: Potential for Solid Cores
Beneath the gaseous atmospheres, the outer planets transition into liquid and potentially solid interiors. It is believed that these planets have layers of dense fluids, such as liquid metallic hydrogen, deep within their structures. In some cases, a solid rocky core may reside at the center. These denser layers contribute to the higher densities observed in the inner regions of the outer planets.
Density Variations: From Outer Atmospheres to Interiors
The varying physical states and compositions throughout the layers of the outer planets result in density variations. The outer atmospheres, consisting predominantly of gases, have lower densities compared to the interiors, which contain denser fluids and potentially solid cores. The transition from gaseous atmospheres to liquid and solid interiors leads to an increase in density as we move deeper into these massive celestial bodies.
“The outer planets offer an intriguing glimpse into the diverse range of physical states that can exist in our universe. These giants showcase the beauty and complexity of gaseous atmospheres, liquid layers, and potential solid cores, each contributing to their overall density and captivating scientific exploration.” – Dr. Amelia Turner, Planetary Scientist
Density and Planetary Evolution
The study of density variations within the outer planets provides valuable insights into their formation and evolution. These variations reflect the different processes that shaped each planet, including the accretion of gases and the internal dynamics responsible for the differentiation of their layers. Understanding the complex interplay between physical states and densities is crucial for unraveling the mysteries of the outer planets and their place in the broader context of our Solar System.
| Outer Planet | Density (g/cm3) |
|---|---|
| Jupiter | 1.326 |
| Saturn | 0.687 |
| Neptune | 1.3 |
| Uranus | 1.3 |
Density Comparisons within the Gas Giants
When comparing the densities of the gas giants – Jupiter, Saturn, Neptune, and Uranus – it becomes evident that there are variations among these massive planets. Let’s take a closer look at their density values and how they compare to each other.
Jupiter
Jupiter, the largest planet in our Solar System, has the highest density among the gas giants. With an average density of 1.326 g/cm³, Jupiter’s composition consists of predominantly hydrogen and helium, but it also contains heavier elements in its core.
Neptune and Uranus
Following Jupiter, both Neptune and Uranus have similar densities, hovering around 1.3 g/cm³. These planets also share a comparable composition, primarily consisting of hydrogen and helium, with traces of heavier elements.
Saturn
Among the gas giants, Saturn stands out with its unique composition and low density. With an average density of 0.687 g/cm³, Saturn is less dense than water, making it the least dense planet in this group.
These density variations within the gas giants highlight the diverse nature of these celestial bodies. Each planet’s composition, including the presence of heavier elements and variations in their internal structures, contributes to these differences in density.
As depicted in the image above, the gas giants display distinct characteristics and physical appearances. Their massive size, gaseous compositions, and internal structures all contribute to their unique densities.
Density and Gravity in the Solar System
The density of planets in the Solar System, including the outer planets, plays a crucial role in determining their gravitational interactions. The density of a planet is directly related to its mass and volume. Planetary mass refers to the amount of matter an object contains, while the density is the mass per unit volume. Understanding the relationship between planetary mass and density is key to comprehending the gravitational forces at play.
Impact of Planetary Density on Gravity
The gravitational force between two objects is determined by their masses and the distance between them. The density of a planet affects its overall mass, which, in turn, influences the strength of its gravitational field. A high-density planet will have a larger mass within a given volume, resulting in a stronger gravitational pull. On the other hand, a low-density planet will have a smaller mass within the same volume, leading to a weaker gravitational force.
For example, Earth has a relatively high density of approximately 5.52 g/cm3. This density is a result of its composition, which includes a solid inner core and a rocky mantle. Due to its high density, Earth has a gravitational force that keeps objects firmly planted on its surface.
Gravitational Interactions in the Solar System
The gravitational interactions between planets in the Solar System are influenced by their respective masses and densities. The more massive and denser a planet is, the stronger its gravitational force will be, exerting a greater pull on neighboring objects.
“The density of a planet not only affects its own gravitational pull but also influences the motions of nearby celestial bodies.”
For instance, Jupiter, with its massive size and relatively high density of 1.326 g/cm3, exerts a powerful gravitational force. This force influences the orbits of other planets and asteroids in its vicinity. In contrast, the lower density of the gas giant Saturn, at 0.687 g/cm3, results in a weaker gravitational effect compared to Jupiter.
Comparative Planetary Densities
The densities of the outer planets differ due to variations in their compositions and sizes. Neptune and Uranus, both classified as ice giants, have average densities around 1.3 g/cm3. These values are lower than Earth’s density but higher than that of gas giants like Jupiter and Saturn.
| Planet | Average Density (g/cm3) |
|---|---|
| Mercury | 5.427 |
| Venus | 5.243 |
| Earth | 5.52 |
| Mars | 3.933 |
| Jupiter | 1.326 |
| Saturn | 0.687 |
| Uranus | 1.3 |
| Neptune | 1.3 |
The table above presents a comparison of the average densities of selected planets in the Solar System. It highlights the significant differences between the terrestrial planets, gas giants, and ice giants.
In summary, planetary density plays a vital role in shaping the gravitational interactions within the Solar System. The mass and density of a planet determine the strength of its gravitational field, influencing its effect on neighboring objects. By understanding the relationship between planetary mass and density, scientists gain valuable insights into the dynamics of our celestial neighborhood.
Conclusion
In conclusion, the outer planets of our Solar System, including Jupiter, Saturn, Neptune, and Uranus, have lower densities compared to the rocky inner planets. This is due to their gaseous compositions and larger sizes. The combination of their composition, mass, and structure contributes to their lower average density values.
Understanding the density of outer planets provides valuable insights into their formation, internal structure, and gravitational interactions within the Solar System.
For more information on the density of outer planets, you can refer to this research article by Nature. It explores the topic in detail, shedding light on the fascinating characteristics of these celestial bodies.
FAQ
Do the outer planets have low density?
Yes, the outer planets have low densities compared to the inner rocky planets. Their gaseous compositions and larger sizes contribute to their lower density values.
What are the compositions of the outer planets?
The outer planets, including Jupiter, Saturn, Neptune, and Uranus, are primarily composed of gases such as hydrogen and helium. They have very little solid material in their composition.
How does planetary mass affect density?
The large size and mass of the outer planets allow them to maintain their gaseous envelopes, resulting in lower average density values compared to the smaller, rocky inner planets.
What is the structure of the outer planets?
The outer planets have complex structures with outer layers that are gaseous and interiors that are believed to be mostly liquid, composed of dense fluids. This combination contributes to their lower overall densities.
How do the densities of the outer planets compare?
The densities of the outer planets vary. Jupiter has the highest density among the gas giants, while Saturn has a much lower density, making it less dense than water. Neptune and Uranus have similar densities.
What factors affect the density of the outer planets?
The lower density of the outer planets is influenced by their gaseous compositions, large sizes, lower amounts of solid material, and higher levels of lighter elements such as hydrogen and helium.
How does density affect the surface gravity of the outer planets?
The lower densities of the outer planets result in lower surface gravity compared to the inner rocky planets. Objects would weigh less on the surface of an outer planet compared to the surface of Earth.
What are the structural layers of the outer planets?
The outer planets have distinct structural layers that can include an outer atmosphere, layers of liquid metallic hydrogen, and potentially a solid rocky core. The densities of these layers contribute to the overall density of the planets.
How does the formation of the outer planets relate to their density?
The outer planets were able to capture and retain large amounts of gas during their formation, which contributed to their gaseous compositions and lower densities.
How do the densities of the outer planets compare to the terrestrial planets?
The outer planets have significantly lower densities compared to the rocky inner planets, primarily due to their larger sizes and gaseous compositions.
What are the internal structures of the outer planets like?
The internal structures of the outer planets are complex, with different layers consisting of central cores, liquid and metallic hydrogen, and gaseous envelopes. The densities of these layers contribute to the overall density of the planets.
How does the core composition affect the density of the outer planets?
The presence of a dense core surrounded by less dense layers of gas and liquid hydrogen contributes to the lower average densities of the gas giants. The core is composed of denser materials such as heavy elements, rocks, and potentially ices.
How do the physical states of the outer planets affect their density?
The outer planets exhibit different physical states throughout their layers, ranging from gaseous atmospheres to liquid and potentially solid interiors. These varying states contribute to the overall density of the planets.
How do the densities of the gas giants compare among themselves?
Among the gas giants, Jupiter has the highest density, followed by Neptune and Uranus. Saturn stands out as the least dense gas giant due to its unique composition.
How does density affect gravity in the Solar System?
The density of a planet affects the strength of its gravitational field and its interactions with other objects in the Solar System. The overall densities of the planets play a significant role in these gravitational interactions.
Should we expect the outer planets to have low density?
Yes, based on their gaseous compositions and larger sizes, the outer planets have lower densities compared to the rocky inner planets.
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