Related Experiment Video
Updated: Mar 19, 2026
11:34
Scattering And Absorption of Light in Planetary Regoliths
Published on: July 1, 2019
11.1K
Obliquity Variability of a Potentially Habitable Early Venus
Jason W Barnes1, Billy Quarles2,3, Jack J Lissauer2
11 Department of Physics, University of Idaho , Moscow, Idaho. Researcher ID: B-1284-2009.
Astrobiology
|June 22, 2016
Summary
Early Venus may have had a rapidly rotating state, influencing its obliquity variations. Unlike Earth, its obliquity dynamics were simpler, with a single chaotic regime at high prograde inclinations.
Area of Science:
- Planetary Science
- Astrobiology
- Solar System Dynamics
Background:
- Venus's current slow rotation is influenced by thermal tides.
- Early Venus, 4 billion years ago, may have had a fainter Sun and a low-mass atmosphere with solid carbon.
Purpose of the Study:
- Investigate obliquity variations for a hypothetical rapidly rotating Early Venus.
- Compare obliquity dynamics of Early Venus to Earth's hypothetical moonless state.
Main Methods:
- Simulated obliquity variations for an ensemble of hypothetical Early Venus models.
- Analyzed obliquity variation structures and long-term variability.
Main Results:
- Early Venus's obliquity variation structure is simpler than a moonless Earth's, featuring one primary chaotic regime at high prograde obliquities.
- Retrograde Venuses exhibited unexpected long-term variability up to ±7°.
- Low-obliquity Venuses displayed minimal variability over billion-year timescales, similar to the Moon-influenced Earth.
Conclusions:
- Hypothetical rapidly rotating Early Venus had distinct obliquity dynamics.
- Obliquity stability on Early Venus varied significantly with rotation direction and initial obliquity.
Related Concept Videos
01:27Eccentricity of an Ellipse
509
An ellipse is a fundamental conic section defined by the constant sum of distances from any point on its curve to two fixed points, known as the foci. This geometric property can be physically demonstrated using a pencil, string, and two pins. By anchoring the string at both ends and maintaining it taut with a pencil, one can trace the outline of an ellipse.The shape and extent of the ellipse are determined by its eccentricity, e, defined as the ratio of the distance between the center and a...
509
01:10Kepler's First Law of Planetary Motion
5.9K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. He formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe.
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
On the other hand,...
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
On the other hand,...
5.9K
01:18Kepler's Third Law of Planetary Motion
4.5K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. In 1909, he formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe. However, in 1918, he published his third law of planetary motion, which gives a precise mathematical relationship between a planet's average distance from the Sun and the amount of time it takes to revolve around the Sun. It...
4.5K
01:29Kepler's Second Law of Planetary Motion
5.6K
In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. His first law states that all planets orbit the Sun in an elliptical orbit, with the Sun at one of the ellipse's foci. Therefore, the distance of a planet from the Sun varies throughout its revolution around the Sun.
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
5.6K
01:16Circular Orbits and Critical Velocity for Satellites
5.6K
The Moon orbits around the Earth. In turn, the Earth (and other planets) orbit the Sun. The space directly above our atmosphere is filled with artificial satellites in orbit. One can examine the circular orbit, the simplest kind of orbit, to understand the relationship between the speed and the period of planets and satellites with respect to their positions and the bodies that they orbit.
Nicolaus Copernicus (1473-1543) first suggested that the Earth and all other planets orbit the Sun in...
Nicolaus Copernicus (1473-1543) first suggested that the Earth and all other planets orbit the Sun in...
5.6K
02:06Conditions on Early Earth
102.8K
Around 4 billion years ago, oceans began to condense on earth while volcanic eruptions released nitrogen, carbon dioxide, methane, ammonia, and hydrogen into the primordial atmosphere. However, organisms with the characteristics of life were not initially present on earth. Scientists have used experimentation to determine how organisms evolved that could grow, reproduce, and maintain an internal environment.
102.8K