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Some recent large-scale events, such as the 2004 Indian Ocean earthquake, have caused the length of a day to shorten by 3 microseconds by reducing Earth's moment of inertia.[48] Post-glacial rebound, ongoing since the last ice age, is also changing the distribution of Earth's mass, thus affecting the moment of inertia of Earth and, by the conservation of angular momentum, Earth's rotation period.[49]

Revolution is often used as a synonym for rotation. However, in many fields like astronomy and its related subjects, revolution is referred to as an orbital revolution. It is used when one body moves around another, while rotation means moving around the axis. For example, the Moon revolves around the Earth, and the Earth revolves around the Sun.

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The movement of the Earth around the Sun in a fixed path is called a revolution. The Earth revolves from west to east, i.e., in the anticlockwise direction. The one revolution of the Earth around the Sun takes around one year or precisely 365.242 days. The revolution speed of the earth is 30 km/s-1.

Revolution refers to Earth's orbital motion around the Sun. The combined effect of Earth's revolution, rotation, and axial tilt produce seasonal variations in the North and South Hemispheres. In general, they influence the global climate, wind and ocean current patterns, and the Sun's heat distribution.

Even though temperature fluctuates slightly during Earth's orbit, these differences have nothing to do with our distance from the Sun. Our planet's seasons and climates can be attributed to the fact that Earth rotates in motion about its central axis and moves in orbital revolution when it travels around the Sun.

A revolution describes Earth's orbital motion around the Sun due to the latter's strong gravitational pull. It takes 365.25 days for Earth to complete one revolution. To compensate for the day and to match the calendar and solar years, a leap day is added every four years. Earth revolves around the Sun at speed ranging from 18.20 to 18.82 miles per second (29.29 to 30.29 kilometers per second).

Earth's constant motion through its rotation and revolution affects various processes such as the movement of surface ocean currents, atmospheric circulation, and distribution of solar radiation on the Earth's surface.

Earth's revolution and axial tilt are the primary factors in the global climate. They ensure that sunlight reaches different areas on Earth. Furthermore, they influence atmospheric and ocean circulation, affecting the planet's climate by redistributing moisture and heat to the surface. For example, areas in the tropics experience warm and relatively wet climates, while temperate regions in the Northern Hemisphere encounter significant temperature changes. On the other hand, the abundance or absence of precipitation dictates the climate in the Southern Hemisphere's temperate areas. Global climate, in general, is produced by dynamic and complex processes influenced by Earth's motions.

Earth has two types of motion: rotation and revolution. Rotation refers to Earth's spinning motion about its axis, while revolution is Earth's motion around the Sun as it follows an elliptical path. Each type of motion explains several phenomena and influences Earth's climate, seasons, air circulation, and ocean current patterns. For example, Earth's rotation is responsible for nighttime and daytime, as each side faces the Sun at different times. It also results in the deflection of wind and ocean currents, known as the Coriolis effect. The occurrence of two high tides and two low tides daily in most coastal regions is another consequence of Earth's spinning motion.

Thankfully, for its inhabitants, the Arctic Circle is not pointed at the sun year-round, and the Antarctic is not always in darkness. They actually experience the same amount of daylight and nighttime over the course of a year. But Earth's axis tilt doesn't change either. What does change is Earth's orientation relative to the Sun. While Earth spins on its axis, it is also traveling around the Sun in orbital revolution. One full orbit around the sun is about 365 Earth days, or one year. The axis tilt remains at 23.4 degrees, but depending on where Earth is in its orbit, the amount of radiation received on different parts of the planet will change.

We already discussed the summer months, and how summertime means more hours of daylight in the Northern Hemisphere and fewer hours in the Southern Hemisphere. During spring and fall months, the axis is tilted neither towards nor away from the sun, and so daylight in both hemispheres is about the same. In the winter months, the axis is pointed away from the sun, causing the Southern Hemisphere to receive more hours of daylight than the Northern Hemisphere. During this time, the Arctic experiences many days of darkness, while the Antarctic gets its due daylight. Seasons are opposite north and south of the equator and are a direct result of Earth's axis tilt combined with its orbital revolution.

The consistencies in seasonal patterns, as caused by Earth's rotation and revolution, help shape the climates, or average weather and seasonal conditions in a given part of the world. The North and South Poles are always colder than equatorial regions, and the temperate zones found in between the tropics and the polar regions tend to have mild climates. Other factors that influence the climate of a given region include proximity to water and permanent wind patterns for that area. Because of Earth's rotation, wind patterns can be fairly constant, as well as ocean surface currents that are generated by wind. Ocean and air movement play a major role in the transportation of heat across the planet.

Because of Earth's spherical shape and axis tilt, incoming radiation is not absorbed evenly across the planet, and this distribution changes with the seasons. Earth's rotation is the cause for the differences in daytime and nighttime as it spins on its axis. When that axis is tilted towards the sun, the Northern Hemisphere receives more radiation than the Southern and vice versa when the axis is tilted away from the sun. The axis tilt doesn't actually change, but its orientation relative to the Sun changes as Earth moves in orbital revolution around the Sun. This motion, combined with the axis tilt, is responsible for our seasons.

A technology revolution in Earth observation sensor design is occurring. This revolution in part is associated with the emergence of CubeSat platforms that have forced a de facto standardization on the volume and power into which sensors have to fit. The extent that small sensors can indeed provide similar or replacement capabilities compared to larger and more expensive counterparts has barely been demonstrated and any loss of capability of smaller systems weighed against the gains in costs and new potential capabilities offered by implementing them with a more distributed observing strategy also has not yet been embraced. This paper provides four examples of observations made with prototype miniaturized observing systems, including from CubeSats, that offer a glimpse of this emerging sensor revolution and a hint at future observing system design.

Somewhat independent of these great challenges is a technology revolution that is occurring before us. Much of the recent discussion about technology innovation of spaceborne systems has revolved around discussion of CubeSat capabilities (National Academies of Sciences, Engineering, and Medicine 2016) and the affordable access to space that such capabilities offer. Spacecraft miniaturization, more generally including and beyond CubeSats, is indeed one important factor in the developing revolution. However, this revolution runs much deeper. The aspect of the miniaturization revolution that is critical to Earth sciences is that of sensor design also aided by advances in detector and other system technology. CubeSat development played a role in advancing this development by providing a de facto standardization that, in concrete terms, sets design principles with specifications on the volume and power into which sensors have to fit. This paper does not focus on the evolving CubeSat or small satellite capabilities [e.g., refer to Millan et al. (2019) for a review] and is not meant to imply these small platforms are yet a replacement for larger more capable systems. The intent of the paper is to provide the reader with a genuine sense for what is occurring in sensor miniaturization today that is the ultimate engine of the observational revolution proposed. Although the examples presented in the next section, are, for the most part, from technical demonstration missions currently in orbit, they provide a view of the future of Earth observations.

Predicting across the time scale from weather to climate is a huge challenge that in part requires the development of affordable, connected observing systems that further advance our understanding of subsystem interactions and provide these over a range of time scales typical of weather prediction to understanding and prediction of changes on decadal and longer time scales. As illustrated in this paper, we are now witnessing a revolution in space engineering that offers some hope for addressing such formidable challenges. We now witness the emergence of reusable launchers that are reducing the cost of access to space. The cost of making observations will also potentially reduce with the miniaturization activities like those highlighted in this paper that both reduce cost of sensors and reduce the effective cost of launch by increased potential for shared launches of multiple small platforms. 17dc91bb1f