what is meant by the yearly motion of the earth?
352683
The earth has several different movements. First, it rotates on its axis, which takes 24 hours. During this period, the parts of the earth that face toward the sun experience day, while the parts that face away from the sun experience night. Second, the earth revolves around the sun.. in a large elliptical orbit. This process takes a year. The earth's journey around the sun along with the earth's tilting axis produce the seasons. Third, the earth, sun and other planets are all moving within the galaxy, but this is on a very large scale, and is not really noticeable or of interest to most people.\n\nTo sum up:\nmovement of the earth on its axis: rotation. it takes 24 hours.\nmovement of the earth around the sun: revolution. it takes 365.24 days.
131841
The seasons would be far milder. There probably still would be some seasonal variations because the earth is not always the same distance from the sun.\n\nAlso, it should be noted that even if the axis of rotation was oriented to be normal to the ecliptic, there is still a 435 day period Chandler Wobble to the earth's axis, caused by redistribution of mass on the earth's surface (and presumably within the earth as well) and the conservation of angular momentum.
1186913
Because the way the earth is tilted on its axises during that part of the year
655853
Precession! The shape of Earth’s orbit becomes more or less oval (eccentricity), Earth wobbles as it spins (precession), and Earth's axis changes too (tilt). All these changes, over thousands of years, causes Earth's climate to change.
199932
The earth's rotation.
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None, the two are not related. Earth's rotation is a measure of time and light years are a measure of distance.
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The Earth orbits the sun at an average speed of 67,000 mph in a counterclockwise direction when viewed from above it's North Pole.
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The axis of the earth shifts seasonally.
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An earth year (Gregorian calendar) is 365.2425 days \n= 31,556,952 seconds.\n\nA jovian year (one orbit of Jupiter around the sun) is 11.86 earth years.\n= 374,265,450 seconds.
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If it's the big picture you're looking at, a year is the time it takes for the earth to make one revolution around the sun. The earth is thought to be some 4 billion years old.\n\nA decade is ten years. A century is one hundred years. A millenium is one thousand years.
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The rotation of the Earth on it's axis does not vary, but the speed of orbit about the sun does, to a tiny degree.  Earth is slightly closer to the sun in the winter months, thus orbits slight faster (and I mean infinitesimally faster).\nAs far as speed- Earth is about 25,000 miles in circumference, if orbits exactly once a day (24 hours) to the speed is a little over 1,000 miles an hour.\nEarth is 93 million miles from the sun, on average-this means the total orbital distance is 93 million X 2 X 3.14 = 584 million miles.  It goes this far in exactly 1 year-364.8 day or (364.8 X 24) 8733 hours. So, 584 million/8733 = about 66,500 miles/hour.  I just checked online and it says about 65,000, so there ya go
375210
Mountains, bodies of water and seasonal tilt in the earths axis. That's the whole 9 yeards.
16582
to tell you with approximate data the earth completes it revolution in 356 and a quarter days. This 1/4 adds up to one full day every 4 years. Thus we need to have this compensatory extra day every four years.
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If you're speaking of the motion of Earth on it's axis or it's rotation about the sun, the answer is the scientific principle of Inertia, read now!\n\nThe principle of inertia is one of the fundamental laws of classical physics which are used to describe the motion of matter and how it is affected by applied forces.Inertia is the property of an object to resist changes in velocity unless acted upon by an outside force.Inertia is dependent upon the mass and shape of the object. The concept of inertia is today most commonly defined using Sir Isaac Newton's First Law of Motion, which states:\n\nEvery body perseveres in its state of being at rest or of moving uniformly straight ahead, except insofar as it is compelled to change its state by forces impressed. [Cohen & Whitman 1999 translation]\n\nThe description of inertia presented by Newton's law is still considered the standard for classical physics. However, it has also been refined and expanded over time to reflect developments in understanding of relativity and quantum physics which have led to somewhat different (and more mathematical) interpretations in some of those fields.\n\nNow read more at the links below:
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If you were to view the Earth from above the North Pole, it will be rotating in an anticlockwise direction (i.e. West to East).\n\nEarth rotates about an axis, where 1 rotation equates to 24 hours (1 day). This axis is at a tilt of 23.45 degrees from the vertical. This tilting results in the seasons.\n\nA cool "video" can be found on: http://www.ncsu.edu/scivis/lessons/earthinspace3d/earth2.html
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Earth rotates. Sun on one side.
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A special case of annual aberration is the nearly constant deflection of the Sun from its true position by κ towards the west (as viewed from Earth), opposite to the apparent motion of the Sun along the ecliptic. This constant deflection is often erroneously explained as due to the motion of the Earth during the 8.3 minutes that it takes light to travel from the Sun to Earth. The latter is a type of parallax, and actually causes the apparent motion of the Sun along the ecliptic towards the east relative to the fixed stars. (8.316746 minutes divided by one sidereal year (365.25636 days) is 20".49265, very close to κ, but of opposite sign, east vs. west.) Nor is this the Sun's light-time correction because the Sun is almost motionless, moving around the barycenter (center of mass) of the solar system by usually much less than 0".03 (as viewed from Earth) during 8.3 minutes.\n\nAberration can be resolved into an east-west and north-south component on the celestial sphere, which therefore produce an apparent displacement of a star's right ascension and declination, respectively. The former is larger (except at the ecliptic poles), but the latter was the first to be detected. This is because very accurate clocks are needed to measure such a small variation in right ascension, but a transit telescope calibrated with a plumb line can detect very small changes in declination.