The method used was to carefully time the very rare transit of Venus across the face of the sun. It was 1st attempted by Jeremiah Horrocks from England in 1639 (published in 1661) but he was off by about 100%.
The 1st accurate measurements followed the 1761 and 1769 transits and were done by the French astronomer Jérôme Lalande.
For more details see http://en.wikipedia.org/wiki/Transit_of_Venus#Modern_observations
Aristarchus of Samos made the first (rather inaccurate) measurement. A more accurate measurement was made by Ptolomy.
Eratosthenes, Greek philosopher and scientist. his methods are still unknown. had something to do with apparent angles of the sun at Noon in different locations
The distance between the earth and the sun is about 150 million km .
The solstices are determined by the distance the Earth is from the sun in its orbit. Winter is when the sun is farthest away relative to the Earth's tilt. Summer occurs when the opposite is true.
One "Astronomical Unit" is (more or less) the average distance between the Sun and Earth.
To find the number of light years between two celestial objects, we first find the distance from each object to earth. If we connect the dots between Earth and the two objects, we have a triangle. We to sides lengths of that triangle (the distances between Earth and the objects), and we can measure one angle (the angle at the vertex where Earth is. This is enough information to find the distance between the objects using trigonometry (in this case, the law of cosines). Finding the distance from Earth to an object can be a bit complex. One commonly used method is to look for a pulsating star. We can figure out the absolute brightness (how bright it is without factoring in distance away) of these stars by how often they pulse. Then we can measure the apparent brightness (how bright it looks to us). We can then use both these values to find the distance to the star. (This also works for some supernovae.) Another method is to use objects that are considered to be 'standard candles'. These objects do not pulse, but we know the relationship between their absolute brightness, apparent brightness, and distance away.
An Astronomical Unit (AU) is the average distance between the Earth and the Sun.
The distance between two points is the distance between them. It doesn't depend on the method an object uses to move between the two points. It also doesn't depend on what route an object follows between them, or even whether or not anything moves between the two points. The distance between the earth and the Orion Nebula is the distance, even though no object has ever moved between the earth and the Orion Nebula.
distance between the earth and the sun.
The answer depends on what distance is being determined: the distance to stars using parallax, the distance to aircraft using radar, the distance from one city to another partway around the earth, the distance between two nearby objects.
The same as between the Moon and the Earth. The distance from the clouds to the surface of the Earth is insignificant, compared to the Moon-Earth distance.The same as between the Moon and the Earth. The distance from the clouds to the surface of the Earth is insignificant, compared to the Moon-Earth distance.The same as between the Moon and the Earth. The distance from the clouds to the surface of the Earth is insignificant, compared to the Moon-Earth distance.The same as between the Moon and the Earth. The distance from the clouds to the surface of the Earth is insignificant, compared to the Moon-Earth distance.
One AU is the distance between the Earth and the Sun.
Parallax is the method that astronomers use to measure the distance from the sun to the earth.
scale
The distance between the earth and the sun is about 150 million km .
The solstices are determined by the distance the Earth is from the sun in its orbit. Winter is when the sun is farthest away relative to the Earth's tilt. Summer occurs when the opposite is true.
The gravitational force between the Earth and sun certainly depends on the distance between the Earth and sun. But the gravitational force between, for example, the Earth and me does not.
Several methods are used, depending on the distance. For nearer stars, the parallax method is used: Sine Earth moves around the Sun, the direction of the star, against the background, changes. This method, of course, requires precise measurement of the parallax (of this angular change), as well as knowledge of the distance between the Sun and Earth.
The average distance between Earth and its moon is 238,000 miles, approximately.