Нужен перевод текста, не с переводчика)
In ancient times, people believed that the Earth was the centre of the solar system and tried to understand and explain the movement of the Sun, the Moon, the stars and the planets around the Earth. As scientific knowledge and technology improved over time, this idea (called the geocentric theory, from the ancient Greek words meaning Earth-centred) lost favour and new theories about the solar system were put forward.
Tycho Brahe (1546-1601) and Galileo (1564¬1642) made accurate measurements of the heavens, which were the basis for later theories. Nicolas Copernicus (1473-1543) believed that the Earth was not the centre of the solar svstem but just another planet revolving around the Sun, which itself never moved. This type of theory was called heliocentric. Johannes Kepler (1571-1630), an assistant to Brahe, used Brahe's measurements to support Copernicus' heliocentric theory. This led to his discovery of three laws relating to planetary movement, including the fact that the planets move in elliptical orbits around the Sun.
It was left to Isaac Newton to expand on these theories by testing and proving Kepler's laws. By observing things around him, Newton realised several things. One was that objects can be in one place, without moving. This is called inertia. Then, if the object moved, it moved toward another object. The phenomenon causing this pull of one object towards another was the force of gravity (or little g). Newton found that the mass of the two objects and the distance between them determined the strength of the force of gravity and developed an equation which expressed this relationship.
Continuing to test and expand his findings, Newton hypothesised that this relationship existed not only between objects on the Earth but also objects in space. This led in 1687 to Newton's Philosophiae Naturalis Principia Mathematica (Mathematical Principles of Natural Philosophy, usually called Principia) in which he wrote about his historic discovery of the Law of Universal Gravitation (or big G). By calling his discovery a lazv, it meant that the relationships he had discovered were true everywhere and in all cases.
Newton's discovery had a huge impact on scientific thinking for centuries afterwards. In fact, his findings were not improved upon until 1905, when Albert Einstein introduced his Special Theory of Relativity.
Нужен перевод текста, не с переводчика)
In ancient times, people believed that the Earth was the centre of the solar system and tried to understand and explain the movement of the Sun, the Moon, the stars and the planets around the Earth. As scientific knowledge and technology improved over time, this idea (called the geocentric theory, from the ancient Greek words meaning Earth-centred) lost favour and new theories about the solar system were put forward.
Tycho Brahe (1546-1601) and Galileo (1564¬1642) made accurate measurements of the heavens, which were the basis for later theories. Nicolas Copernicus (1473-1543) believed that the Earth was not the centre of the solar svstem but just another planet revolving around the Sun, which itself never moved. This type of theory was called heliocentric. Johannes Kepler (1571-1630), an assistant to Brahe, used Brahe's measurements to support Copernicus' heliocentric theory. This led to his discovery of three laws relating to planetary movement, including the fact that the planets move in elliptical orbits around the Sun.
It was left to Isaac Newton to expand on these theories by testing and proving Kepler's laws. By observing things around him, Newton realised several things. One was that objects can be in one place, without moving. This is called inertia. Then, if the object moved, it moved toward another object. The phenomenon causing this pull of one object towards another was the force of gravity (or little g). Newton found that the mass of the two objects and the distance between them determined the strength of the force of gravity and developed an equation which expressed this relationship.
Continuing to test and expand his findings, Newton hypothesised that this relationship existed not only between objects on the Earth but also objects in space. This led in 1687 to Newton's Philosophiae Naturalis Principia Mathematica (Mathematical Principles of Natural Philosophy, usually called Principia) in which he wrote about his historic discovery of the Law of Universal Gravitation (or big G). By calling his discovery a lazv, it meant that the relationships he had discovered were true everywhere and in all cases.
Newton's discovery had a huge impact on scientific thinking for centuries afterwards. In fact, his findings were not improved upon until 1905, when Albert Einstein introduced his Special Theory of Relativity.
In ancient times, people believed that the Earth was the centre of the solar system and tried to understand and explain the movement of the Sun, the Moon, the stars and the planets around the Earth. As scientific knowledge and technology improved over time, this idea (called the geocentric theory, from the ancient Greek words meaning Earth-centred) lost favour and new theories about the solar system were put forward.
Tycho Brahe (1546-1601) and Galileo (1564¬1642) made accurate measurements of the heavens, which were the basis for later theories. Nicolas Copernicus (1473-1543) believed that the Earth was not the centre of the solar svstem but just another planet revolving around the Sun, which itself never moved. This type of theory was called heliocentric. Johannes Kepler (1571-1630), an assistant to Brahe, used Brahe's measurements to support Copernicus' heliocentric theory. This led to his discovery of three laws relating to planetary movement, including the fact that the planets move in elliptical orbits around the Sun.
It was left to Isaac Newton to expand on these theories by testing and proving Kepler's laws. By observing things around him, Newton realised several things. One was that objects can be in one place, without moving. This is called inertia. Then, if the object moved, it moved toward another object. The phenomenon causing this pull of one object towards another was the force of gravity (or little g). Newton found that the mass of the two objects and the distance between them determined the strength of the force of gravity and developed an equation which expressed this relationship.
Continuing to test and expand his findings, Newton hypothesised that this relationship existed not only between objects on the Earth but also objects in space. This led in 1687 to Newton's Philosophiae Naturalis Principia Mathematica (Mathematical Principles of Natural Philosophy, usually called Principia) in which he wrote about his historic discovery of the Law of Universal Gravitation (or big G). By calling his discovery a lazv, it meant that the relationships he had discovered were true everywhere and in all cases.
Newton's discovery had a huge impact on scientific thinking for centuries afterwards. In fact, his findings were not improved upon until 1905, when Albert Einstein introduced his Special Theory of Relativity.
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В древние времена люди верили, что Земля является центром солнечной системы и пытались понять и объяснить движение Солнца, Луны, звезд и планет вокруг Земли. По мере улучшения научных знаний и технологий, эта идея (называемая геоцентрической теорией, от древнегреческих слов, означающих "центр Земли") утратила свою популярность, и были выдвинуты новые теории о солнечной системе.
Тихо Браге (1546-1601) и Галилео Галилей (1564-1642) сделали точные измерения небес, которые послужили основой для последующих теорий. Николай Коперник (1473-1543) верил, что Земля не является центром солнечной системы, а всего лишь еще одной планетой, вращающейся вокруг Солнца, которое само по себе не двигалось. Такой тип теории назывался гелиоцентрическим. Иоанн Кеплер (1571-1630), ассистент Браге, использовал измерения Браге для поддержки гелиоцентрической теории Коперника. Это привело к его открытию трех законов относительно движения планет, включая то, что планеты движутся по эллиптическим орбитам вокруг Солнца.
Исааку Ньютону пришлось расширить эти теории, проверив и доказав законы Кеплера. Наблюдая вещи вокруг себя, Ньютон понял несколько вещей. Одна из них была то, что объекты могут находиться в одном месте, не двигаясь. Это называется инерцией. Затем, если объект двигался, он двигался к другому объекту. Явление, вызывающее это притяжение одного объекта к другому, была сила тяжести (или маленькая g). Ньютон обнаружил, что масса двух объектов и расстояние между ними определяют силу гравитационного взаимодействия и разработал уравнение, выражающее эту связь.
Продолжая тестировать и расширять свои открытия, Ньютон предположил, что эта связь существует не только между объектами на Земле, но и между объектами в космосе. Это привело в 1687 году к "Математическим принципам естественной философии" Ньютона, где он писал о своем историческом открытии закона всемирного притяжения (или большой G). Называя свое открытие законом, это означало, что законы, которые он открыл, справедливы везде и во всех случаях.
Открытие Ньютона оказало огромное влияние на научное мышление на протяжении веков. Фактически его открытия не были улучшены до 1905 года, когда Альберт Эйнштейн представил свою Специальную теорию относительности.