heliocentric model
Image 1: Heliocentric Model

Copernicus was not the first who claimed that the Earth rotates around the Sun. Before Copernicus, many ancient astronomers claimed the same, and some also gave mathematical and theoretical explanations. Indian scholars, astronomers, and mathematicians Aryabhatta, Brahmagupta, and Yajnavalkya had discovered that the earth is round and rotates on its axis much before Copernicus. Then, Aristarchus proposed a Sun-centered astrological hypothesis of the universe in modern civilization.

Aristarchus’ hypothesis was less recognized at the time, but after 18 centuries astronomer, Galileo constructed a completely predictable simulation of a planet’s orbit. Learn how great astronomers and mathematicians through centuries predicted and explained, how Earth Moves Around The Sun.

In The Ancient Times

Aryabhatta and Brahmagupta

Thousand years before Galileo the Indian scholar aryabhatta had mentioned clearly in the audAyaka system that the days were counted from uday.” Some of his later astronomical papers, which appear to propose a second model (or Ardha-ratrika, midnight), are lost, but the discussion in Brahmagupta’s Khandakhadyaka can be somewhat reconstructed. He appeared to attribute the apparent motions of the heavens to the Earth’s rotation in several works. He might have thought the planet’s orbits were elliptical instead than circular.

In contrast to the then-prevailing belief that the sky rotated, Aryabhata correctly asserted that the earth rotates about its axis daily and that the apparent movement of the stars is a relative motion caused by the rotation of the Earth. In the first chapter of the Aryabhatiya, where he gives the number of yuga rotations and more explicit in the gola chapter as:

४.९.१ अनुलोमगतिर्नौस्थ: पश्यत्यचलं विलोमगं यद्वत्।
४.९.१ अचलानि भानि तद्वत्समपश्चिमगानि लङ्कायाम्॥

४.१०.१ उदयास्तमयनिमित्तं नित्यं प्रवहेण वायुना क्षिप्त:।
४.१०.२ लङ्कासमपश्चिमगो भपञ्जर: सग्रहो भ्रमति॥

“Someone on the equator sees the unmoving stars going uniformly westward, just as someone in a boat moving forward sees an unmoving object moving backward. The rising and setting of the sun are caused by the fact that the sphere of the stars, along with the planets, appears to turn due west at the equator, pushed by the cosmic wind.”

३.१५.१ भानामध: शनैश्चरसुरगुरुभौमार्कशुक्रबुधचन्द्राः ।
३.१५.२ एषामधश्च भूमिर्मेधीभूता खमध्यस्था॥

४.६.१ वृत्तभपञ्जरमध्ये कक्षापरिवेष्टित: खमध्यगत:।
४.६.२ मृज्जलशिखिवायुमयो भूगोल: सर्वतो वृत्त:॥

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“According to Aryabhata’s geocentric model of the solar system the Sun and Moon are each carried by epicycles, they, in turn, revolve around the Earth. In this concept, the planets’ motions are governed by two epicycles, a smaller manda(slow) and a larger śīghra(rapid), which is also found in the Paitmahasiddhnta. The order of the planets in terms of distance from earth is taken as the Moon, Mercury, Venus, the Sun, Mars, Jupiter, Saturn, and the asterisms. The sphere of the Earth, made of earth, water, fire, space, and wind, sits amid space, within the cage formed by stars and encircled by orbits.”

The planets’ locations and periods were computed about uniformly moving points. Mercury and Venus, for example, orbit the Earth at the same mean speed as the Sun. Mars, Jupiter, and Saturn orbit the Earth at different speeds, representing the motion of each planet through the zodiac. Most astronomy historians believe that this two-epicycle model reflects pre-Ptolemaic Greek astronomy. Some historians believe the ghrocca, or basic planetary time about the Sun, is a hint of an underlying heliocentric concept in Aryabhata’s model.

Aryabhata scientifically explained solar and lunar eclipses. According to him, the Moon and planets are illuminated by reflected sunlight. He explains eclipses in terms of shadows thrown by and falling on Earth, rather than the prevalent cosmogony in which eclipses are caused by Rahu and Ketu (designated as the pseudo-planetary lunar nodes). As a result, a lunar eclipse occurs when the Moon passes through the shadow of the Earth (verse gola.37). He goes into great detail about the magnitude and extent of the Earth’s shadow (verses gola.38–48) and then explains how to calculate the size of the obscured portion during an eclipse.

Later Indian astronomers improved on Aryabhata’s calculations, but they were the foundation. During a visit to Pondicherry, India in the 18th century, 18th-century scientist Guillaume Le Gentil discovered that Indian computations of the duration of the lunar eclipse of August 30, 1765, were short by 41 seconds, whilst his charts were long by 68 seconds.

Aryabhata calculated the sidereal rotation (the earth’s rotation based on fixed stars) to be 23 hours, 56 minutes, and 4.1 seconds in contemporary English units of time; the modern figure is 23:56:4.091. Similarly, his value of 365 days, 6 hours, 12 minutes, and 30 seconds (365.25858 days) for the length of the sidereal year is an inaccuracy of 3 minutes and 20 seconds over a year (365.25636 days).

Aryabhata advocated an astronomical concept in which the Earth rotated on its axis, as previously described. In terms of the mean speed of the Sun, his model also provided corrections (the gra anomaly) for the speeds of the planets in the sky. As a result, it has been proposed that Aryabhata’s calculations were based on an underlying heliocentric paradigm, in which the planets orbit the Sun, although this has been refuted and been suggested that some features of Aryabhata’s theory were borrowed from an earlier, presumably pre-Ptolemaic Greek, the heliocentric model that Indian astronomers were unaware of, however evidence for this is limited.

If we look thoroughly at Aryabhata’s writings we can conclude that at a time when the majority of people believed in the Ptolemaic view solar system, He was the first to propose that the stars were immobile and that the movement of the sky was driven by the Earth’s daily motion. However, he did not elaborate on how he came to this decision. He had begun the process of rejecting the prevailing Ptolemaic viewpoint, but his successors did not carry it out, therefore nothing came out of it.

Many individuals claim that Aryabhata held the heliocentric view in mind, according to which the Sun is fixed and the planets, including the Earth, revolve around it in orbits. However, we have not found any convincing evidence to support this claim. We ask any member who is aware of it to email us in response and let us know. Therefore we concluded that Aryabhata’s system was not explicitly heliocentric, according to the consensus.

Aristarchus of Samos (3rd century BCE) is credited with holding a heliocentric theory but the version of Greek astronomy known in ancient India as the Paulisa Siddhanta does not refer to such a theory. A synodic anomaly (depending on the position of the Sun) does not imply a physically heliocentric orbit (such corrections are also present in late Babylonian astronomical texts).

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Rishi Yajnavalkya

The idea that the Sun, rather than the Earth, is at “the center of the spheres” can be traced back to the Indian philosopher Yajnavalkya (9th Century BCE), He was a follower of the Vedic Tradition, which included the use of mathematics and geometry in religious rites and was a key character in early Indian astronomy. In the Satapatha Brahmana(Shatapatha Brahmana:, he discusses a 95-year intercalary cycle to balance the lunar and solar years and the Sun’s non-uniform motion. Yajnavalkya mentions as:

द्वादिं सतं वै देवरथहन्याम लोकस्तं सामंतम पृथ्वी द्विस्तवतपर्यति तमसमंतम पृथ्वी द्विस्तवत्समुद्रा पर्यति।

“Thirty-two times the place covered by the chariot of the Sun in a day makes this vimana (Loka); around it, covers twice the area of the world (Prithivi); Around the world, covering twice the area, is the ocean”.

“The sun strings these worlds – the earth, the planets, the atmosphere – to himself on a thread.”

This is one of the first recorded references to heliocentrism, but supporters of the idea were in the minority and India continued to believe in a geocentric model until the telescope was invented in the 17th century.


During 310BC–230 BCE, our solar system was formerly thought to represent the whole known universe by most of the people around the world, with the Earth at its center and the rest of the planets and fixed stars circling it every day. The Sun, not the Earth, inhabited the center of the universe, but Aristarchus believed the stars to be other very far-off suns and thought there was no discernible parallax—a movement of the stars relative to one another as the Earth revolves around the Sun—as a result.

His accurate speculation was at the time unprovable since stellar parallax is only measurable with telescopes. His groundbreaking new idea, while the Earth and the other planets orbited the Sun in a circular motion and the fixed stars and the Sun does not move and that the Earth rotates around the Sun in a circle, with the Sun in the center.

Despite this, Aristarchus’s heliocentric thesis seemed counter-intuitive to the senses, so some philosophers, mathematicians, and scientists agreed with him. Seleucus of Seleucia (190–150 BC), who was born nearly four decades after the death of Aristarchus, is the only astronomer by the name known to do so.

Plato and Aristotle

The geocentric theory of the solar system—proposed by Greek philosophers like Plato (428–348 BCE) and Aristotle (384–322 BCE)—with the Earth at its center emerged as the most widely accepted explanation for celestial occurrences. Ptolemy (90-168 AD) cataloged the geocentric model in his masterpiece, “Almagest,” which was published in 140 AD. For the following 14 centuries, this theory was accepted in the western world until Nicolaus Copernicus came out with a new theory.

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In The Modern Times


Before 1514, Copernicus made his “Commentariolus” (“Little Commentary”), a manuscript outlining his thoughts on the heliocentric theory, available to acquaintances. It has seven fundamental presumptions. He then kept compiling information for more in-depth work.

Although his closest friends urged him to do so, Copernicus resisted, saying that he did not want to risk the ridicule “to which he would expose himself on account of the novelty and incomprehensibility of his theses.” Copernicus had essentially finished writing the manuscript of D’ revolutionibus orbium coelestium by around 1532 and proposed a completely predictable model of the cosmos in which the Earth is merely another planet orbiting the Sun in his major work, but he waited until his deathbed in 1543 to publish it for fear of being labeled a heretic by the Christian Church.

Although the Catholic church halted Copernicus’ book, pending revisions, and violently fought to suppress all arguments connected to his heliocentric theory at the time, the Copernican Revolution is now regarded as the starting point for modern astronomy. De revolutionibus was not officially forbidden by the Catholic Church until March 5, 1616, and Galileo used it to reinforce his heliocentric beliefs.

Giordano Bruno’s cosmological claims

After Copernicus, Bruno wrote two major philosophical conversations in 1584 (La Cena de le Ceneri and De infinito universo et Mondi), in which he argued against planetary spheres and affirmed the Copernican principle. In 1586 and 1587, Christoph Rothmann and Tycho Brahe did the same.

In La Cena de le Ceneri, Bruno anticipates some of Galilei’s arguments on the relativity principle, and he also uses the example now known as Galileo’s ship, to support the Copernican view and oppose the objection that the motion of the Earth would be perceived by the motion of winds, clouds, and so on.

Christoph Rothmann and Tycho Brahe

An oft-quoted correspondence between Christoph Rothmann and Tycho Brahe encapsulated the physicists’ quandary at the moment. Brahe was skeptical of Nikolaus Copernicus’ heliocentric view of the world, in a letter to Rothmann, he raised the following objection to the Earth’s movement: “if the Earth turns from west to east, then a cannonball fired toward the turning of the Earth must continue to fly as fast as a projectile fired in the opposite direction.” Rothmann responded that both projectiles and cannons would participate in the Earth’s movement, rendering his objection moot. This, however, was counter to the Aristotelian view of motion that was prevalent in Europe at the time.

tychonian solar system
Tychonian Solar System | In this depiction of the Tychonic system, the objects in blue orbits (the Moon and the Sun) revolve around the Earth. The objects in orange orbits (Mercury, Venus, Mars, Jupiter, and Saturn) revolve around the Sun. Around all is a sphere of fixed stars.

Galileo Galilei

After discovering Jupiter’s four main moons in 1610, the first satellites ever discovered orbiting another planet, Galileo Galilei (1564-1642) used the newly invented refracting telescope to further expand on Copernicus’ theory, and after observing the phases of Venus, he proved that the planets that orbit the Sun are, in fact, the planets. By 1615, Galileo’s writings on heliocentrism had been submitted to the Roman Inquisition by Father Niccolò Lorini, who claimed that Galileo and his followers were attempting to reinterpret the Bible. Galileo then wrote ‘The Dialogue Concerning the Two Chief World Systems’ in 1632, in which he contrasted the Copernican and Ptolemaic world systems, but was later condemned on “grave suspicion of heresy,” compelled to renounce his ideas, and spent the rest of his life under house arrest.

Sir Isaac Newton

As soon as Sir Isaac Newton built the reflecting telescope in 1688, the Earth was not the center of our solar system. Newton’s Principia Mathematica, in which he fully demonstrated the heliocentric model initially introduced by Copernicus, was the last theory to falsify geocentrism. And thus to support the heliocentric hypothesis, Edmund Halley (1656–1742) used Newton’s calculations to predict the comet’s return in 1758.


Aryabhatta’s writings show that he believed that the stars were fixed in their positions and that the earth moves. Most experts believe that this motion is the daily motion of the Earth, in which it rotates around its north-south axis. It is also possible that this motion is the annual rotation of the Earth around the Sun, although no solid reasoning is available for this.

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The Hellenistic astronomer Seleucus of Seleucia, who lived a century after Aristarchus, is said to have maintained and demonstrated heliocentrism as a definite opinion, although no complete record of the performance has been found. Aristarchus proposed heliocentrism only as a hypothesis. Pliny the Elder later questioned whether the displacement of the Earth from its central position could be the reason for the inaccuracy in his predictions of the heavens in his Naturalis Historia. It is implied by heliocentrism rather than geocentrism that Pliny and Seneca describe the apparent (and untrue) phenomenon of retrograde motion of some planets. The geocentric model, which was accepted as accurate in the Middle Ages, was supported by Plato, Aristotle, and Ptolemy, even though no stellar parallax was ever observed. Aristarchus also concluded after realizing that the planets revolve around the Sun i.e. how big the Sun would be from Earth and other planets. However, it turned out that this profound revelation was “too much for the philosophers of the time to digest, and astronomy had to wait another 2000 years to find the right path.”

After Copernicus reintroduced the heliocentric idea, Johannes Kepler developed his three laws to more precisely characterize planetary motions. Later, Isaac Newton provided a theoretical justification based on the dynamics and gravitational attraction laws and then the new age of astronomy started.


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