# Line 17q Heliocentric Universe Celestial Mechanics Principia Hipparchus Ptolemaic WOW SETI

Line 17q Heliocentric Universe Celestial Mechanics Principia Hipparchus Ptolemaic WOW SETI

part 95 of 100 videos

Math Equation: 14 1 113 2 1

6EQUJ5

1420.40575177 MHz. hydrogen line

Jan 24 2012 940 pm est

My Thoughts

I learned something new from all this. I always assumed that the earth was the middle of the universe. I didn’t know it was the sun. Interesting theories on both parts and I don’t know if they have made up their mind yet because it seems they are using BOTH types of charts to figure star charts out.

I could be wrong, let me know if I’m wrong about this and give us a reference of where to find the proof as to where it says differently.

Here’s a thought. The James Webb Telescope finds out that were part of an even BIGGER Universe and that our solar system is one of the “little” systems in it.

Now wouldn’t that be something! That would definitely mean there is alien life forms out there living on other “habitable” planets.

They must be trying to communicate with us. We just have to figure out how to answer back in “their” languages, so that they can understand what we are saying…

**Heliocentric Universe Celestial Mechanics Newton Principia Hipparchus Ptolemaic system **

Heliocentric Universe

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Heliocentrism (lower panel) in comparison to the geocentric model (upper panel)

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Modern analytic celestial mechanics started over 300 years ago with Isaac Newton’s Principia of 1687. The name “celestial mechanics” is more recent than that. Newton wrote that the field should be called “rational mechanics.” The term “dynamics” came in a little later with Gottfried Leibniz, and over a century after Newton, Pierre-Simon Laplace introduced the term “celestial mechanics.” Nevertheless, prior studies addressing the problem of planetary positions are known going back perhaps 3,000 or more years, as early as the Babylonian astronomers.

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quotesHeliocentrism, or heliocentricism,[1] is the astronomical model in which the Earth and planets revolve around a stationary Sun at the center of the universe.

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geocentrism, which placed the Earth at the center.

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The Sun makes a slower circle eastward over the course of a year; the planets have similar motions, but they sometimes move in the reverse direction for a while (retrograde motion).

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The basic elements of Ptolemaic astronomy, showing a planet on an epicycle with an eccentric deferent and an equant point.

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Pages from 1550 SACROBOSCO “Tractatus de Sphaera” with the Ptolemaic system.

In the Ptolemaic system, each planet is moved by a system of two or more spheres: one called its deferent, the others, its epicycles. The deferent is a circle whose center point exists halfway between the equant and the earth, marked by the X in the picture to the right where the equant is the solid point opposite the earth. Another sphere, the epicycle, is embedded inside of the deferent and is represented by the smaller dotted line to the right. A given planet then moves along the epicycle at the same time the epicycle moves along the path marked by the deferent. These combined movements cause the given planet to move closer to and further away from the Earth at different points in its orbit, and caused observers to believe that the planet even slowed down, stopped, and moved backward (in retrograde motion).

The Ptolemaic order of spheres from Earth outward is:

1. Moon

2. Mercury

3. Venus

4. Sun

5. Mars

6. Jupiter

7. Saturn

8. Fixed Stars

9. Sphere of Prime Mover

The deferent-and-epicycle model had been used by Greek astronomers for centuries, as had the idea of the eccentric (a deferent which is slightly off-center from the Earth). In the illustration, the center of the deferent is not the Earth but X, making it eccentric (from the Greek ἐκ ec- meaning “from,” and κέντρονcentrum meaning “center”).

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Gravitation

Johannes Kepler, after analysing Tycho Brahe’s famously accurate observations, constructed his three laws in 1609 and 1619, based on a heliocentric view where the planets move in elliptical paths. Using these laws, he was the first astronomer to successfully predict a transit of Venus (for the year 1631). The transition from circular orbits to elliptical planetary paths dramatically changed the accuracy of celestial observations and predictions. Because the heliocentric model by Copernicus was no more accurate than Ptolemy’s system, new mathematical observations were needed to persuade those who still held on to the geocentric model. However, the observations made by Kepler, using Brahe’s data, became a problem not easily overturned for geocentrists.

In 1687, Isaac Newton devised his law of universal gravitation, which introduced gravitation as the force that both kept the Earth and planets moving through the heavens and also kept the air from flying away, allowing scientists to quickly construct a plausible heliocentric model for the solar system. In his Principia, Newton explained his system of how gravity, previously considered to be an occult force, conducted the movements of celestial bodies, and kept our solar system in its working order.

His descriptions of centripetal force[26] were a breakthrough in scientific thought, and finally replaced the previous schools of scientific thought, i.e. those of Aristotle and Ptolemy. However, the process was gradual.

quoteA geocentric frame is useful for many everyday activities and most laboratory experiments, but is a less appropriate choice for solar-system mechanics and space travel.

While a heliocentric frame is most useful in those cases, galactic and extra-galactic astronomy is easier if the sun is treated as neither stationary nor the center of the universe, but rotating around the center of our galaxy, and in turn our galaxy is also not at rest in the cosmic background.

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Jan 20, 2012 702 pmest

My thoughts

(Maya comes to mind) when I see 3000 or more years for modern analytic celestial mechanics – Isaac Newton’s Principia of 1687.

Geometric construction used by Hipparchus in his determination of the distances to the sun and moon.

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Geometric definition

When a circle’s diameter is 1unit, its circumference is π units.

In Euclidean plane geometry, π is defined as the ratio of a circle’s circumference C to its diameter d:[1]

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The Ptolemaic order of spheres from earth

Celestial mechanics is the branch of astronomy that deals with the motions of celestial objects. The field applies principles of physics, historicallyclassical mechanics, to astronomical objects such as stars and planets to produce ephemeris data. Orbital mechanics (astrodynamics) is a subfield which focuses on the orbits of artificial satellites. Lunar theory is another subfield focusing on the orbit of the Moon.

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Sir Isaac Newton published 5 July 1687

Philosophiæ Naturalis Principia Mathematica, Latin for “Mathematical Principles of Natural Philosophy”, often referred to as simply the Principia, is a work in three books by Sir Isaac Newton, first published 5 July 1687.[1][2] After annotating and correcting his personal copy of the first edition[3], Newton also published two further editions, in 1713 and 1726.[4] The Principia states Newton’s laws of motion, forming the foundation of classical mechanics, also Newton’s law of universal gravitation, and a derivation of Kepler’s laws of planetary motion (which Kepler first obtained empirically). The Principia is “justly regarded as one of the most important works in the history of science”.[5]

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in the heliocentric model (Venus Orbit)

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Geometric definition

When a circle’s diameter is 1unit, its circumference is π units.

In Euclidean plane geometry, π is defined as the ratio of a circle’s circumference C to its diameter d:[1]

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in the heliocentric model (Venus Orbit)

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Venus is huge when it’s a crescent because it’s closer to Earth, and small when it’s fullbecause it’s on the other side of the Sun!

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