In

astronomyAstronomy is a natural science that deals with the study of celestial objects and phenomena that originate outside the atmosphere of Earth...

,

**Kepler's laws** give a description of the

motionIn physics, motion is a change in position of an object with respect to time. Change in action is the result of an unbalanced force. Motion is typically described in terms of velocity, acceleration, displacement and time . An object's velocity cannot change unless it is acted upon by a force, as...

of

planetA planet is a celestial body orbiting a star or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science,...

s around the

SunThe Sun is the star at the center of the Solar System. It is almost perfectly spherical and consists of hot plasma interwoven with magnetic fields...

.

Kepler's laws are:

- The orbit
In physics, an orbit is the gravitationally curved path of an object around a point in space, for example the orbit of a planet around the center of a star system, such as the Solar System...

of every planetA planet is a celestial body orbiting a star or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science,...

is an ellipseIn geometry, an ellipse is a plane curve that results from the intersection of a cone by a plane in a way that produces a closed curve. Circles are special cases of ellipses, obtained when the cutting plane is orthogonal to the cone's axis...

with the Sun at one of the two fociIn geometry, the foci are a pair of special points with reference to which any of a variety of curves is constructed. For example, foci can be used in defining conic sections, the four types of which are the circle, ellipse, parabola, and hyperbola...

.
- A line
The notion of line or straight line was introduced by the ancient mathematicians to represent straight objects with negligible width and depth. Lines are an idealization of such objects...

joining a planet and the Sun sweeps out equal areaArea is a quantity that expresses the extent of a two-dimensional surface or shape in the plane. Area can be understood as the amount of material with a given thickness that would be necessary to fashion a model of the shape, or the amount of paint necessary to cover the surface with a single coat...

s during equal intervals of time.
- The square of the orbital period
The orbital period is the time taken for a given object to make one complete orbit about another object.When mentioned without further qualification in astronomy this refers to the sidereal period of an astronomical object, which is calculated with respect to the stars.There are several kinds of...

of a planet is directly proportionalIn mathematics, two variable quantities are proportional if one of them is always the product of the other and a constant quantity, called the coefficient of proportionality or proportionality constant. In other words, are proportional if the ratio \tfrac yx is constant. We also say that one...

to the cubeIn arithmetic and algebra, the cube of a number n is its third power — the result of the number multiplying by itself three times:...

of the semi-major axisThe major axis of an ellipse is its longest diameter, a line that runs through the centre and both foci, its ends being at the widest points of the shape...

of its orbit.

## History

Johannes KeplerJohannes Kepler was a German mathematician, astronomer and astrologer. A key figure in the 17th century scientific revolution, he is best known for his eponymous laws of planetary motion, codified by later astronomers, based on his works Astronomia nova, Harmonices Mundi, and Epitome of Copernican...

published his first two laws in 1609, having found them by analyzing the astronomical observations of

Tycho BraheTycho Brahe , born Tyge Ottesen Brahe, was a Danish nobleman known for his accurate and comprehensive astronomical and planetary observations...

. Kepler discovered his third law many years later, and it was published in 1619. At the time, Kepler's laws were radical claims; the prevailing belief (particularly in epicycle-based theories) was that orbits should be based on perfect circles. Most of the planetary orbits can be rather closely approximated as circles, so it is not immediately evident that the orbits are ellipses. Detailed calculations for the orbit of the planet Mars first indicated to Kepler its elliptical shape, and he inferred that other heavenly bodies, including those farther away from the

SunThe Sun is the star at the center of the Solar System. It is almost perfectly spherical and consists of hot plasma interwoven with magnetic fields...

, have elliptical orbits too. Kepler's laws and his analysis of the observations on which they were based, the assertion that the Earth orbited the Sun, proof that the planets' speeds varied, and use of elliptical orbits rather than circular orbits with epicycles—challenged the long-accepted

geocentric modelIn astronomy, the geocentric model , is the superseded theory that the Earth is the center of the universe, and that all other objects orbit around it. This geocentric model served as the predominant cosmological system in many ancient civilizations such as ancient Greece...

s of

AristotleAristotle was a Greek philosopher and polymath, a student of Plato and teacher of Alexander the Great. His writings cover many subjects, including physics, metaphysics, poetry, theater, music, logic, rhetoric, linguistics, politics, government, ethics, biology, and zoology...

and

PtolemyClaudius Ptolemy , was a Roman citizen of Egypt who wrote in Greek. He was a mathematician, astronomer, geographer, astrologer, and poet of a single epigram in the Greek Anthology. He lived in Egypt under Roman rule, and is believed to have been born in the town of Ptolemais Hermiou in the...

, and generally supported the

heliocentric theoryCopernican heliocentrism is the name given to the astronomical model developed by Nicolaus Copernicus and published in 1543. It positioned the Sun near the center of the Universe, motionless, with Earth and the other planets rotating around it in circular paths modified by epicycles and at uniform...

of

Nicolaus CopernicusNicolaus Copernicus was a Renaissance astronomer and the first person to formulate a comprehensive heliocentric cosmology which displaced the Earth from the center of the universe....

(although Kepler's ellipses likewise did away with Copernicus's circular orbits and epicycles).

Some eight decades later,

Isaac NewtonSir Isaac Newton PRS was an English physicist, mathematician, astronomer, natural philosopher, alchemist, and theologian, who has been "considered by many to be the greatest and most influential scientist who ever lived."...

proved that relationships like Kepler's would apply exactly under certain ideal conditions that are to a good approximation fulfilled in the solar system, as consequences of Newton's own

laws of motionNewton's laws of motion are three physical laws that form the basis for classical mechanics. They describe the relationship between the forces acting on a body and its motion due to those forces...

and

law of universal gravitationNewton's law of universal gravitation states that every point mass in the universe attracts every other point mass with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them...

. Because of the nonzero planetary masses and resulting

perturbationsPerturbation is a term used in astronomy in connection with descriptions of the complex motion of a massive body which is subject to appreciable gravitational effects from more than one other massive body....

, Kepler's laws apply only approximately and not exactly to the motions in the solar system.

VoltaireFrançois-Marie Arouet , better known by the pen name Voltaire , was a French Enlightenment writer, historian and philosopher famous for his wit and for his advocacy of civil liberties, including freedom of religion, free trade and separation of church and state...

's

*Eléments de la philosophie de Newton* (

*Elements of Newton's Philosophy*) was in 1738 the first publication to call Kepler's Laws "laws". Together with Newton's mathematical theories, they are part of the foundation of modern

astronomyAstronomy is a natural science that deals with the study of celestial objects and phenomena that originate outside the atmosphere of Earth...

and

physicsPhysics is a natural science that involves the study of matter and its motion through spacetime, along with related concepts such as energy and force. More broadly, it is the general analysis of nature, conducted in order to understand how the universe behaves.Physics is one of the oldest academic...

.

## First Law

- "The orbit
In physics, an orbit is the gravitationally curved path of an object around a point in space, for example the orbit of a planet around the center of a star system, such as the Solar System...

of every planetA planet is a celestial body orbiting a star or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science,...

is an ellipseIn geometry, an ellipse is a plane curve that results from the intersection of a cone by a plane in a way that produces a closed curve. Circles are special cases of ellipses, obtained when the cutting plane is orthogonal to the cone's axis...

with the Sun at one of the two fociIn geometry, the foci are a pair of special points with reference to which any of a variety of curves is constructed. For example, foci can be used in defining conic sections, the four types of which are the circle, ellipse, parabola, and hyperbola...

."

An ellipse is a particular class of mathematical shapes that resemble a stretched out circle. (See the figure to the right.) Note as well that the Sun is not at the center of the ellipse but is at one of the focal points. The other focal point is marked with a lighter dot but is a point that has no physical significance for the orbit. Ellipses have two focal points neither of which is in the center of the ellipse (except for the one special case of the ellipse being a circle). Circles are a special case of an ellipse that are not stretched out and in which both focal points coincide at the center.

How stretched out that ellipse is from a perfect circle is known as its

eccentricityThe orbital eccentricity of an astronomical body is the amount by which its orbit deviates from a perfect circle, where 0 is perfectly circular, and 1.0 is a parabola, and no longer a closed orbit...

; a parameter that varies from 0 (a simple circle) to 1 (an ellipse that is so stretched out that it is a straight line back and forth between the two focal points). The eccentricities of the planets known to Kepler varies from 0.007 (

VenusVenus is the second planet from the Sun, orbiting it every 224.7 Earth days. The planet is named after Venus, the Roman goddess of love and beauty. After the Moon, it is the brightest natural object in the night sky, reaching an apparent magnitude of −4.6, bright enough to cast shadows...

) to 0.2 (

MercuryMercury is the innermost and smallest planet in the Solar System, orbiting the Sun once every 87.969 Earth days. The orbit of Mercury has the highest eccentricity of all the Solar System planets, and it has the smallest axial tilt. It completes three rotations about its axis for every two orbits...

). (See List of planetary objects in the Solar System for more detail.)

After Kepler, though, bodies with highly eccentric orbits have been identified, among them many

cometA comet is an icy small Solar System body that, when close enough to the Sun, displays a visible coma and sometimes also a tail. These phenomena are both due to the effects of solar radiation and the solar wind upon the nucleus of the comet...

s and

asteroidAsteroids are a class of small Solar System bodies in orbit around the Sun. They have also been called planetoids, especially the larger ones...

s. The

dwarf planetA dwarf planet, as defined by the International Astronomical Union , is a celestial body orbiting the Sun that is massive enough to be spherical as a result of its own gravity but has not cleared its neighboring region of planetesimals and is not a satellite...

PlutoPluto, formal designation 134340 Pluto, is the second-most-massive known dwarf planet in the Solar System and the tenth-most-massive body observed directly orbiting the Sun...

was discovered as late as 1929, the delay mostly due to its small size, far distance, and optical faintness. Heavenly bodies such as comets with

parabolicIn astrodynamics or celestial mechanics a parabolic trajectory is a Kepler orbit with the eccentricity equal to 1. When moving away from the source it is called an escape orbit, otherwise a capture orbit...

or even

hyperbolicIn astrodynamics or celestial mechanics a hyperbolic trajectory is a Kepler orbit with the eccentricity greater than 1. Under standard assumptions a body traveling along this trajectory will coast to infinity, arriving there with hyperbolic excess velocity relative to the central body. Similarly to...

orbits are possible under the

Newtonian theoryNewton's law of universal gravitation states that every point mass in the universe attracts every other point mass with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them...

and have been observed.

Symbolically an ellipse can be represented in polar coordinates as:

where (

*r*,

*θ*) are the polar coordinates (from the focus) for the ellipse,

*p* is the semi-latus rectum, and

*ε* is the

eccentricityIn mathematics, the eccentricity, denoted e or \varepsilon, is a parameter associated with every conic section. It can be thought of as a measure of how much the conic section deviates from being circular.In particular,...

of the ellipse. For a planet orbiting the Sun then

*r* is the distance from the Sun to the planet and

*θ* is the angle with its vertex at the Sun from the location where the planet is closest to the Sun.

At

*θ* = 0°, perihelion, the distance is minimum

At

*θ* = 90° and at

*θ* = 270°, the distance is

At

*θ* = 180°, aphelion, the distance is maximum

The

semi-major axisThe major axis of an ellipse is its longest diameter, a line that runs through the centre and both foci, its ends being at the widest points of the shape...

*a* is the

arithmetic meanIn mathematics and statistics, the arithmetic mean, often referred to as simply the mean or average when the context is clear, is a method to derive the central tendency of a sample space...

between

*r*_{min} and

*r*_{max}:

so

The

semi-minor axisIn geometry, the semi-minor axis is a line segment associated with most conic sections . One end of the segment is the center of the conic section, and it is at right angles with the semi-major axis...

*b* is the

geometric meanThe geometric mean, in mathematics, is a type of mean or average, which indicates the central tendency or typical value of a set of numbers. It is similar to the arithmetic mean, except that the numbers are multiplied and then the nth root of the resulting product is taken.For instance, the...

between

*r*_{min} and

*r*_{max}:

so

The semi-latus rectum

*p* is the

harmonic meanIn mathematics, the harmonic mean is one of several kinds of average. Typically, it is appropriate for situations when the average of rates is desired....

between

*r*_{min} and

*r*_{max}:

so

The

eccentricityIn mathematics, the eccentricity, denoted e or \varepsilon, is a parameter associated with every conic section. It can be thought of as a measure of how much the conic section deviates from being circular.In particular,...

*ε* is the

coefficient of variationIn probability theory and statistics, the coefficient of variation is a normalized measure of dispersion of a probability distribution. It is also known as unitized risk or the variation coefficient. The absolute value of the CV is sometimes known as relative standard deviation , which is...

between

*r*_{min} and

*r*_{max}:

The

areaArea is a quantity that expresses the extent of a two-dimensional surface or shape in the plane. Area can be understood as the amount of material with a given thickness that would be necessary to fashion a model of the shape, or the amount of paint necessary to cover the surface with a single coat...

of the ellipse is

The special case of a circle is

*ε* = 0, resulting in

*r* =

*p* =

*r*_{min} =

*r*_{max} =

*a* =

*b* and

*A* = π

*r*^{2}.

## Second law

- "A line
The notion of line or straight line was introduced by the ancient mathematicians to represent straight objects with negligible width and depth. Lines are an idealization of such objects...

joining a planet and the Sun sweeps out equal areas during equal intervals of time."

In a small time

the planet sweeps out a small triangle having base line

and height

The area of this triangle is

and so the constant

areal velocityAreal velocity is the rate at which area is swept out by a particle as it moves along a curve. In many applications, the curve lies in a plane, but in others, it is a space curve....

is

Now as the first law states that the planet follows an ellipse, the planet is at different distances from the Sun at different parts in its orbit. So the planet has to move faster when it is closer to the Sun so that it sweeps equal areas in equal times.

The total area enclosed by the elliptical orbit is

.

Therefore the period

satisfies

or

where

is the

angular velocityIn physics, the angular velocity is a vector quantity which specifies the angular speed of an object and the axis about which the object is rotating. The SI unit of angular velocity is radians per second, although it may be measured in other units such as degrees per second, revolutions per...

, (using Newton notation for differentiation), and

is the

mean motionMean motion, n\,\!, is a measure of how fast a satellite progresses around its elliptical orbit. Unless the orbit is circular, the mean motion is only an average value, and does not represent the instantaneous angular rate....

of the planet around the sun.

## Third law

- "The square of the orbital period
The orbital period is the time taken for a given object to make one complete orbit about another object.When mentioned without further qualification in astronomy this refers to the sidereal period of an astronomical object, which is calculated with respect to the stars.There are several kinds of...

of a planet is directly proportionalIn mathematics, two variable quantities are proportional if one of them is always the product of the other and a constant quantity, called the coefficient of proportionality or proportionality constant. In other words, are proportional if the ratio \tfrac yx is constant. We also say that one...

to the cubeIn arithmetic and algebra, the cube of a number n is its third power — the result of the number multiplying by itself three times:...

of the semi-major axisThe major axis of an ellipse is its longest diameter, a line that runs through the centre and both foci, its ends being at the widest points of the shape...

of its orbit."

The third law, published by Kepler in 1619

http://www-istp.gsfc.nasa.gov/stargaze/Skeplaws.htm captures the relationship between the distance of planets from the Sun, and their orbital periods.

For example, suppose planet A is 4 times as far from the Sun as planet B. Then planet A must traverse 4 times the distance of Planet B each orbit, and moreover it turns out that planet A travels at half the speed of planet B, in order to maintain equilibrium with the reduced gravitational

centripetal forceCentripetal force is a force that makes a body follow a curved path: it is always directed orthogonal to the velocity of the body, toward the instantaneous center of curvature of the path. The mathematical description was derived in 1659 by Dutch physicist Christiaan Huygens...

due to being 4 times further from the Sun. In total it takes 4×2=8 times as long for planet A to travel an orbit, in agreement with the law (8

^{2}=4

^{3}).

This third law used to be known as the

*harmonic law*, because Kepler enunciated it in a laborious attempt to determine what he viewed as the "

music of the spheresMusica universalis is an ancient philosophical concept that regards proportions in the movements of celestial bodies—the Sun, Moon, and planets—as a form of musica . This 'music' is not usually thought to be literally audible, but a harmonic and/or mathematical and/or religious concept...

" according to precise laws, and express it in terms of musical notation.

This third law currently receives additional attention as it can be used to estimate the distance from an exoplanet to its central

starA star is a massive, luminous sphere of plasma held together by gravity. At the end of its lifetime, a star can also contain a proportion of degenerate matter. The nearest star to Earth is the Sun, which is the source of most of the energy on Earth...

, and help to decide if this distance is inside the

habitable zoneIn astronomy and astrobiology, a habitable zone is an umbrella term for regions that are considered favourable to life. The concept is inferred from the empirical study of conditions favourable for Life on Earth...

of that star.

Symbolically:

where

is the orbital period of planet and

is the semimajor axis of the orbit.

The proportionality constant is the same for any planet around the Sun.

So the constant is 1 (

sidereal yearA sidereal year is the time taken by the Earth to orbit the Sun once with respect to the fixed stars. Hence it is also the time taken for the Sun to return to the same position with respect to the fixed stars after apparently travelling once around the ecliptic. It was equal to at noon 1 January...

)

^{2}(

astronomical unitAn astronomical unit is a unit of length equal to about or approximately the mean Earth–Sun distance....

)

^{−3} or 2.97472505×10

^{−19} s

^{2}m

^{−3}. See the actual figures: attributes of major planets.

## Generality

These laws approximately describe the motion of any two bodies in orbit around each other. (The statement in the first law about the focus becomes closer to exactitude as one of the masses becomes closer to zero mass. Where there are more than two masses, all of the statements in the laws become closer to exactitude as all except one of the masses become closer to zero mass and as the

perturbationsPerturbation is a term used in astronomy in connection with descriptions of the complex motion of a massive body which is subject to appreciable gravitational effects from more than one other massive body....

then also tend towards zero). The masses of the two bodies can be nearly equal, e.g.

CharonCharon is the largest satellite of the dwarf planet Pluto. It was discovered in 1978 at the United States Naval Observatory Flagstaff Station. Following the 2005 discovery of two other natural satellites of Pluto , Charon may also be referred to as Pluto I...

—

PlutoPluto, formal designation 134340 Pluto, is the second-most-massive known dwarf planet in the Solar System and the tenth-most-massive body observed directly orbiting the Sun...

(~1:10), in a small proportion, e.g.

MoonThe Moon is Earth's only known natural satellite,There are a number of near-Earth asteroids including 3753 Cruithne that are co-orbital with Earth: their orbits bring them close to Earth for periods of time but then alter in the long term . These are quasi-satellites and not true moons. For more...

—

EarthEarth is the third planet from the Sun, and the densest and fifth-largest of the eight planets in the Solar System. It is also the largest of the Solar System's four terrestrial planets...

(~1:100), or in a great proportion, e.g.

MercuryMercury is the innermost and smallest planet in the Solar System, orbiting the Sun once every 87.969 Earth days. The orbit of Mercury has the highest eccentricity of all the Solar System planets, and it has the smallest axial tilt. It completes three rotations about its axis for every two orbits...

—

SunThe Sun is the star at the center of the Solar System. It is almost perfectly spherical and consists of hot plasma interwoven with magnetic fields...

(~1:10,000,000).

In all cases of two-body motion, rotation is about the

barycenterIn astronomy, barycentric coordinates are non-rotating coordinates with origin at the center of mass of two or more bodies.The barycenter is the point between two objects where they balance each other. For example, it is the center of mass where two or more celestial bodies orbit each other...

of the two bodies, with neither one having its center of mass exactly at one focus of an ellipse. However, both orbits are ellipses with one focus at the barycenter. When the ratio of masses is large, the barycenter may be deep within the larger object, close to its center of mass. In such a case it may require sophisticated precision measurements to detect the separation of the barycenter from the center of mass of the larger object. But in the case of the planets orbiting the Sun, the largest of them are in mass as much as 1/1047.3486 (Jupiter) and 1/3497.898 (Saturn) of the solar mass, and so it has long been known that the solar system barycenter can sometimes be outside the body of the Sun, up to about a solar diameter from its center. Thus Kepler's first law, though not far off as an approximation, does not quite accurately describe the orbits of the planets around the Sun under classical physics.

## Zero eccentricity

Kepler's laws refine the model of Copernicus. If the eccentricity of a planetary

orbitIn physics, an orbit is the gravitationally curved path of an object around a point in space, for example the orbit of a planet around the center of a star system, such as the Solar System...

is zero, then Kepler's laws state:

- The planetary orbit is a circle
- The Sun is in the center
- The speed of the planet in the orbit is constant
- The square of the sidereal period
The orbital period is the time taken for a given object to make one complete orbit about another object.When mentioned without further qualification in astronomy this refers to the sidereal period of an astronomical object, which is calculated with respect to the stars.There are several kinds of...

is proportionate to the cubeIn geometry, a cube is a three-dimensional solid object bounded by six square faces, facets or sides, with three meeting at each vertex. The cube can also be called a regular hexahedron and is one of the five Platonic solids. It is a special kind of square prism, of rectangular parallelepiped and...

of the distance from the Sun.

Actually the eccentricities of the orbits of the six planets known to Copernicus and Kepler are quite small, so this gives excellent approximations to the planetary motions, but Kepler's laws give even better fit to the observations.

Kepler's corrections to the Copernican model are not at all obvious:

- The planetary orbit is
*not* a circle, but an *ellipse*
- The Sun is
*not* at the center but at a *focal point*
- Neither the linear speed nor the angular speed of the planet in the orbit is constant, but the
*area speed* is constant.
- The square of the sidereal period
The orbital period is the time taken for a given object to make one complete orbit about another object.When mentioned without further qualification in astronomy this refers to the sidereal period of an astronomical object, which is calculated with respect to the stars.There are several kinds of...

is proportionate to the cube of the *mean between the maximum and minimum* distances from the Sun.

The nonzero eccentricity of the orbit of the earth makes the time from the March

equinoxAn equinox occurs twice a year, when the tilt of the Earth's axis is inclined neither away from nor towards the Sun, the center of the Sun being in the same plane as the Earth's equator...

to the September equinox, around 186 days, unequal to the time from the September equinox to the March equinox, around 179 days. The

equatorAn equator is the intersection of a sphere's surface with the plane perpendicular to the sphere's axis of rotation and containing the sphere's center of mass....

cuts the orbit into two parts having areas in the proportion 186 to 179, while a diameter cuts the orbit into equal parts. So the eccentricity of the orbit of the Earth is approximately

close to the correct value (0.016710219). (See

Earth's orbitIn astronomy, the Earth's orbit is the motion of the Earth around the Sun, at an average distance of about 150 million kilometers, every 365.256363 mean solar days .A solar day is on average 24 hours; it takes 365.256363 of these to orbit the sun once in the sense of returning...

).

The calculation is correct when the perihelion, the date that the Earth is closest to the Sun, is on a

solsticeA solstice is an astronomical event that happens twice each year when the Sun's apparent position in the sky, as viewed from Earth, reaches its northernmost or southernmost extremes...

. The current perihelion, near January 4, is fairly close to the solstice on December 21 or 22.

## Relation to Newton's laws

Isaac NewtonSir Isaac Newton PRS was an English physicist, mathematician, astronomer, natural philosopher, alchemist, and theologian, who has been "considered by many to be the greatest and most influential scientist who ever lived."...

computed in his Philosophiæ Naturalis Principia Mathematica the

accelerationIn physics, acceleration is the rate of change of velocity with time. In one dimension, acceleration is the rate at which something speeds up or slows down. However, since velocity is a vector, acceleration describes the rate of change of both the magnitude and the direction of velocity. ...

of a planet moving according to Kepler's first and second law.

- The
*direction* of the acceleration is towards the Sun.
- The
*magnitude* of the acceleration is in inverse proportion to the square of the distance from the Sun.

This suggests that the Sun may be the physical cause of the acceleration of planets.

Newton defined the

forceIn physics, a force is any influence that causes an object to undergo a change in speed, a change in direction, or a change in shape. In other words, a force is that which can cause an object with mass to change its velocity , i.e., to accelerate, or which can cause a flexible object to deform...

on a planet to be the product of its

massMass can be defined as a quantitive measure of the resistance an object has to change in its velocity.In physics, mass commonly refers to any of the following three properties of matter, which have been shown experimentally to be equivalent:...

and the acceleration. (See

Newton's laws of motionNewton's laws of motion are three physical laws that form the basis for classical mechanics. They describe the relationship between the forces acting on a body and its motion due to those forces...

). So:

- Every planet is attracted towards the Sun.
- The force on a planet is in direct proportion to the mass of the planet and in inverse proportion to the square of the distance from the Sun.

Here the Sun plays an unsymmetrical part which is unjustified. So he assumed

Newton's law of universal gravitationNewton's law of universal gravitation states that every point mass in the universe attracts every other point mass with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them...

:

- All bodies in the solar system attract one another.
- The force between two bodies is in direct proportion to their masses and in inverse proportion to the square of the distance between them.

As the planets have small masses compared to that of the Sun, the orbits conform to Kepler's laws approximately. Newton's model improves Kepler's model and gives better fit to the observations. See

two-body problemIn classical mechanics, the two-body problem is to determine the motion of two point particles that interact only with each other. Common examples include a satellite orbiting a planet, a planet orbiting a star, two stars orbiting each other , and a classical electron orbiting an atomic nucleus In...

.

A deviation of the motion of a planet from Kepler's laws due to attraction from other planets is called a

perturbationPerturbation is a term used in astronomy in connection with descriptions of the complex motion of a massive body which is subject to appreciable gravitational effects from more than one other massive body....

.

## Computing position as a function of time

Kepler used his two first laws for computing the position of a planet as a function of time. His method involves the solution of a

transcendental equationA transcendental function is a function that does not satisfy a polynomial equation whose coefficients are themselves polynomials, in contrast to an algebraic function, which does satisfy such an equation...

called

Kepler's equationKepler's equation is M = E -\epsilon \cdot \sin E ,where M is the mean anomaly, E is the eccentric anomaly, and \displaystyle \epsilon is the eccentricity....

.

The procedure for calculating the heliocentric polar coordinates (

*r*,

*θ*) to a planetary position as a function of the time

*t* since perihelion, and the orbital period

*P*, is the following four steps.

- 1. Compute the
**mean anomaly**In celestial mechanics, the mean anomaly is a parameter relating position and time for a body moving in a Kepler orbit. It is based on the fact that equal areas are swept at the focus in equal intervals of time....

*M* from the formula

- 2. Compute the
**eccentric anomaly**In celestial mechanics, the eccentric anomaly is an angular parameter that defines the position of a body that is moving along an elliptic Kepler orbit.For the point P orbiting around an ellipse, the eccentric anomaly is the angle E in the figure...

*E* by solving Kepler's equation:

- 3. Compute the
**true anomaly**In celestial mechanics, the true anomaly is an angular parameter that defines the position of a body moving along a Keplerian orbit. It is the angle between the direction of periapsis and the current position of the body, as seen from the main focus of the ellipse .The true anomaly is usually...

*θ* by the equation:

- 4. Compute the
**heliocentric distance** *r* from the first law:

The important special case of circular orbit, ε = 0, gives simply

*θ* =

*E* =

*M*. Because the uniform circular motion was considered to be

*normal*, a deviation from this motion was considered an

**anomaly**.

The proof of this procedure is shown below.

### Mean anomaly, *M*

The Keplerian problem assumes an

elliptical orbitIn astrodynamics or celestial mechanics an elliptic orbit is a Kepler orbit with the eccentricity less than 1; this includes the special case of a circular orbit, with eccentricity equal to zero. In a stricter sense, it is a Kepler orbit with the eccentricity greater than 0 and less than 1 . In a...

and the four points:

*s* the Sun (at one focus of ellipse);
*z* the perihelion
*c* the center of the ellipse
*p* the planet

and

distance between center and perihelion, the

**semimajor axis**,

the

**eccentricity**,

the

**semiminor axis**,

the distance between Sun and planet.

the direction to the planet as seen from the Sun, the

**true anomaly**In celestial mechanics, the true anomaly is an angular parameter that defines the position of a body moving along a Keplerian orbit. It is the angle between the direction of periapsis and the current position of the body, as seen from the main focus of the ellipse .The true anomaly is usually...

.

The problem is to compute the polar coordinates (

*r*,

*θ*) of the planet from the

**time since perihelion**,

*t*.

It is solved in steps. Kepler considered the circle with the major axis as a diameter, and

the projection of the planet to the auxiliary circle

the point on the circle such that the sector areas

*|zcy|* and

*|zsx|* are equal,

the

**mean anomaly**In celestial mechanics, the mean anomaly is a parameter relating position and time for a body moving in a Kepler orbit. It is based on the fact that equal areas are swept at the focus in equal intervals of time....

.

The sector areas are related by

The

circular sectorA circular sector or circle sector, is the portion of a disk enclosed by two radii and an arc, where the smaller area is known as the minor sector and the larger being the major sector. In the diagram, θ is the central angle in radians, r the radius of the circle, and L is the arc length of the...

area

The area swept since perihelion,

is by Kepler's second law proportional to time since perihelion. So the mean anomaly,

*M*, is proportional to time since perihelion,

*t*.

where

*P* is the

orbital periodThe orbital period is the time taken for a given object to make one complete orbit about another object.When mentioned without further qualification in astronomy this refers to the sidereal period of an astronomical object, which is calculated with respect to the stars.There are several kinds of...

.

### Eccentric anomaly, *E*

When the mean anomaly

*M* is computed, the goal is to compute the true anomaly

*θ*. The function

*θ*=

*f*(

*M*) is, however, not elementary. Kepler's solution is to use

,

*x* as seen from the centre, the

**eccentric anomaly**In celestial mechanics, the eccentric anomaly is an angular parameter that defines the position of a body that is moving along an elliptic Kepler orbit.For the point P orbiting around an ellipse, the eccentric anomaly is the angle E in the figure...

as an intermediate variable, and first compute

*E* as a function of

*M* by solving Kepler's equation below, and then compute the true anomaly

*θ* from the eccentric anomaly

*E*. Here are the details.

Division by

*a*^{2}/2 gives

**Kepler's equation**Kepler's equation is M = E -\epsilon \cdot \sin E ,where M is the mean anomaly, E is the eccentric anomaly, and \displaystyle \epsilon is the eccentricity....

This equation gives

*M* as a function of

*E*. Determining

*E* for a given

*M* is the inverse problem. Iterative numerical algorithms are commonly used.

Having computed the eccentric anomaly

*E*, the next step is to calculate the true anomaly

*θ*.

### True anomaly, θ

Note from the figure that

so that

Dividing by

and inserting from Kepler's first law

to get

The result is a usable relationship between the eccentric anomaly

*E* and the true anomaly

*θ*.

A computationally more convenient form follows by substituting into the trigonometric identity:

Get

Multiplying by (1+ε)/(1−ε) and taking the square root gives the result

We have now completed the third step in the connection between time and position in the orbit.

One could even develop a series computing

*θ* directly from

*M*.

http://info.ifpan.edu.pl/firststep/aw-works/fsII/mul/mueller.html
### Distance, *r*

The fourth step is to compute the heliocentric distance

*r* from the true anomaly

*θ* by Kepler's first law:

## Computing the planetary acceleration

In his Principia Mathematica Philosophiae Naturalis, Newton showed that Kepler's laws imply that the

accelerationIn physics, acceleration is the rate of change of velocity with time. In one dimension, acceleration is the rate at which something speeds up or slows down. However, since velocity is a vector, acceleration describes the rate of change of both the magnitude and the direction of velocity. ...

of the planets are directed towards the sun and depend on the distance from the sun by the inverse square law. However, The geometrical method used by Newton to prove the result is quite complicated. The demonstration below is based on calculus.

### Acceleration vector

From the heliocentric point of view consider the vector to the planet

where

is the distance to the planet and the direction

is a

unit vector. When the planet moves the direction vector

changes:

where

is the unit vector orthogonal to

and pointing in the direction of rotation, and

is the polar angle, and where a dot on top of the variable signifies differentiation with respect to time.

So differentiating the position vector twice to obtain the velocity and the acceleration vectors:

So

where the

**radial acceleration** is

and the

**tangential acceleration** is

### The inverse square law

Kepler's second law implies that the

areal velocityAreal velocity is the rate at which area is swept out by a particle as it moves along a curve. In many applications, the curve lies in a plane, but in others, it is a space curve....

is a constant of motion.

The tangential acceleration

is zero by Kepler's second law:

So the acceleration of a planet obeying Kepler's second law is directed exactly towards the sun.

Kepler's first law implies that the area enclosed by the orbit is

, where

is the

semi-major axisThe major axis of an ellipse is its longest diameter, a line that runs through the centre and both foci, its ends being at the widest points of the shape...

and

is the

semi-minor axisIn geometry, the semi-minor axis is a line segment associated with most conic sections . One end of the segment is the center of the conic section, and it is at right angles with the semi-major axis...

of the ellipse. Therefore the period

satisfies

or

where

is the

mean motionMean motion, n\,\!, is a measure of how fast a satellite progresses around its elliptical orbit. Unless the orbit is circular, the mean motion is only an average value, and does not represent the instantaneous angular rate....

of the planet around the sun.

The radial acceleration

is

Kepler's first law states that the orbit is described by the equation:

Differentiating with respect to time

or

Differentiating once more

The radial acceleration

satisfies

Substituting the equation of the ellipse gives

The relation

gives the simple final result

This means that the acceleration vector

of any planet obeying Kepler's first and second law satisfies the

**inverse square law**
where

is a constant, and

is the unit vector pointing from the Sun towards the planet, and

is the distance between the planet and the Sun.

According to Kepler's third law,

has the same value for all the planets. So the inverse square law for planetary accelerations applies throughout the entire solar system.

The inverse square law is a

differential equationA differential equation is a mathematical equation for an unknown function of one or several variables that relates the values of the function itself and its derivatives of various orders...

. The solutions to this differential equation includes the Keplerian motions, as shown, but they also include motions where the orbit is a

hyperbolaIn mathematics a hyperbola is a curve, specifically a smooth curve that lies in a plane, which can be defined either by its geometric properties or by the kinds of equations for which it is the solution set. A hyperbola has two pieces, called connected components or branches, which are mirror...

or

parabolaIn mathematics, the parabola is a conic section, the intersection of a right circular conical surface and a plane parallel to a generating straight line of that surface...

or a straight line. See

kepler orbitIn celestial mechanics, a Kepler orbit describes the motion of an orbiting body as an ellipse, parabola, or hyperbola, which forms a two-dimensional orbital plane in three-dimensional space...

.

## Newton's law of gravitation

By Newton's second law, the gravitational force that acts on the planet is:

where

only depends on the property of the Sun. According to Newton's third Law, the Sun is also attracted by the planet with a force of the same magnitude. Now that the force is proportional to the mass of the planet, under the symmetric consideration, it should also be proportional to the mass of the Sun. So the form of the gravitational force should be

where

is a universal constant. This is

Newton's law of universal gravitationNewton's law of universal gravitation states that every point mass in the universe attracts every other point mass with a force that is directly proportional to the product of their masses and inversely proportional to the square of the distance between them...

.

The acceleration of solar system body no

*i* is, according to Newton's laws:

where

is the mass of body no

*j*, and

is the distance between body

*i* and body

*j*, and

is the unit vector from body

*i* pointing towards body

*j*, and the vector summation is over all bodies in the world, besides no

*i* itself. In the special case where there are only two bodies in the world, Planet and Sun, the acceleration becomes

which is the acceleration of the Kepler motion.

## See also

- Kepler orbit
In celestial mechanics, a Kepler orbit describes the motion of an orbiting body as an ellipse, parabola, or hyperbola, which forms a two-dimensional orbital plane in three-dimensional space...

- Kepler problem
In classical mechanics, the Kepler problem is a special case of the two-body problem, in which the two bodies interact by a central force F that varies in strength as the inverse square of the distance r between them. The force may be either attractive or repulsive...

- Kepler's equation
Kepler's equation is M = E -\epsilon \cdot \sin E ,where M is the mean anomaly, E is the eccentric anomaly, and \displaystyle \epsilon is the eccentricity....

- Circular motion
In physics, circular motion is rotation along a circular path or a circular orbit. It can be uniform, that is, with constant angular rate of rotation , or non-uniform, that is, with a changing rate of rotation. The rotation around a fixed axis of a three-dimensional body involves circular motion of...

- Gravity
- Two-body problem
In classical mechanics, the two-body problem is to determine the motion of two point particles that interact only with each other. Common examples include a satellite orbiting a planet, a planet orbiting a star, two stars orbiting each other , and a classical electron orbiting an atomic nucleus In...

- Free-fall time
The free-fall time is the characteristic time that would take a body to collapse under its own gravitational attraction, if no other forces existed to oppose the collapse...

- Laplace–Runge–Lenz vector

## External links

- B.Surendranath Reddy; animation of Kepler's laws: applet
- Crowell, Benjamin,
*Conservation Laws*, http://www.lightandmatter.com/area1book2.html, an online bookAn on-line book is a resource in book-like form that is only available to read online. It differs from the common idea of an ebook, which is usually available to download and read locally or on an ebook reader.Book-like means:...

that gives a proof of the first law without the use of calculus. (see section 5.2, p. 112)
- David McNamara and Gianfranco Vidali,
*Kepler's Second Law - Java Interactive Tutorial*, http://www.phy.syr.edu/courses/java/mc_html/kepler.html, an interactive Java applet that aids in the understanding of Kepler's Second Law.
- Audio - Cain/Gay (2010) Astronomy Cast Johannes Kepler and His Laws of Planetary Motion
- University of Tennessee's Dept. Physics & Astronomy: Astronomy 161 page on Johannes Kepler: The Laws of Planetary Motion http://csep10.phys.utk.edu/astr161/lect/history/kepler.html
- Equant compared to Kepler: interactive model http://people.scs.fsu.edu/~dduke/kepler.html
- Kepler's Third Law:interactive model http://people.scs.fsu.edu/~dduke/kepler3.html
- Solar System Simulator (Interactive Applet)
- Kepler and His Laws, educational web pages by David P. Stern