Link to here: walter.bislins.ch/Helio
The model is a scaled down numerical simulation of 3 bodies (sun, earth, moon), obeying only Newton's law of universal gravitation and Newton's laws of motion. The simulation shows, that stable orbits can exist in the Heliocentric Model. You can change parameters of the simulated solar system and disable some forces to study the consequences.
The big gray circle around the earth is the Hill Sphere. It defines the range where stable orbits around the earth are possible. As long as the moon orbits within the light gray circle with the thick border, the orbit is stable. Outside this circle the orbit is instable and the moon may be lost in space or captured by the sun.
The other cicles show the initial orbits of earth and moon. You can disable all circles by disabling Show Orbits Checkbox.
The App on this page is a Simulation, not an Animation. An animation is a predetermined programmed sequence of movements, following explicit steps or certain formulas that describe the motions.
A simulation is not predetermined. It follows physical laws. The motions are generally not predictable in detail and depend on start conditions and interactions with the user.
This simulation uses Newton's laws of universal gravitation and the laws of motion. The shown trajectories and orbits are the result of this natural laws, implemented in a computer program. The simulations shows what would happen in reality given the same parameters.
So if this simulation can produce stable orbits obeying Newton's laws, then such orbits are possible in reality too.
From an observer stationary with respect to the sun we can see that the moon traces a weird epicyclic path: Sometimes he is taking over the earth on the far side of the sun, gets nearer to the sun, seems to come to a halt and the suddenly gets accelerated to catch up with the earth again:
Even weirder is the corkscrew path of earth and moon as seen from an observer stationary with respect to the galaxy:
How is it possible that the apparent path of the bodies depend on the observer? How is it possible, that the orbits are stable despite the observation that they trace weird paths depending on the observer?
To answer this question, ask yourself the following: How does an observer influence the motion (positions and velocities) of objects which he does not affect by exerting a force on them, only by looking at them?
The answer is: The motions of observed objects are not affected by a pure observer at all. The traces of moving objects are illusions caused by the relative motion of the observer with respect to the observed objects. The traces are only pictures emerging from plotting past relative positions of objects in the coordinate system of the observer. So each observer sees their own traces, but no observer has any influence on positions, velocities or any other physical properties of the objects, as described in Relativity of Positions and Velocities.
To get a deeper inside into orbital mechanics, we need to understand some basic properties of the universe and their implications on motion in general and on orbits in particular. Here I start with a rough description of how orbits work. Read Basic Properties of the Universe to get a deeper understanding.
The attractive force between two bodies creates an acceleration that is directed from one body to the other. If both bodies were initially at rest with respect to each other, this would result in the bodies getting closer until they collide. But if the bodies have relative velocities that are not in the direction of the acceleration, they constantly miss each other. Because there is no friction in space slowing things down the bodies keep orbiting each other around a common center of mass, called the Barycenter.
If one body is much more massive than the other, the barycenter lies near the center of the heavier body, so the less massive body practically orbits the heavier body, while the heavy body seams to stay rather stationary, only wiggles slowly around the barycenter.
Orbits are generally not perfect circles but ellipses. Only if the velocitiy is always exactly at 90° to the acceleration vector and the magnitude has exactly a certain value then the orbit is a perfect circle. Although the orbits of the planets and moons in the solar system are all slightly elliptical, the deviation from a perfect circle is barely noticable.
On elliptical orbits the distance between two bodies and the speed of the orbiting body constantly changes, which means that the forces/accelerations between the bodies are constantly changing too. How can such orbits be stable?
In orbits (circular and elliptic), the total energy = sum of potential and kinetic energy at each point of the orbit is constant = conserved. It is not dependent on the excentricity of the orbit. This is also a consequence of the inverse square law of Gravity. The inverse square law on the other hand is a consequence of the universe being 3-dimensional. All this enables stable elliptical orbits.
In the simulation the darker gray circle around the earth shows the range of the so called Hill Sphere. Orbits inside 1/2 (lighter gray circle) to 1/3 of this sphere are stable. Greater orbits are instable due to the influence of the sun or other big planets. Bodies outside of the Hill sphere can not orbit the earth.
If the Hill sphere lies inside a body, then there are no orbits possible around the body. For example the Hill sphere of the ISS lies inside the hull of the ISS, so an astronaut outside can not orbit the station although he gets attracted to it.
One consequence of the fact, that all masses in the solar system attract each other, is, that the earth and the other planets do not orbit around the center of the sun, but all planets and the sun orbit around the common center of mass, called the Barycenter.
The barycenter of two bodies lies on the line connecting the center of the two bodies and is nearer the body with the greater mass. In our solar system the barycenter of the sun and all planets makes complicated figures and lies sometimes inside the sun, sometimes outside.
So with respect to the common center of mass of the solar system the sun makes very slow complicated movements.
In the simulation it can be observed, that the sun revolves around a center that is not the center of the sun. Select the option Show CM to show the center of masses. The barycenter of the whole system is indicated by the red crosshair.
The barycenter of earth and moon lies also not at the center of the earth (black cross). The Earth-Moon systems barycenter revolves around the sun on the orange orbit. Earth and moon revolve around this barycenter on their orbit. This feature of the simulation can be observed in reality.
Now that we understand how the paths of objects are an illusion created by the observer and the observer has no effect on the motion of the objects, we can analyze the paths without having an observer to take into account.
To determine the trajectory of the moon we have to determine all forces acting on the moon all the times.
In the solar system all bodies exert a force on each other due to Gravity. Because the force gets much weaker as further away a body is (proportional to one over distance squared), only the force of the earth and the sun are relevant to the motion of the moon. Although the sun is very far away from the moon compared to the earth, its influence can not be neglegted, because the sun has an enormous mass.
More than 99.8% of the mass of the whole solar system is concentrated in the sun. In fact the attracting force on the moon is more than twice as strong as the attracting force of the earth on the moon. See Hill Sphere for an explanation why the moon orbits the earth anyway.
Lets explore the forces between sun, earth and moon. Because the earth has a bigger mass than the moon, the attraction force between sun and earth is greater than the attraction force between the sun and moon. The attraction force between earth and moon is the same for both, according to Newton's third law of motion.
This may be surprising. It implies that you are attracting the earth with the same force as the earth is attracting you. But because acceleration is also dependent on the mass of the attracted object, the movement of the earth caused by you attracting it is not perceivable, but not zero!
To be specific: The earth has roughly 1023 times more mass than a human, so the earth's displacement caused by you attracting it is 1023 times smaller than the displacement of you caused by earth's attraction. Nowadays we can measure the change in earths rotation rate due to the displacement of large masses, like when we empty a big artificial lake.
But back to the forces between sun, earth and moon. You can visualize the forces in the simulation:
Note that the forces between earth and moon are equal but opposite. The moon is attracting the earth with the same force as the earth is attracting the moon (Newton's third law).
Note that the acceleration of the moon and earth caused by the sun are almost the same. So they both orbit the sun at about the same path, because their mean speed around the sun is the same too.
In the left image above you see the individual force components. The total force on a body is the vector sum of the force components acting on the body. By showing the individual force components, it is easier to see what's going on.
Notice, that the attraction force sun/earth is greater than the attraction force sun/moon. You may ask, how can the moon follow a nearly circular orbit around the earth, if earth and moon are not attracted with the same force to the sun? Sould not the earth get caught by the sun or the moon get lost into space?
This is not the case. It has to do with the fact that not the force is responsible for the motion of objects, but the resulting acceleration. The acceleration is not only dependent on the force, but depends on the mass of the object too: a = F / m. So if we look at the components of the acceleration in the right image above, we notice that the acceleration in direction to the sun is the same for earth and moon! So the sun accelerates earth and moon with the same amount towards it.
This may be surprising. But on the earth we can observer the same phenomenon: each mass is accelerated exactly the same amount to the center of the earth, no matter how much mass an object has. This also applies to space. If two objects are the same distance to the sun, they get attracted to the sun with the same acceleration. So the whole earth/moon system orbits the sun on the same track.
Strictly speaking, this is not quite right. The orbit of the moon is not always exactly at the same distance to the sun. So the attraction between sun and moon changes constantly. But as long as the attraction between sun and moon does not vary a lot with respect to the mean attraction, the orbit of the moon around the earth is not disturbed much by the sun. This is the case if the distance between the earth/moon system and sun is much greater than the distance between earth and moon, so that the moon lies well inside the Hill Sphere, which is the case in reality.
Lets calculate the accelerations in the real solar system:
|Sun accelerating Earth||0.00593 m/s2|
|Sun accelerating Moon||(0.00593 ± 0.00003) m/s2|
|Earth accelerating Moon||0.00270 m/s2|
|Moon accelerating Earth||0.0000332 m/s2|
We can see that the sun is accelerating earth and moon the same amount, so earth and moon orbit the sun together. But surprisingly the sun is accelerating the moon about twice as much as the earth is accelerating the moon. Why does the moon not get accelerated away from the earth?
To answer this we have to calculate the range around the earth in which the influence of the earth on any satellite like the moon is greater than the sun. This range is a sphere around the earh which radius is the distance from the center of the earth to the Lagrangian Points L1 and L2. This sphere is called Hill sphere. As long as a satellite stays within this sphere it keeps orbiting the earth.
The radius of the Hill sphere for the earth is:
Detailed numerical calculations show that orbits at or just within the Hill sphere are not stable in the long term; it appears that stable satellite orbits exist only inside 1/2 to 1/3 of the Hill radius (Source Wikipedia: Hill sphere). The distance between earth and moon is with 384,000 km smaller than 1/3 of the Hill sphere radius, so it's orbit is stable.
In the simulation the Hill sphere around the earth is displayed in light grey. You can simulate a solar system where the acceleration of the moon from the sun is bigger than the acceleration of the moon from the earth maintaining a stable orbit by clicking the following button:
In the simulation, using the blue buttons, you can deactivate the attraction between sun, earth and moon to simulate what happens. Try to disable one force only for a very short time to disturb the orbits. There are three possibles outcomes of such disturbances:
This has 3 reasons:
Because of the Relativity of Positions and Velocities, which states that there is no such thing as absolute position and velocity, it follows, that in all systems that are not accelerated, the physical laws are not dependent on the motion of the system with respect to anything. Therefore there is no way to measure or feel any motion in a non-accelerated system. There is no physical effect that is caused by uniform motion.
Because the impression of motion is caused by forces acting on a person and there are no forces caused by uniform motion, you can not feel uniform motion. The impression of motion can be caused by vibrations or accelerations of the vehicle. The impression of motion can also be caused by looking at objects which are moving relative to the observer. Without such a reference this impression vanishes.
Is a rotating planet orbiting a sun a non-accelerated system?
No, orbits are accelerated motions and an object on the surface of a rotating body is in an accelerated state too. Acceleration can be measured with accelerometers. Rotations can be measured eg. with ring LASER Gyros.
So why can't we feel the accelerations due to rotation of the earth and the moon orbiting the earth and the orbit of the earth around the sun?
The tidal acceleration from the moon, the tidal part from the sun and the centrifugal acceleration due to earths rotation are too small to be noticed by the human body. But they can be measured.
The acceleration from the sun's gravity can not be measured on earth (except the tidal part), because everything on earth is accelerated the same amount by the sun. We call this free fall around the sun.
If you don't have any difference in acceleration between objects, you can't measure or feel an acceleration.
So in a rocket orbiting the earth, you are in free fall on a curved = accelerated path around the earth. Although there is still gravitational acceleration acting on you, it is also acting on everything around you the same amount. So all objects are orbiting exactly on the same track together. There is no relative acceleration between you, the rocket and anything else in the rocket. All is freely floating inside the rocket and you feel weightless.
But there are still the very small attractions between all objects and very small tidal effects from earth, moon and sun. That's the reason why we speak of micro gravity environment instead of zero gravity. Gravity acts berween all objects, not only between earth and other objects.
Tidal forces arise because no gravitational field is homogeneous, but they are radial symmetric and point to a center of mass and the magnitude decreases with the square of the distance from the center of mass. This results in very slightly different gravitational accelerations in different directions. A sphere of small objects starts to be elongated in the direction of the center of mass and to be squashed perpendicular to that direction. Two tidal bulges appear like the tides on earth.
To be specific, the accelerations are:
So a 100 kg weight measured at the poles would weigh 340 g less at the equator.
To understand orbital mechanics, we need to understand some basic properties of the universe and their implications on motion in general and on orbits specifically. All motions of gravitationally bound objects obey the following basic observable properties of the universe:
Note: it is not nessesary that you understand what Noether's theorem is, only the physical consequences due to observable properties of the universe are important here.
Noether's theorem states that every differentiable symmetry of the action of a physical system has a corresponding conservation law. The theorem was proven by mathematician Emmy Noether in 1915 and published in 1918.
The action of a physical system is the integral over time of a Lagrangian function, from which the system's behavior can be determined by the principle of least action. The principle of least action can be used to obtain the equations of motion for a system.
Loosely speaking, symmetries in nature account for conservations laws like:
Source: Wikipedia Noether's theorem
This symmetries of the universe are one reason why stable orbits can exist.
Position and velocity are not properties that can be assigned to a single object or system of objects. Position and velocity are relations between different objects or systems. There is no absolute reference point or center of the universe that would allow to assign an absolute position and velocity to an object or system.
You always have to measure position and velocity with respect to a certain observer or reference frame. An observer, moving relativ to another observer measures different positions and velocities of the same observed object or system.
The physical laws are the same at any point in the universe. Therefore there is no special point in the universe that is distinct from any other point, that we could call origin and use as an universal reference point. All positions and velocities are relative to a certain observer and the corresponding values are unique for this observer but different for any other observer.
Because we cannot assign any position or velocity to an object or system itself, no matter what position and velocity that system has with respect to any observer, it has no effect on the system itself whatsoever. You cannot measure a position or velocity or feel a velocity of a system itself, because it has no position and velocity assigned to itself. Position and velocity only exist in the context of relations between objects and observers and do not change the physics in the observed object or system.
This implies that we can choose an arbitrary non-accelerated point, observer or frame as our reference to describe the motion of an object or system of objects, but for all computations we have to use the same choosen observer or reference frame.
This is reflected in the simulation as you can choose between four observer coordinate systems CoordSys and it does not change the orbits of the bodies. It only changes the apparent paths of the bodies, as apparent paths are distinct for each observer.
The simulation uses for all calculations the galaxy as the non-accelerated reference frame, no matter which observer coordinate system is choosen. But any non-accelerated reference frame will do the same.
Contrary to position and velocity, accelerations and forces are absolute and not relative to an observer. Each object can have an acceleration of its own due to forces acting on it independent of any observer. This means each observer measures the same acceleration of a certain object (the same change in velocity) and the same forces acting on that object. This includes an observer that is on the observed object itself at any moment in time.
So accelerations and forces that change the trajectory are local properties of an object or system that can be measured within the system itself without reference to something external. This is taken advantige of in Inertial Reference Units. It's the reason why we can feel accelerations respectively the corresponding forces, if they are greater than a certain threshold.
Accelerations and forces are related to each other according to Newton's second law of motion:
Why are accelerations and forces absolute local properties of an object while position and velocity are relative to an observer?
Acceleration is the rate of change of velocity with respect to time:
This is spelled: vector a is the limit, as delta t goes to zero, of vector delta v over delta t.
Acceleration and velocity are vector quantities. At time t the velocity of an object relative to an observer is
We can see that the relative velocities
This means every observer sees the same acceleration of an object, no matter what the relative velocity is between observer and object. This includes an observer at the object itself. Therefore it follows, that the acceleration is observable from within the object itself. Acceleration is a property that can be assigned to an object itself and is independent of an observer.
Because forces and accelerations are proportional to each other, forces, like accelerations, are not dependent on any non-accelerated observer or Inertial frame of reference.
Note that even if the speed remains constant, the direction of the velocity vector can change as the results of an applied force. So you can have accelerations or forces that do not change the speed, but the direction of motion. This is the case if the acceleration or force always acts perpendicular to the direction of motion like in circular orbits, where the acceleration/force is due to the gravitational attraction towards the central object.
According to Newton's third law body 1 attracts body 2 with the same force F as body 2 attracts body 1. The force vectors are pointing from one body to the other. For the vector form of this equation see Computing all Forces.
Now that we know how to compute all forces acting on an object due to gravity we can compute its acceleration, velocity and path.
Newton's laws of motion describe the connection between forces, accelerations, velocities and positions:
The second law is also called Equation of motion. If we know all forces acting on an object, we can calculate the acceleration of the object which determines the change in velocity and position in time. The connection between acceleration, velocity and position is described by the following differential equations (bare with me, I explain it below):
This equations simply mean, that current velocity at any time t is nothing more than an infinitesimal small path
The same applies to accelerations:
But we don't know the path of an object and it's velocity. That is what we want to calculate from the known acceleration. This can be achieved by integrating the differential equations above, so we get:
These are the foundations of classical mechanics and can be applied to any system of objects, as long as the speeds involved are much smaller than the speed of light and gravity is weak (eg. far from a neutron star or black hole).
The simulation uses Numerical Integration to compute velocity and position from acceleration.
The App divides the simulation in many tiny time steps of length Δt = 50 μs. For each time step the following algorithm is executed:
This algorithm is repeatet over and over again and produces the shown orbits. The essential parts of the simulation code is explained in Simulation Code of Solar System Animation explained. The whole source code can be inspected in Source Code: Solar System Animation.
First the simulation computes the forces between all bodies according to Newton's law of universal gravitation. Given the positions
Note that the attraction force is a vector pointing from one mass to the other. According to Newton's fist law of motion the force pointing from object i to object j is the same in magnitude but in opposite direction as the force pointing from object j to object i:
For each of the 3 bodies we get 2 forces respectively. One force to each other body. Now we have to combine all forces acting on one body by vectorial addition to get the vector sum:
To add vectors, you simply add the corresponding components of the vectors to get a new vector. Note, the new vector
Now each object has one single combined force acting on it. From Newton's second law of motion F = m·a we can compute the acceleration of each object due to the combined forces acting on it:
Note that the acceleration vector
Now we have the acceleration of each body and the direction in which the acceleration acts. How do we get from this the individual velocities and poisitions while the time is passing?
To get the velocity for each object, we have to integrate the acceleration. This is mathematically expressed as follows:
Or we can get the change in velocity
Similar we can calculate the position for each object at each time by integrating the velocity:
Or the change
We can not integrate
This steps are continuously repeatet for each time step
Note: the simulation uses a more sophisticated rule for the integration, that halves the error compared to the above method.
Numeric simulations like this one have one big problem: small rounding errors accumulate by the integration process. In the case of this simulation it results in slowly decaying orbits, especially if the angular speed around an object gets big. To minimize the errors the simulation computes 20,000 steps for each frame, ie 20,000 steps each 16.7 ms!
If you encounter decaying orbits, it's due to accumulating numerical errors. In reality such decays do not happen, except a body is slowed down by friction.
We have to compute start conditions, the values for positions and velocities of the bodys, so that they initially produce stable orbits. We can use Kepler's laws to compute the start positions and velocities given distances between the bodies and their orbital period.
The App also computes the masses and their corresponding sizes of the objects from the distances and periods, assuming some density of the objects, so that their pixel size is appropriate.
Note: in reality the masses, their distances and their velocities and start positions are given and the orbital periods and center of masses depend on that. For the simulation it was a priority, that the graphics fits onto the sceen. Therefor the data is computed the other way around as follows:
Given the orbital period T and the distance between two bodies D we can compute the central mass needed to hold the body in orbit using Kepler's law:
The mass of the moon is computed from the relative position of the common center of mass (CMEarthMoon) between earth and moon:
The sun and earth-moon system orbits around a common center of mass. The distance between sun and earth-moon system as given by the parameter DSunEarth has to be corrected by incorporating the calculated mass of the sun and mass of the earth-moon system from above:
The distance of the common center of mass sun-earth from the earth is:
The distance of the common center of mass sun-earth from the sun is:
The tangential velocity of the sun around the CM is:
And the tangential velocity of the earth-moon CM around the CM of the sun is:
Now we can setup an initial state for the sun. To simulate movement of the whole solar system through the galaxy in the left direction we add a negative velocity component
The earth and moon orbit around a common center of mass between them. The distance between earth and moon as given by the parameter DEarthMoon has to be corrected by incorporating the calculated masses of the earth and moon:
The distance of the common center of mass earth-moon from the moon is:
The distance of the common center of mass earth-moon from the earth is:
The tangential velocity of the Earth around the CM is:
And the tangential velocity of the moon around the CM is:
Now we can setup an initial states for earth and moon:
The presented formulas work for a real solar system. The model however uses distances in pixels and periods in seconds. To account for that, the gravitational constant was scaled to G = 1 px3/(kg·s2) and all masses are scaled accordingly. The size of the bodies are computed from the scaled masses by incorporating a scaled density, so that the radius of the bodies gets in a range of 8 to 80 pixels.
The radius of a sphere with mass M and density ρ is:
So the radius is proportional the the cube root of the mass. I can define a density factor ρ', that converts a scaled simulator mass to a decent radius:
The following density factors turned out to be usefull to get decent pixel sizes depending on the masses:
ρ' for sun :
ρ' for earth: ρ' for moon :