# hamilton

Physics on generalized coordinate systems using Hamiltonian Mechanics and AD https://github.com/mstksg/hamilton

Version on this page: | 0.1.0.0 |

LTS Haskell 8.1: | 0.1.0.0 |

Stackage Nightly 2017-02-19: | 0.1.0.0 |

Latest on Hackage: | 0.1.0.0 |

**Justin Le**

**justin@jle.im**

#### Module documentation for 0.1.0.0

- Numeric

# Hamilton

Simulate physics on arbitrary coordinate systems using automatic differentiation and Hamiltonian mechanics.

For example, a simulating a double pendulum system by simulating the progression of the angles of each bob:

You only need:

Your generalized coordinates (in this case,

`θ1`

and`θ2`

), and equations to convert them to cartesian coordinates of your objects:`x1 = sin θ1 y1 = -cos θ1 x2 = sin θ1 + sin θ2 / 2 -- second pendulum is half-length y2 = -cos θ1 - cos θ2 / 2`

The masses/inertias of each of those cartesian coordinates (

`m1`

for`x1`

and`y1`

,`m2`

for`x2`

and`y2`

)A potential energy function for your objects:

`U = (m1 y1 + m2 y2) * g`

And that's it! Hamiltonian mechanics steps your generalized coordinates (`θ1`

and `θ2`

) through time, without needing to do any simulation involving
`x1`

/`y1`

/`x2`

/`y2`

! And you don't need to worry about tension or any other
stuff like that. All you need is a description of your coordinate system
itself, and the potential energy!

```
doublePendulum :: System 4 2
doublePendulum =
mkSystem' (vec4 m1 m1 m2 m2) -- masses
(\(V2 θ1 θ2) -> V4 (sin θ1) (-cos θ1)
(sin θ1 + sin θ2/2) (-cos θ1 - cos θ2/2)
) -- coordinates
(\(V4 _ y1 _ y2) -> (m1 * y1 + m2 * y2) * g)
-- potential
```

Thanks to ~~Alexander~~ William Rowan Hamilton, we can express our system parameterized by arbitrary coordinates and get back equations of motions as first-order differential equations. This library solves those first-order differential equations for you using automatic differentiation and some matrix manipulation.

See documentation and example runner.

### Full Exmaple

Let's turn our double pendulum (with the second pendulum half as long) into an
actual running program. Let's say that `g = 5`

, `m1 = 1`

, and `m2 = 2`

.

First, the system:

```
import Numeric.LinearAlgebra.Static
import qualified Data.Vector.Sized as V
doublePendulum :: System 4 2
doublePendulum = mkSystem' masses coordinates potential
where
masses :: R 4
masses = vec4 1 1 2 2
coordinates
:: Floating a
=> V.Vector 2 a
-> V.Vector 4 a
coordinates (V2 θ1 θ2) = V4 (sin θ1) (-cos θ1)
(sin θ1 + sin θ2/2) (-cos θ1 - cos θ2/2)
potential
:: Num a
=> V.Vector 4 a
-> a
potential (V4 _ y1 _ y2) = (y1 + 2 * y2) * 5
```

Neat! Easy, right?

Okay, now let's run it. Let's pick a starting configuration (state of the
system) of `θ1`

and `θ2`

:

```
config0 :: Config 2
config0 = Cfg (vec2 1 0 ) -- initial positions
(vec2 0 0.5) -- initial velocities
```

Configurations are nice, but Hamiltonian dynamics is all about motion through phase space, so let's convert this configuration-space representation of the state into a phase-space representation of the state:

```
phase0 :: Phase 2
phase0 = toPhase doublePendulum config0
```

And now we can ask for the state of our system at any amount of points in time!

```
ghci> evolveHam doublePendulum phase0 [0,0.1 .. 1]
-- result: state of the system at times 0, 0.1, 0.2, 0.3 ... etc.
```

Or, if you want to run the system step-by-step:

```
evolution :: [Phase 2]
evolution = iterate (stepHam 0.1 doublePendulum) phase0
```

And you can get the position of the coordinates as:

```
positions :: [R 2]
positions = phsPos <$> evolution
```

And the position in the underlying cartesian space as:

```
positions' :: [R 4]
positions' = underlyingPos doublePendulum <$> positions
```

## Example App runner

Installation:

```
$ git clone https://github.com/mstksg/hamilton
$ cd hamilton
$ stack install
```

Usage:

```
$ hamilton-examples [EXAMPLE] (options)
$ hamilton-examples --help
$ hamilton-examples [EXAMPLE] --help
```

The example runner is a command line application that plots the progression of several example system through time.

| Example | Description | Coordinates | Options |
|--------------|------------------------------------------------------------|---------------------------------------------------------------------|---------------------------------------------------------------|
| `doublepend`

| Double pendulum, described above | `θ1`

, `θ2`

(angles of bobs) | Masses of each bob |
| `pend`

| Single pendulum | `θ`

(angle of bob) | Initial angle and velocity of bob |
| `room`

| Object bounding around walled room | `x`

, `y`

| Initial launch angle of object |
| `twobody`

| Two gravitationally attracted bodies, described below | `r`

, `θ`

(distance between bodies, angle of rotation) | Masses of bodies and initial angular veocity |
| `spring`

| Spring hanging from a block on a rail, holding up a weight | `r`

, `x`

, `θ`

(position of block, spring compression, spring angle) | Masses of block, weight, spring constant, initial compression |
| `bezier`

| Bead sliding at constant velocity along bezier curve | `t`

(Bezier time parameter) | Control points for arbitrary bezier curve |

Call with `--help`

(or `[EXAMPLE] --help`

) for more information.

## More examples

### Two-body system under gravity

The generalized coordinates are just:

`r`

, the distance between the two bodies`θ`

, the current angle of rotation

`x1 = m2/(m1+m2) * r * sin θ -- assuming (0,0) is the center of mass y1 = m2/(m1+m2) * r * cos θ x2 = -m1/(m1+m2) * r * sin θ y2 = -m1/(m1+m2) * r * cos θ`

The masses/inertias are again

`m1`

for`x1`

and`y1`

, and`m2`

for`x2`

and`y2`

The potential energy function is the classic gravitational potential:

`U = - m1 * m2 / r`

And...that's all you need!

Here is the actual code for the two-body system:

```
twoBody :: System 4 2
twoBody =
mkSystem (vec4 m1 m1 m2 m2) -- masses
(\(V2 r θ) -> let r1 = r * m2 / (m1 + m2)
r2 = - r * m1 / (m1 + m2)
in V4 (r1 * cos θ) (r1 * sin θ)
(r2 * cos θ) (r2 * sin θ)
) -- coordinates
(\(V2 r _) -> - m1 * m2 / r) -- potential
```