This page presents a variety of calculations for latitude/longitude points, with the formulæ and code fragments for implementing them.
All these formulæ are for calculations on the basis of a spherical earth (ignoring ellipsoidal effects) – which is accurate enough^{*} for most purposes… [In fact, the earth is very slightly ellipsoidal; using a spherical model gives errors typically up to 0.3%^{1} – see notes for further details].
Distance
This uses the ‘haversine’ formula to calculate the greatcircle distance between two points – that is, the shortest distance over the earth’s surface – giving an ‘asthecrowflies’ distance between the points (ignoring any hills they fly over, of course!).
Haversine formula: 
a = sin²(Δφ/2) + cos φ_{1} ⋅ cos φ_{2} ⋅ sin²(Δλ/2) 
c = 2 ⋅ atan2( √a, √(1−a) )  
d = R ⋅ c  
where  φ is latitude, λ is longitude, R is earth’s radius (mean radius = 6,371km); note that angles need to be in radians to pass to trig functions! 
JavaScript:  var R = 6371e3; // metres var φ1 = lat1.toRadians(); var φ2 = lat2.toRadians(); var Δφ = (lat2lat1).toRadians(); var Δλ = (lon2lon1).toRadians(); var a = Math.sin(Δφ/2) * Math.sin(Δφ/2) + Math.cos(φ1) * Math.cos(φ2) * Math.sin(Δλ/2) * Math.sin(Δλ/2); var c = 2 * Math.atan2(Math.sqrt(a), Math.sqrt(1a)); var d = R * c; 
Note in these scripts, I generally use lat/lon for latitude/longitude in degrees, and φ/λ for latitude/longitude in radians – having found that mixing degrees & radians is often the easiest route to headscratching bugs...
The haversine formula^{1} ‘remains particularly wellconditioned for numerical computation even at small distances’ – unlike calculations based on the spherical law of cosines. The ‘(re)versed sine’ is 1−cosθ, and the ‘halfversedsine’ is (1−cosθ)/2 or sin²(θ/2) as used above. Once widely used by navigators, it was described by Roger Sinnott in Sky & Telescope magazine in 1984 (“Virtues of the Haversine”): Sinnott explained that the angular separation between Mizar and Alcor in Ursa Major – 0°11′49.69″ – could be accurately calculated on a TRS80 using the haversine.
For the curious, c is the angular distance in radians, and a is the square of half the chord length between the points.
If atan2
is not available, c could be calculated
from 2 ⋅ asin( min(1, √a) )
(including protection against rounding errors).
Using Chrome on a middling Core i5 PC, a distance calculation takes around 2 – 5 microseconds (hence around 200,000 – 500,000 per second). Little to no benefit is obtained by factoring out common terms; probably the JIT compiler optimises them out.
Spherical Law of Cosines
In fact, JavaScript (and most modern computers & languages) use ‘IEEE 754’ 64bit floatingpoint numbers, which provide 15 significant figures of precision. By my estimate, with this precision, the simple spherical law of cosines formula (cos c = cos a cos b + sin a sin b cos C) gives wellconditioned results down to distances as small as a few metres on the earth’s surface. (Note that the geodetic form of the law of cosines is rearranged from the canonical one so that the latitude can be used directly, rather than the colatitude).
This makes the simpler law of cosines a reasonable 1line alternative to the haversine formula for many geodesy purposes (if not for astronomy). The choice may be driven by programming language, processor, coding context, available trig functions (in different languages), etc – and, for very small distances an equirectangular approximation may be more suitable.
Law of cosines:  d = acos( sin φ_{1} ⋅ sin φ_{2} + cos φ_{1} ⋅ cos φ_{2} ⋅ cos Δλ ) ⋅ R 
JavaScript:  var φ1 = lat1.toRadians(), φ2 = lat2.toRadians(), Δλ = (lon2lon1).toRadians(), R = 6371e3; // gives d in metres var d = Math.acos( Math.sin(φ1)*Math.sin(φ2) + Math.cos(φ1)*Math.cos(φ2) * Math.cos(Δλ) ) * R; 
Excel:  =ACOS( SIN(lat1)*SIN(lat2) + COS(lat1)*COS(lat2)*COS(lon2lon1) ) * 6371000 
(or with lat/lon in degrees):  =ACOS( SIN(lat1*PI()/180)*SIN(lat2*PI()/180) + COS(lat1*PI()/180)*COS(lat2*PI()/180)*COS(lon2*PI()/180lon1*PI()/180) ) * 6371000 
While simpler, the law of cosines is slightly slower than the haversine, in my tests.
Equirectangular approximation
If performance is an issue and accuracy less important, for small distances Pythagoras’ theorem can be used on an equirectangular projection:^{*}
Formula  x = Δλ ⋅ cos φ_{m} 
y = Δφ  
d = R ⋅ √x² + y²  
JavaScript:  var x = (λ2λ1) * Math.cos((φ1+φ2)/2); var y = (φ2φ1); var d = Math.sqrt(x*x + y*y) * R; 
This uses just one trig and one sqrt function – as against halfadozen trig functions for cos law, and 7 trigs + 2 sqrts for haversine. Accuracy is somewhat complex: along meridians there are no errors, otherwise they depend on distance, bearing, and latitude, but are small enough for many purposes^{*} (and often trivial compared with the spherical approximation itself).
Alternatively, the polar coordinate flatearth formula can be used: using the colatitudes θ_{1} = π/2−φ_{1} and θ_{2} = π/2−φ_{2}, then d = R ⋅ √θ_{1}² + θ_{2}² − 2 ⋅ θ_{1} ⋅ θ_{2} ⋅ cos Δλ. I’ve not compared accuracy.
Bearing
In general, your current heading will vary as you follow a great circle path (orthodrome); the final heading will differ from the initial heading by varying degrees according to distance and latitude (if you were to go from say 35°N,45°E (≈ Baghdad) to 35°N,135°E (≈ Osaka), you would start on a heading of 60° and end up on a heading of 120°!).
This formula is for the initial bearing (sometimes referred to as forward azimuth) which if followed in a straight line along a greatcircle arc will take you from the start point to the end point:^{1}
Formula:  θ = atan2( sin Δλ ⋅ cos φ_{2} , cos φ_{1} ⋅ sin φ_{2} − sin φ_{1} ⋅ cos φ_{2} ⋅ cos Δλ ) 
where  φ_{1},λ_{1} is the start point, φ_{2},λ_{2} the end point (Δλ is the difference in longitude) 
JavaScript: (all angles in radians) 
var y = Math.sin(λ2λ1) * Math.cos(φ2); var x = Math.cos(φ1)*Math.sin(φ2)  Math.sin(φ1)*Math.cos(φ2)*Math.cos(λ2λ1); var brng = Math.atan2(y, x).toDegrees(); 
Excel: (all angles in radians) 
=ATAN2(COS(lat1)*SIN(lat2)SIN(lat1)*COS(lat2)*COS(lon2lon1), SIN(lon2lon1)*COS(lat2)) *note that Excel reverses the arguments to ATAN2 – see notes below 
Since atan2 returns values in the range π ... +π (that is, 180° ... +180°), to normalise the result to a compass bearing (in the range 0° ... 360°, with −ve values transformed into the range 180° ... 360°), convert to degrees and then use (θ+360) % 360, where % is (floating point) modulo.
For final bearing, simply take the initial bearing from the end point to the start point and reverse it (using θ = (θ+180) % 360).
Midpoint
This is the halfway point along a great circle path between the two points.^{1}
Formula:  B_{x} = cos φ_{2} ⋅ cos Δλ 
B_{y} = cos φ_{2} ⋅ sin Δλ  
φ_{m} = atan2( sin φ_{1} + sin φ_{2}, √(cos φ_{1} + B_{x})² + B_{y}² )  
λ_{m} = λ_{1} + atan2(B_{y}, cos(φ_{1})+B_{x})  
JavaScript: (all angles in radians) 
var Bx = Math.cos(φ2) * Math.cos(λ2λ1); var By = Math.cos(φ2) * Math.sin(λ2λ1); var φ3 = Math.atan2(Math.sin(φ1) + Math.sin(φ2), Math.sqrt( (Math.cos(φ1)+Bx)*(Math.cos(φ1)+Bx) + By*By ) ); var λ3 = λ1 + Math.atan2(By, Math.cos(φ1) + Bx); 
The longitude can be normalised to −180…+180 using (lon+540)%360180 
Just as the initial bearing may vary from the final bearing, the midpoint may not be located halfway between latitudes/longitudes; the midpoint between 35°N,45°E and 35°N,135°E is around 45°N,90°E.
Intermediate point
An intermediate point at any fraction along the great circle path between two points can also be calculated.^{1}
Formula:  a = sin((1−f)⋅δ) / sin δ 
b = sin(f⋅δ) / sin δ  
x = a ⋅ cos φ_{1} ⋅ cos λ_{1} + b ⋅ cos φ_{2} ⋅ cos λ_{2}  
y = a ⋅ cos φ_{1} ⋅ sin λ_{1} + b ⋅ cos φ_{2} ⋅ sin λ_{2}  
z = a ⋅ sin φ_{1} + b ⋅ sin φ_{2}  
φ_{i} = atan2(z, √x² + y²)  
λ_{i} = atan2(y, x)  
where  f is fraction along great circle route (f=0 is point 1, f=1 is point 2), δ is the angular distance d/R between the two points. 
Destination point given distance and bearing from start point
Given a start point, initial bearing, and distance, this will calculate the destination point and final bearing travelling along a (shortest distance) great circle arc.
Formula:  φ_{2} = asin( sin φ_{1} ⋅ cos δ + cos φ_{1} ⋅ sin δ ⋅ cos θ ) 
λ_{2} = λ_{1} + atan2( sin θ ⋅ sin δ ⋅ cos φ_{1}, cos δ − sin φ_{1} ⋅ sin φ_{2} )  
where  φ is latitude, λ is longitude, θ is the bearing (clockwise from north), δ is the angular distance d/R; d being the distance travelled, R the earth’s radius 
JavaScript: (all angles in radians) 
var φ2 = Math.asin( Math.sin(φ1)*Math.cos(d/R) + Math.cos(φ1)*Math.sin(d/R)*Math.cos(brng) ); var λ2 = λ1 + Math.atan2(Math.sin(brng)*Math.sin(d/R)*Math.cos(φ1), Math.cos(d/R)Math.sin(φ1)*Math.sin(φ2)); 
The longitude can be normalised to −180…+180 using (lon+540)%360180 

Excel: (all angles in radians) 
lat2: =ASIN(SIN(lat1)*COS(d/R) + COS(lat1)*SIN(d/R)*COS(brng)) lon2: =lon1 + ATAN2(COS(d/R)SIN(lat1)*SIN(lat2), SIN(brng)*SIN(d/R)*COS(lat1)) * Remember that Excel reverses the arguments to ATAN2 – see notes below 
For final bearing, simply take the initial bearing from the end point to the start
point and reverse it with (brng+180)%360
.
Intersection of two paths given start points and bearings
This is a rather more complex calculation than most others on this page, but I've been asked for it a number of times. This comes from Ed William’s aviation formulary. See below for the JavaScript.
Formula:  δ_{12} = 2⋅asin( √(sin²(Δφ/2) + cos φ_{1} ⋅ cos φ_{2} ⋅ sin²(Δλ/2)) )  angular dist. p1–p2 
θ_{a} = acos( ( sin φ_{2} − sin φ_{1} ⋅ cos δ_{12} ) / ( sin δ_{12} ⋅ cos φ_{1} ) ) θ_{b} = acos( ( sin φ_{1} − sin φ_{2} ⋅ cos δ_{12} ) / ( sin δ_{12} ⋅ cos φ_{2} ) ) 
initial / final bearings between points 1 & 2 

if sin(λ_{2}−λ_{1}) > 0 θ_{12} = θ_{a} θ_{21} = 2π − θ_{b} else θ_{12} = 2π − θ_{a} θ_{21} = θ_{b} 

α_{1} = θ_{13} − θ_{12} α_{2} = θ_{21} − θ_{23} 
angle p2–p1–p3 angle p1–p2–p3 

α_{3} = acos( −cos α_{1} ⋅ cos α_{2} + sin α_{1} ⋅ sin α_{2} ⋅ cos δ_{12} )  angle p1–p2–p3  
δ_{13} = atan2( sin δ_{12} ⋅ sin α_{1} ⋅ sin α_{2} , cos α_{2} + cos α_{1} ⋅ cos α_{3} )  angular dist. p1–p3  
φ_{3} = asin( sin φ_{1} ⋅ cos δ_{13} + cos φ_{1} ⋅ sin δ_{13} ⋅ cos θ_{13} )  p3 lat  
Δλ_{13} = atan2( sin θ_{13} ⋅ sin δ_{13} ⋅ cos φ_{1} , cos δ_{13} − sin φ_{1} ⋅ sin φ_{3} )  long p1–p3  
λ_{3} = λ_{1} + Δλ_{13}  p3 long  
where  φ_{1}, λ_{1}, θ_{13} : 1st start point & (initial) bearing from 1st point towards intersection point % = (floating point) modulo 

note –  if sin α_{1} = 0 and sin α_{2} = 0: infinite solutions if sin α_{1} ⋅ sin α_{2} < 0: ambiguous solution this formulation is not always wellconditioned for meridional or equatorial lines 
This is a lot simpler using vectors rather than spherical trigonometry: see latlongvectors.html.
Crosstrack distance
Here’s a new one: I’ve sometimes been asked about distance of a point from a greatcircle path (sometimes called cross track error).
Formula:  d_{xt} = asin( sin(δ_{13}) ⋅ sin(θ_{13}−θ_{12}) ) ⋅ R 
where 
δ_{13} is (angular) distance from start point to third point θ_{13} is (initial) bearing from start point to third point θ_{12} is (initial) bearing from start point to end point R is the earth’s radius 
JavaScript:  var dXt = Math.asin(Math.sin(d13/R)*Math.sin(θ13θ12)) * R; 
Here, the greatcircle path is identified by a start point and an end point – depending on what initial data you’re working from, you can use the formulæ above to obtain the relevant distance and bearings. The sign of d_{xt} tells you which side of the path the third point is on.
The alongtrack distance, from the start point to the closest point on the path to the third point, is
Formula:  d_{at} = acos( cos(δ_{13}) / cos(δ_{xt}) ) ⋅ R 
where 
δ_{13} is (angular) distance from start point to third point δ_{xt} is (angular) crosstrack distance R is the earth’s radius 
JavaScript:  var dAt = Math.acos(Math.cos(d13/R)/Math.cos(dXt/R)) * R; 
Closest point to the poles
And: ‘Clairaut’s formula’ will give you the maximum latitude of a great circle path, given a bearing θ and latitude φ on the great circle:
Formula:  φ_{max} = acos(  sin θ ⋅ cos φ  ) 
JavaScript:  var φMax = Math.acos(Math.abs(Math.sin(θ)*Math.cos(φ))); 
Rhumb lines
A ‘rhumb line’ (or loxodrome) is a path of constant bearing, which crosses all meridians at the same angle.
Sailors used to (and sometimes still) navigate along rhumb lines since it is easier to follow a constant compass bearing than to be continually adjusting the bearing, as is needed to follow a great circle. Rhumb lines are straight lines on a Mercator Projection map (also helpful for navigation).
Rhumb lines are generally longer than greatcircle (orthodrome) routes. For instance, London to New York is 4% longer along a rhumb line than along a great circle – important for aviation fuel, but not particularly to sailing vessels. New York to Beijing – close to the most extreme example possible (though not sailable!) – is 30% longer along a rhumb line.
Key to calculations of rhumb lines is the inverse Gudermannian function¹, which gives the height on a Mercator projection map of a given latitude: ln(tanφ + secφ) or ln( tan(π/4+φ/2) ). This of course tends to infinity at the poles (in keeping with the Mercator projection). For obsessives, there is even an ellipsoidal version, the ‘isometric latitude’: ψ = ln( tan(π/4+φ/2) / [ (1−e⋅sinφ) / (1+e⋅sinφ) ]^{e/2}), or its betterconditioned equivalent ψ = atanh(sinφ) − e⋅atanh(e⋅sinφ).
The formulæ to derive Mercator projection easting and northing coordinates from spherical latitude and longitude are then¹
E = R ⋅ λ  
N = R ⋅ ln( tan(π/4 + φ/2) ) 
The following formulæ are from Ed Williams’ aviation formulary.¹
Distance
Since a rhumb line is a straight line on a Mercator projection, the distance between two points along a rhumb line is the length of that line (by Pythagoras); but the distortion of the projection needs to be compensated for.
On a constant latitude course (travelling eastwest), this compensation is simply cosφ; in the general case, it is Δφ/Δψ where Δψ = ln( tan(π/4 + φ_{2}/2) / tan(π/4 + φ_{1}/2) ) (the ‘projected’ latitude difference)
Formula:  Δψ = ln( tan(π/4 + φ_{2}/2) / tan(π/4 + φ_{1}/2) )  (‘projected’ latitude difference) 
q = Δφ/Δψ (or cosφ for EW line)  
d = √(Δφ² + q²⋅Δλ²) ⋅ R  (Pythagoras)  
where  φ is latitude, λ is longitude, Δλ is taking shortest route (<180°), R is the earth’s radius, ln is natural log  
JavaScript: (all angles in radians) 
var Δψ = Math.log(Math.tan(Math.PI/4+φ2/2)/Math.tan(Math.PI/4+φ1/2)); var q = Math.abs(Δψ) > 10e12 ? Δφ/Δψ : Math.cos(φ1); // EW course becomes illconditioned with 0/0 // if dLon over 180° take shorter rhumb line across the antimeridian: if (Math.abs(Δλ) > Math.PI) Δλ = Δλ>0 ? (2*Math.PIΔλ) : (2*Math.PI+Δλ); var dist = Math.sqrt(Δφ*Δφ + q*q*Δλ*Δλ) * R; 
Bearing
A rhumb line is a straight line on a Mercator projection, with an angle on the projection equal to the compass bearing.
Formula:  Δψ = ln( tan(π/4 + φ_{2}/2) / tan(π/4 + φ_{1}/2) )  (‘projected’ latitude difference) 
θ = atan2(Δλ, Δψ)  
where  φ is latitude, λ is longitude, Δλ is taking shortest route (<180°), R is the earth’s radius, ln is natural log  
JavaScript: (all angles in radians) 
var Δψ = Math.log(Math.tan(Math.PI/4+φ2/2)/Math.tan(Math.PI/4+φ1/2)); // if dLon over 180° take shorter rhumb line across the antimeridian: if (Math.abs(Δλ) > Math.PI) Δλ = Δλ>0 ? (2*Math.PIΔλ) : (2*Math.PI+Δλ); var brng = Math.atan2(Δλ, Δψ).toDegrees(); 
Destination
Given a start point and a distance d along constant bearing θ, this will calculate the destination point. If you maintain a constant bearing along a rhumb line, you will gradually spiral in towards one of the poles.
Formula:  δ = d/R  (angular distance) 
φ_{2} = φ_{1} + δ ⋅ cos θ  
Δψ = ln( tan(π/4 + φ_{2}/2) / tan(π/4 + φ_{1}/2) )  (‘projected’ latitude difference)  
q = Δφ/Δψ (or cos φ for EW line)  
Δλ = δ ⋅ sin θ / q  
λ_{2} = λ_{1} + Δλ  
where  φ is latitude, λ is longitude, Δλ is taking shortest route (<180°), ln is natural log, R is the earth’s radius  
JavaScript: (all angles in radians) 
var δ = d/R; var Δφ = δ * Math.cos(θ); var φ2 = φ1 + Δφ; var Δψ = Math.log(Math.tan(φ2/2+Math.PI/4)/Math.tan(φ1/2+Math.PI/4)); var q = Math.abs(Δψ) > 10e12 ? Δφ / Δψ : Math.cos(φ1); // EW course becomes illconditioned with 0/0 var Δλ = δ*Math.sin(θ)/q; var λ2 = λ1 + Δλ; // check for some daft bugger going past the pole, normalise latitude if so if (Math.abs(φ2) > Math.PI/2) φ2 = φ2>0 ? Math.PIφ2 : Math.PIφ2; 

The longitude can be normalised to −180…+180 using (lon+540)%360180 
Midpoint
This formula for calculating the ‘loxodromic midpoint’, the point halfway along a rhumb line between two points, is due to Robert Hill and Clive Tooth^{1} (thx Axel!).
Formula:  φ_{m} = (φ_{1}+φ_{2}) / 2 
f_{1} = tan(π/4 + φ_{1}/2)  
f_{2} = tan(π/4 + φ_{2}/2)  
f_{m} = tan(π/4+φ_{m}/2)  
λ_{m} = [ (λ_{2}−λ_{1}) ⋅ ln(f_{m}) + λ_{1} ⋅ ln(f_{2}) − λ_{2} ⋅ ln(f_{1}) ] / ln(f_{2}/f_{1})  
where  φ is latitude, λ is longitude, ln is natural log 
JavaScript: (all angles in radians) 
if (Math.abs(λ2λ1) > Math.PI) λ1 += 2*Math.PI; // crossing antimeridian var φ3 = (φ1+φ2)/2; var f1 = Math.tan(Math.PI/4 + φ1/2); var f2 = Math.tan(Math.PI/4 + φ2/2); var f3 = Math.tan(Math.PI/4 + φ3/2); var λ3 = ( (λ2λ1)*Math.log(f3) + λ1*Math.log(f2)  λ2*Math.log(f1) ) / Math.log(f2/f1); if (!isFinite(λ3)) λ3 = (λ1+λ2)/2; // parallel of latitude 
The longitude can be normalised to −180…+180 using (lon+540)%360180 
Using the scripts in web pages
Using these scripts in web pages would be something like the following:
<!doctype html> <html lang="en"> <head> <title>Using the scripts in web pages</title> <meta charset="utf8"> <script defer src="//cdn.rawgit.com/chrisveness/geodesy/v1.1.2/latlonspherical.js"></script> <script defer src="//cdn.rawgit.com/chrisveness/geodesy/v1.1.2/dms.js"></script> <script> document.addEventListener('DOMContentLoaded', function() { document.querySelector('#calcdist').onclick = function() { const lat1 = document.querySelector('#lat1').value; const lon1 = document.querySelector('#lon1').value; const lat2 = document.querySelector('#lat2').value; const lon2 = document.querySelector('#lon2').value; const p1 = new LatLon(Dms.parseDMS(lat1), Dms.parseDMS(lon1)); const p2 = new LatLon(Dms.parseDMS(lat2), Dms.parseDMS(lon2)); const dist = parseFloat(p1.distanceTo(p2).toPrecision(4)); document.querySelector('#resultdistance').textContent = dist; } }); </script> </head> <body> <form> Lat 1: <input type="text" name="lat1" id="lat1"> Lon 1: <input type="text" name="lon1" id="lon1"> Lat 2: <input type="text" name="lat2" id="lat2"> Lon 2: <input type="text" name="lon2" id="lon2"> <button type="button" id="calcdist">Calculate distance</button> <output id="resultdistance"></output> metres </form> </body> </html>
Convert between degreesminutesseconds & decimal degrees
Notes:
 Accuracy: since the earth is not quite a sphere, there are small errors in using spherical geometry; the earth is actually roughly ellipsoidal (or more precisely, oblate spheroidal) with a radius varying between about 6,378km (equatorial) and 6,357km (polar), and local radius of curvature varying from 6,336km (equatorial meridian) to 6,399km (polar). 6,371 km is the generally accepted value for the earth’s mean radius. This means that errors from assuming spherical geometry might be up to 0.55% crossing the equator, though generally below 0.3%, depending on latitude and direction of travel (whuber explores this in excellent detail on stackexchange). An accuracy of better than 3m in 1km is mostly good enough for me, but if you want greater accuracy, you could use the Vincenty formula for calculating geodesic distances on ellipsoids, which gives results accurate to within 1mm. (Out of sheer perversity – I’ve never needed such accuracy – I looked up this formula and discovered the JavaScript implementation was simpler than I expected).
 Trig functions take arguments in radians, so latitude, longitude, and bearings in degrees (either decimal or degrees/minutes/seconds) need to be converted to radians, rad = π.deg/180. When converting radians back to degrees (deg = 180.rad/π), West is negative if using signed decimal degrees. For bearings, values in the range π to +π [180° to +180°] need to be converted to 0 to +2π [0°–360°]; this can be done by (brng+2.π)%2.π [or brng+360)%360] where % is the (floating point) modulo operator (note that different languages implement the modulo operation in different ways).
 All bearings are with respect to true north, 0°=N, 90°=E, etc; if you are working from a compass, magnetic north varies from true north in a complex way around the earth, and the difference has to be compensated for by variances indicated on local maps.
 The atan2() function widely used here takes two arguments, atan2(y, x), and computes the arc tangent of the ratio y/x. It is more flexible than atan(y/x), since it handles x=0, and it also returns values in all 4 quadrants π to +π (the atan function returns values in the range π/2 to +π/2).
 If you implement any formula involving atan2 in a spreadsheet (Microsoft Excel, LibreOffice Calc, Google Sheets, Apple Numbers), you will need to reverse the arguments, as Excel etc have them the opposite way around from JavaScript – conventional order is atan2(y, x), but Excel uses atan2(x, y). To use atan2 in a (VBA) macro, you can use WorksheetFunction.Atan2().
 If you are using Google Maps, several of these functions are now provided in the Google Maps API V3 ‘spherical’ library (computeDistanceBetween(), computeHeading(), computeOffset(), interpolate(), etc; note they use a default Earth radius of 6,378,137 meters).
 If you use UK Ordnance Survey Grid References, I have implemented a script for converting between Lat/Long & OS Grid References.
 If you use UTM coordinates or MGRS grid references, I have implemented scripts for converting between Lat/Long, UTM, & MGRS.
 I learned a lot from the US Census Bureau GIS FAQ which is no longer available, so I’ve made a copy.
 Thanks to Ed Williams’ Aviation Formulary for many of the formulæ.
 For miles, divide km by 1.609344
 For nautical miles, divide km by 1.852
See below for the JavaScript source code,
also available on GitHub.
Note I use Greek letters in variables representing maths symbols conventionally presented as Greek letters:
I value the great benefit in legibility over the minor inconvenience in typing (if you
encounter any problems, ensure your <head>
includes <meta charset="utf8">
).
With its untyped Cstyle syntax, JavaScript reads remarkably close to pseudocode: exposing the algorithms with a minimum of syntactic distractions. These functions should be simple to translate into other languages if required, though can also be used asis in browsers and Node.js.
I have extended the base JavaScript Number object with toRadians() and toDegrees() methods: I don’t see great likelihood of conflicts, as these are ubiquitous operations.
I also have a page illustrating the use of the spherical law of cosines for selecting points from a database within a specified bounding circle – the example is based on MySQL+PDO, but should be extensible to other DBMS platforms.
Several people have asked about example Excel spreadsheets, so I have implemented the distance & bearing and the destination point formulæ as spreadsheets, in a form which breaks down the all stages involved to illustrate the operation.
January 2010: I have revised the scripts to be structured as methods of a LatLon object.
Of course, while JavaScript is objectoriented,
it is a prototypebased
rather than classbased language, so this is not actually a class, but isolating code into a separate namespace
is good JavaScript practice.
If you’re not familiar with JavaScript syntax, LatLon.prototype.distanceTo = function(point)
{ ... }
, for instance, defines a ‘distanceTo
’ method of the LatLon
object
(/class) which takes a LatLon
object as a parameter (and returns a number). The
Dms namespace acts as a static class for geodesy formatting / parsing / conversion functions.
January 2015: I have refactored the scripts to interoperate better, and rationalised certain aspects: the
JavaScript file is now latlonspherical.js instead of simply latlon.js; distances are now always in metres; the earth’s
radius is now a parameter to distance calculation methods rather than to the constructor; the
previous Geo
object is now Dms
, to better indicate its purpose; the
destinationPoint
function has the distance parameter before the bearing.
Performance: as noted above, the haversine distance calculation takes around 2 – 5 microseconds (hence around 200,000 – 500,000 per second). I have yet to complete timing tests on other calculations.
Other languages: I cannot support translations into other languages, but if you have ported the code to another language, I am happy to provide links here.
 Brian Lambert has made an ObjectiveC version.
 Jean Brouwers has made a Python version.
I offer these scripts for free use and adaptation to balance my debt to the opensource infoverse. You are welcome to reuse these scripts [under an MIT licence, without any warranty express or implied] provided solely that you retain my copyright notice and a link to this page.
If you would like to show your appreciation and support continued development of these scripts, I would most gratefully accept donations.
If you need any advice or development work done, I am available for consultancy.
If you have any queries or find any problems, contact me at ku.oc.epytelbavom@oegstpircs.
© 20022017 Chris Veness