Distance Between Two Stars Right Ascension (H M S  or H.hhh) Declination (D M S  or D.ddd) Dist   LY Vis Mag 1st Star 2nd Star NOTE: Decimal RA and declination arguments may also be used: e.g., `06 33 27` is equivalent to `6.5575` Computing the Distance Between Two Stars In this case of computing the distance between two stars, we are treating the stars as simple points in 3D space.  So, finding the distance between them, becomes a simple matter of 3D trigonometry. In astronomy, we generally give stars 3D spherical coordinates.   They are the standard right ascension, declination and distance coordinates of the stars.  On Earth we use longitude and latitude, in astronomy, we use right ascension and declination respectively as coordinates.   These standard stellar coordinates are cataloged for many stars (Epoch J2000 is used here) and they can be used for 3D computations to the extent of their accuracy. The 3rd coordinate, the distance, is often symbolized by R because it represents the radius vector (radius of a sphere), the line directed between the eye and star.  The coordinates are envisioned as a grid drawn on the surface of an infinitely large sphere with our eye at the center and the star at distance R from the eye with apparent longitude (right ascension) and latitude (declination) coordinates as viewed projected against the sphere. From the stellar spherical coordinates (α,δ,R), we can compute the corresponding rectangular (X,Y,Z)coordinates from which the linear spatial distance (D) between the two stars can then be computed. For any given star, let: Given the spherical (α,δ,R) coordinates of a planet or star, the corresponding rectangular (X,Y,Z) coordinates may be computed from: Given the spherical (α,δ,R) coordinates for two stars, distinguished by subscripts,to compute the distance between the stars, we first compute their correspondingrectangular (X,Y,Z) coordinates: For the first star: For the second star: The distance between the two stars in 3D XYZ-space may then be computed as the square root of the sum of the squares of the differences between their rectangular coordinates: A Numerical Example - Part 1: In this example we will compute the distance between the bright stars Sirius (= 1st Star) and Vega (= 2nd Star) and then compute how bright each star would appear to be from the perspective of the other. This is the computational data pertaining to the stars used in the example: ```J2000.0 CATALOG DATA FOR SIRIUS AND VEGA AS VIEWED FROM EARTH/SUN -------- --------------- ---------------- ------- ------- 1ST STAR RIGHT ASCENSION DECLINATION DIST LY VIS MAG Sirius 06h 45m 08.9s -16° 42' 58" 8.6 -1.46 101.2870833 deg -16.7161111 deg -------- --------------- ---------------- ------- ------- 2ND STAR RIGHT ASCENSION DECLINATION DIST LY VIS MAG Vega 18h 36m 56.3s +38° 47' 01" 25.3 +0.03 279.2345833 deg +38.7836111 deg ``` Performing the distance computations for the given data (Angles expressed in degrees): ```DISTANCE BETWEEN THE STARS SIRIUS AND VEGA Rectangular Coordinates of Sirius: x1 = 8.6 * Cos(101.2870833) * Cos(-16.7161111) = -1.6121048578 y1 = 8.6 * Sin(101.2870833) * Cos(-16.7161111) = 8.0772729746 z1 = 8.6 * Sin(-16.7161111) = -2.4736166278 Rectangular Coordinates of Vega: x2 = 25.3 * Cos(279.2345833) * Cos(38.7836111) = 3.1648925282 y2 = 25.3 * Sin(279.2345833) * Cos(38.7836111) = -19.4661817544 z2 = 25.3 * Sin(+38.7836111) = 15.8474358553 Rectangular Coordinate Differences: dx = (x2 - x1) = 4.7769973860 dy = (y2 - y1) = -27.5434547290 dz = (z2 - z1) = 18.3210524831 The distance (D) between the stars Sirius and Vega may then be found from: D = SqRoot(dx*dx + dy*dy + dz*dz) = 33.4233835290 LY So, D = 33.42 light years ``` APPARENT BRIGHTNESS Once we know the distance (D) between two stars, we may then determine how bright each star would appear to be (ideally) as viewed from the other's perspective, as opposed to their apparent brightness (or magnitudes) as viewed from Earth. In this case, the general stellar magnitude vs. distance formula may be expressed as: Where: m = Visual magnitude of star as viewed from distance d M = Visual magnitude of star as viewed from distance D d and m respectively refer to the distance to and visual magnitude of one of the stars as viewed from Earth. D is the distance between the two stars previously computed above. M is the visual magnitude of one of the stars at distance D. The known values are (d, m, D) from which we compute M for each star. Numerical Example Continued - Part 2: ```From Sirius (Star 2 as viewed from Star 1 Vega): m = +0.03 = Magnitude of Vega as viewed from Earth d = 25.3 = Distance to Vega from Earth in light years D = 33.423 = Distance between Sirius and Vega in light years M = Magnitude of Vega as viewed from Sirius M = 5*Log10(D/d) + m M = 5*Log10(33.423/25.3) + 0.03 = 0.604625 + 0.03 = 0.634625 So, from Sirius, the magnitude of Vega would be +0.63 ============================================================== From Vega (Star 1 as viewed from Star 2 Sirius): m = -1.46 = Magnitude of Sirius as viewed from Earth d = 8.6 = Distance to Sirius from Earth in light years D = 33.423 = Distance between Sirius and Vega in light years M = Magnitude of Sirius as viewed from Vega M = 5*Log10(D/d) + m M = 5*Log10(33.423/8.6) + (-1.46) = 2.947735 - 1.46 = 1.487735 So, from Vega, the magnitude of Sirius would be +1.49 ``` Jay Tanner - 2019