Difference between revisions of "Absolute Magnitude"

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'''Magnitude''' is a measure of the brightness of an object. The scale is logrithmic and the brighter the object the lower the number. Magnitude is usually one of two types ''Apparent Magnitude'' (m) and ''Absolute Magnitude'' (M).
 
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On ancient [[Terra]] the stars of the sky were divided into 6 magnitudes, with 1 being the brightest and 6 the faintest with each division being approximately 2 times difference, this was later revised so that a 1<sup>st</sup> magnitude star was 100 times brighter than a 6<sup>th</sup> magnitude star. First [[Polaris (star)|Polaris]] then [[Vega (star)|Vega]] were taken to be the 0 point on the scale. So each step is the fifth root of 100 different (2.512).
 
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Magnitude is not limited to the 0-6 scale, most primary stars will be highly negative (Sol from Terra is −26.73). The faintest magnitude visible with a [[Humaniti]] eye is 6.5. Binoculars give 9.5, and an 8m ground telescope can resolve to 27.
 
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;Apparent Magnitude
 
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:a measure of its brightness as seen by an observer on the ground, normalized to the value it would have in the absence of the atmosphere
 
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;Absolute Magnitude
 
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:the apparent magnitude, an object would have if it were at a standard luminosity distance away from us, in the absence of interstellar extinction
 
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'''Absolute Magnitude''' is the apparent magnitude at 10 [[parsec]]s. Given the absolute magnitude and the distance to a star, the apparent magnitude can be caclulated by: <math>m = M + 5((\log_{10}D)-1)</math> where D is the distance in Parsecs (must be adjusted for extra galactic objects). Thus [[Antares (star)|Antares]] at M -5.28 as seen from [[Capital (world)|Capital]] (distance of ~38 parsecs) would be:<br><math>m = -5.28 + 5((\log_{10}38)-1)</math><br><math>m = -5.28 + 5(1.58-1)</math><br><math>m = -5.28 + 5(0.58)</math><br><math>m=-5.28 + 2.9</math><br><math>m=-2.38</math>
 
'''Absolute Magnitude''' is the apparent magnitude at 10 [[parsec]]s. Given the absolute magnitude and the distance to a star, the apparent magnitude can be caclulated by: <math>m = M + 5((\log_{10}D)-1)</math> where D is the distance in Parsecs (must be adjusted for extra galactic objects). Thus [[Antares (star)|Antares]] at M -5.28 as seen from [[Capital (world)|Capital]] (distance of ~38 parsecs) would be:<br><math>m = -5.28 + 5((\log_{10}38)-1)</math><br><math>m = -5.28 + 5(1.58-1)</math><br><math>m = -5.28 + 5(0.58)</math><br><math>m=-5.28 + 2.9</math><br><math>m=-2.38</math>
 
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== Description / Specifications ==
 
Absolute/Apparent Magnitudes for comparison:
 
Absolute/Apparent Magnitudes for comparison:
 
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| 12.8
 
| 12.8
 
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*Note the numbers in () above are for adjusted locations of stars on the maps.
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* Note the numbers in () above are for adjusted locations of stars on the maps.
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{{Sources
 
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|S1=Wikipedia (various)}}
 
  
 +
== History & Background / Dossier ==
 +
'''Magnitude''' is a measure of the brightness of an object. The scale is logrithmic and the brighter the object the lower the number. Magnitude is usually one of two types ''Apparent Magnitude'' (m) and ''Absolute Magnitude'' (M).
 +
On ancient [[Terra]] the stars of the sky were divided into 6 magnitudes, with 1 being the brightest and 6 the faintest with each division being approximately 2 times difference, this was later revised so that a 1<sup>st</sup> magnitude star was 100 times brighter than a 6<sup>th</sup> magnitude star. First [[Polaris (star)|Polaris]] then [[Vega (star)|Vega]] were taken to be the 0 point on the scale. So each step is the fifth root of 100 different (2.512).
  
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{{LE|M}}
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Magnitude is not limited to the 0-6 scale, most primary stars will be highly negative (Sol from Terra is −26.73). The faintest magnitude visible with a [[Humaniti]] eye is 6.5. Binoculars give 9.5, and an 8m ground telescope can resolve to 27.
−
 
+
−
 
+
;Apparent Magnitude
−
 
+
:a measure of its brightness as seen by an observer on the ground, normalized to the value it would have in the absence of the atmosphere
−
== Description / Specifications ==
+
;Absolute Magnitude
−
No information yet available.
+
:the apparent magnitude, an object would have if it were at a standard luminosity distance away from us, in the absence of interstellar extinction
−
 
 
−
== History & Background / Dossier ==
 
−
No information yet available.
 
  
 
== References & Contributors / Sources ==
 
== References & Contributors / Sources ==
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{{Detail}}
 
{{Detail}}
 
{{Sources
 
{{Sources
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|S1= TBD
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|S1= Wikipedia (various)
 
|S2= [[Traveller Wiki Editorial Team]]
 
|S2= [[Traveller Wiki Editorial Team]]
 
|S3= Author & Contributor: Lord (Marquis) and Master of Sophontology [[User:Maksim-Smelchak|Maksim-Smelchak]] of the [[Ministry of Science]]  
 
|S3= Author & Contributor: Lord (Marquis) and Master of Sophontology [[User:Maksim-Smelchak|Maksim-Smelchak]] of the [[Ministry of Science]]  

Revision as of 05:12, 18 May 2018

Absolute Magnitude is the apparent magnitude at 10 parsecs. Given the absolute magnitude and the distance to a star, the apparent magnitude can be caclulated by: <math>m = M + 5((\log_{10}D)-1)</math> where D is the distance in Parsecs (must be adjusted for extra galactic objects). Thus Antares at M -5.28 as seen from Capital (distance of ~38 parsecs) would be:
<math>m = -5.28 + 5((\log_{10}38)-1)</math>
<math>m = -5.28 + 5(1.58-1)</math>
<math>m = -5.28 + 5(0.58)</math>
<math>m=-5.28 + 2.9</math>
<math>m=-2.38</math>

Description / Specifications

Absolute/Apparent Magnitudes for comparison:

Object Absoulte Magnitude Apparent Magnitude (Terra) Apparent Magnitude (Capital)
Sun 4.83 −26.73 10.38
Moon (full) n/a −12.6 n/a
Visible during Daylight n/a −3.9 -3.9
Moon (new) n/a –2.5 n/a
Sirius Brightest Star 1.42 −1.47 6.97
Canopus 2nd Brightest star −5.53 -0.7 (-2.04) (0.73)
Vega 5th Brightest star 0.58 0.03 5.96
Antares 16th Brightest star −5.28 1.09 (0.83) -1.35 (-2.38)
Deneb 19th Brightest star −8.73 1.25 (-2.2) 0.96 (-3.09)
LBV 1806-20 −14.2 8.4 8.4
Quasar 3C 273 −26.7 12.8 12.8
  • Note the numbers in () above are for adjusted locations of stars on the maps.

History & Background / Dossier

Magnitude is a measure of the brightness of an object. The scale is logrithmic and the brighter the object the lower the number. Magnitude is usually one of two types Apparent Magnitude (m) and Absolute Magnitude (M). On ancient Terra the stars of the sky were divided into 6 magnitudes, with 1 being the brightest and 6 the faintest with each division being approximately 2 times difference, this was later revised so that a 1st magnitude star was 100 times brighter than a 6th magnitude star. First Polaris then Vega were taken to be the 0 point on the scale. So each step is the fifth root of 100 different (2.512).

Magnitude is not limited to the 0-6 scale, most primary stars will be highly negative (Sol from Terra is −26.73). The faintest magnitude visible with a Humaniti eye is 6.5. Binoculars give 9.5, and an 8m ground telescope can resolve to 27.

Apparent Magnitude
a measure of its brightness as seen by an observer on the ground, normalized to the value it would have in the absence of the atmosphere
Absolute Magnitude
the apparent magnitude, an object would have if it were at a standard luminosity distance away from us, in the absence of interstellar extinction

References & Contributors / Sources

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