Difference between revisions of "Magnitude"
GypsyComet (talk | contribs) m |
|||
| (9 intermediate revisions by 2 users not shown) | |||
| Line 1: | Line 1: | ||
| − | [[Magnitude]] is a unit of measure for the brightness (or visibility) of stellar object | + | [[File: Wiki Navy.png|right]] |
| − | + | [[Magnitude]] is a unit of measure for the brightness (or visibility) of stellar object. | |
| − | + | ||
| + | == Description ([[Specifications]]) == | ||
| + | Absolute magnitudes for stars generally range from -10 to +17. | ||
| − | Absolute | + | There are two kinds of magnitude: |
| + | # ''Apparent Magnitude'' (''m'') which measures the brightness of a stellar object from the point of view of the observer. | ||
| + | # ''Absolute Magnitude'' (''M'') measures the brightness of a stellar object from 10 [[parsec]]s, or a planetary object from 1 [[Astronomical unit]]. | ||
| + | === Points of Reference === | ||
Some points of reference: | Some points of reference: | ||
* Sol from Terra: -26.73 | * Sol from Terra: -26.73 | ||
| Line 13: | Line 18: | ||
* Faintest objects visible with binoculars: 9.5 | * Faintest objects visible with binoculars: 9.5 | ||
| − | == Conversion == | + | === Conversion === |
Given the absolute magnitude <math>M\!\,</math>, for objects within our galaxy you can also calculate the apparent magnitude <math>m\!\,</math> from any distance <math>D_L\!\,</math>: | Given the absolute magnitude <math>M\!\,</math>, for objects within our galaxy you can also calculate the apparent magnitude <math>m\!\,</math> from any distance <math>D_L\!\,</math>: | ||
| Line 23: | Line 28: | ||
where <math>D_L\!\,</math> is the star's luminosity distance in [[parsec]]s, which are (≈ 3.2616 [[light-year]]s) | where <math>D_L\!\,</math> is the star's luminosity distance in [[parsec]]s, which are (≈ 3.2616 [[light-year]]s) | ||
| + | == History & Background ([[Dossier]]) == | ||
| + | The original magnitude measurement was a scale of 1 to 6 to categorize the stars visible in the [[Terra (world)|Terran]] skies. This was later formalized into a logarithmic scale, with the smaller numbers indicating brighter objects than larger ones. The scale is defined such that each 5 points magnitude is 100 times brighter (or dimmer). The scale also extends into the negative numbers, so for example magnitude -5 is 100 times brighter than magnitude 0. | ||
| + | |||
| + | == References & Contributors ([[Sources]]) == | ||
| + | {{Wikipedia|Absolute_magnitude}} | ||
{{Wikipedia|Apparent_magnitude}} | {{Wikipedia|Apparent_magnitude}} | ||
| − | {{ | + | {{Intermediate}} |
| + | {{Sources | ||
| + | |S2= [[Traveller Wiki Editorial Team]] | ||
| + | }} | ||
| − | {{LE|Metric| | + | {{LEN|Star}} |
| + | {{LE|Metric|}} | ||
Latest revision as of 03:09, 23 October 2023
Magnitude is a unit of measure for the brightness (or visibility) of stellar object.
Description (Specifications)[edit]
Absolute magnitudes for stars generally range from -10 to +17.
There are two kinds of magnitude:
- Apparent Magnitude (m) which measures the brightness of a stellar object from the point of view of the observer.
- Absolute Magnitude (M) measures the brightness of a stellar object from 10 parsecs, or a planetary object from 1 Astronomical unit.
Points of Reference[edit]
Some points of reference:
- Sol from Terra: -26.73
- Projects enough light to cast shadows: -5
- Faintest objects observable during the day with naked eye: −3.9
- Faintest stars visible in an urban neighborhood with naked eye: 3
- Faintest stars observable with naked eye under perfect conditions: 6.5
- Faintest objects visible with binoculars: 9.5
Conversion[edit]
Given the absolute magnitude <math>M\!\,</math>, for objects within our galaxy you can also calculate the apparent magnitude <math>m\!\,</math> from any distance <math>D_L\!\,</math>:
- <math> m = M + 5 (\log_{10}{D_L} - 1)\!\,</math>
One can compute the absolute magnitude <math>M\!\,</math> of an object given its apparent magnitude <math>m\!\,</math> and luminosity distance <math>D_L\!\,</math>:
- <math> M = m - 5 ((\log_{10}{D_L}) - 1)\!\,</math>
where <math>D_L\!\,</math> is the star's luminosity distance in parsecs, which are (≈ 3.2616 light-years)
History & Background (Dossier)[edit]
The original magnitude measurement was a scale of 1 to 6 to categorize the stars visible in the Terran skies. This was later formalized into a logarithmic scale, with the smaller numbers indicating brighter objects than larger ones. The scale is defined such that each 5 points magnitude is 100 times brighter (or dimmer). The scale also extends into the negative numbers, so for example magnitude -5 is 100 times brighter than magnitude 0.
References & Contributors (Sources)[edit]
| This page uses content from Wikipedia. The original article was at Absolute_magnitude. The list of authors can be seen in the page history. The text of Wikipedia is available under the Commons Attribution-ShareAlike 3.0 Unported License. |
| This page uses content from Wikipedia. The original article was at Apparent_magnitude. The list of authors can be seen in the page history. The text of Wikipedia is available under the Commons Attribution-ShareAlike 3.0 Unported License. |
