Astronomy & space · University
Flux, luminosity and stellar magnitudes
Luminosity is emitted power; flux is received power per area. For isotropic emission with negligible absorption, F=L/(4πd²).
Prerequisites
Logarithms and inverse-square relationships.
Study notes
Luminosity and flux
Luminosity is emitted power; flux is received power per area. For isotropic emission with negligible absorption, F=L/(4πd²).
Magnitude
Magnitude differences use a logarithmic scale: m2−m1=−2.5 log10(F2/F1). A smaller magnitude denotes a brighter source in the same band.
Absolute magnitude
Absolute magnitude compares sources at the conventional distance of 10 pc. Bandpass and extinction assumptions must be specified.
Distance modulus
Ignoring extinction, m−M=5 log10(d/10 pc). Dust can dim and redden a source, so uncorrected brightness is not purely a distance indicator.
Worked examples
For equal luminosity and negligible absorption, one source is twice as far away. Find its flux divided by the nearer source's flux.
The inverse-square law gives 1/2².
0.25
A source becomes 100 times brighter in the same band. Find mnew−mold.
−2.5 log10(100)=−5.
-5
Check your understanding
Which quantity describes emitted power rather than received power per area?
- Luminosity
- Parallax angle
- Apparent magnitude by itself
- Flux
Ignoring extinction, find m−M for d=100 pc.
At which conventional distance is absolute magnitude defined?
- 1 km
- 1 AU
- 1000 light-years
- 10 pc
Why can two equally bright-looking stars have different luminosities?
Answers and marking guidance
Answers and marking notes
- Luminosity
Luminosity is intrinsic emitted power under the model.
- 5
5 log10(100/10)=5.
- 10 pc
Absolute magnitude standardizes the distance at 10 parsecs.
- Their distances and intervening extinction can differ. The received flux alone does not uniquely determine luminosity.
Credit distance and at least the possibility of absorption.
Further reading and review references
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