Stars, radiation and scale
導入済み| English | 意味 |
|---|---|
| flux/flʌks/ | フラックス |
| luminosity/ˌluːmɪˈnɒsɪti/ | 光度 |
What would explain this observation?
- Two stars can have the same apparent brightness while having different luminosities. Distance changes the flux 通量 reaching an observer.
- Start with a prediction. State the quantities or features you would compare, then decide what evidence could distinguish two explanations.
Build the model
- Luminosity 光度 is total power emitted; flux is power received per area. A stellar spectrum carries information about surface temperature and composition. Fusion transfers energy as light nuclei combine.
- luminosity: Total emitted power; flux: Power received per unit area.
At fixed luminosity, what happens to flux when distance doubles?
難易度 1/5 · 100 コイン + 今日初回完了時に小ボーナス付与
Flux follows an inverse-square law, F proportional to 1/d^2, because the same luminosity spreads over a sphere of area 4 pi d^2. Doubling d gives 1/4 of the flux - not a half.
Match each technical term to its precise meaning.
難易度 2/5 · 140 コイン + 今日初回完了時に小ボーナス付与
Use the definitions to distinguish related quantities and processes.
Choose evidence that can test it
- For isotropic emission without absorption, flux follows an inverse-square relationship with distance. Observed brightness alone therefore cannot establish luminosity.
- Keep distance units consistent, identify which quantities are intrinsic to the star, and distinguish observational evidence from a model of stellar evolution. Do not confuse a red giant stage with every possible final remnant.
Which two habits make the investigation or model in this case more defensible?
難易度 2/5 · 140 コイン + 今日初回完了時に小ボーナス付与
Stating the conditions and assumptions lets others repeat the work exactly, and recording the supporting evidence lets them check the conclusion. Hiding disagreeing results removes the evidence that could challenge a wrong conclusion, and one measurement can never establish a wider claim.
Work from known quantities
- State the known values and their units. Choose the relation because its assumptions fit this case, then rearrange before substitution.
- Known: distance doubles while luminosity remains fixed. Use F proportional to 1/d². Flux ratio = 1/2² = 1/4. A flux of 12 units becomes 3 units. This assumes no change in absorption or source output.
A source gives flux 18 units. Find flux at three times the distance. Use the same sequence: known quantities → model → relation → substitution → unit and interpretation.
A source gives flux 18 units. Find flux at three times the distance.
難易度 2/5 · 140 コイン + 今日初回完了時に小ボーナス付与
The result is 2 . Known: flux 18 units at the original distance; distance triples. Use F proportional to 1/d^2. New flux = 18/3^2 = 18/9 = 2 units. This assumes constant luminosity and no extra absorption.
Check the conclusion and its limits
- The Sun is not expected to become a supernova. Redshift can support cosmological expansion; it does not mean every nearby object must move away from every observer.
- Return to the original observation. Explain what the result supports, which conditions it assumes, and one way to test a competing explanation.
Apparent brightness alone always determines a star luminosity. This claim is false: Apparent brightness depends on distance as well as luminosity (F = L/4 pi d^2). A dim-looking star may be very luminous but far away, so brightness alone cannot fix luminosity without a distance.
Stars, radiation and scale: For isotropic emission without absorption, flux follows an inverse-square relationship with distance. Observed brightness alone therefore cannot establish luminosity.
Apparent brightness alone always determines a star luminosity.
難易度 1/5 · 100 コイン + 今日初回完了時に小ボーナス付与
Apparent brightness depends on distance as well as luminosity (F = L/4 pi d^2). A dim-looking star may be very luminous but far away, so brightness alone cannot fix luminosity without a distance.
Total emitted power: write the technical term.
難易度 1/5 · 100 コイン + 今日初回完了時に小ボーナス付与
luminosity means Total emitted power.