Answer:
1.[tex]I=5200\frac{W}{m^2}[/tex]
2.[tex]I=325\frac{W}{m^2}[/tex]
3.[tex]I=26.53\frac{W}{m^2}[/tex]
Explanation:
The apparent brightness is inversally proportional to the square of distance, and it can be written as:
[tex]\frac{I_{1}}{I_{2}} =\frac{r_{2}^2}{r_{1}^2}[/tex]
Where, for instance, state 1 is the Earth (given, known values) and state 2 is the unknown value. Knowing a new distance leads to a known apparent brightness, and viceversa.
This is a very simple proportionallity law, so, rearranging the equation:
[tex]I_{2}=I_{1}\frac{r_{1}^2}{r_{2}^2}=I_{1}(\frac{r_{1}}{r_{2}})^2[/tex]
1. For a distance of half the distance from the Sun (i.e., 0.5 AU, regardless its actual value since we are using AU multiples):
[tex]I_{2}=1300\cdot2^2=5200\frac{W}{m^2}[/tex]
2. Similarly, for r2=2AU:
[tex]I_{2}=1300\cdot0.5^2=325\frac{W}{m^2}[/tex]
3. Finally, for r2=7AU:
[tex]I_{2}=1300\cdot\frac{1}{7^2}=26.53\frac{W}{m^2}[/tex]