The figure below is a scaled representation of a planet's orbit with a semimajor axis of 1.528 AU. (Use the exact values you enter in previous answer(s) to make later calculation(s).)
(a) Find the ratio of the aphelion-to-perihelion distance.
rA
rP
=
(b) Find the perihelion and aphelion distances in astronomical units.
rP =
AU
rA =
AU
(c) Find the distance the Sun is from the center of the orbit.
AU
I know answer for a) is 1.5
If you want to see the figure, then type the website below part by part because jiskha doesn't allow the whole link be posted on it site.
part1:world wide web
part2: webassign.
part2: net
part:3: /katzpse1/
part4: 7-p-009.gif
a)=1.5
b)rP=1.22AU
b) rA=1.70AU
c)d=.308AU
To find the ratio of the aphelion-to-perihelion distance, we need to know the eccentricity of the orbit. The eccentricity of an orbit determines how elongated or circular it is.
If the eccentricity of the orbit is known, we can use the formula:
Ratio of aphelion-to-perihelion distance = 1 + eccentricity
However, the eccentricity of the orbit is not given in the question. Therefore, we cannot directly find the ratio of the aphelion-to-perihelion distance.
Moving on to part (b), to find the perihelion and aphelion distances in astronomical units, we need to know the semimajor axis of the orbit. The semimajor axis (a) is the average distance from the center of the orbit to the furthest and closest points to the Sun (aphelion and perihelion, respectively) in an elliptical orbit.
Given the semimajor axis (a) value of 1.528 AU, we can calculate the perihelion (rP) and aphelion (rA) distances using the following formulas:
rP = a * (1 - eccentricity)
rA = a * (1 + eccentricity)
Since we do not have the eccentricity value, we cannot directly find the perihelion and aphelion distances in astronomical units.
Moving on to part (c), to find the distance the Sun is from the center of the orbit, we need to calculate the semi-latus rectum (ℓ). The semi-latus rectum is a value associated with an ellipse and is determined by the eccentricity of the orbit.
The formula to calculate the semi-latus rectum is:
ℓ = a * (1 - eccentricity^2)
Again, since we do not have the eccentricity value, we cannot directly find the distance the Sun is from the center of the orbit.