« Last post by KathAveara on October 08, 2014, 11:26:24 AM »
I certainly would.
In fact, I can write an algorithm to map stars in our night sky to those in Epsilon Eridani's night sky. I'll need to know what the co-ordinates are measured in, though.
Edit: Assuming your data uses right ascension and declination (and to be honest, there's no reason why not. But if not, you can find said data on the internet), use the following:
Right ascension and declination are angles, conventionally measured in hours, minutes, and seconds. 1 hour = 15°, 1 minute = 1/4°, 1 second = 1/240°. Distances are measured in light years or parsecs. The more accurate the data, the better.
α = right ascension (measured from Sol)
δ = declination (measured from Sol)
r = distance between Sol and star
αε = right ascension (measured from Epsilon Eridani)
δε = declination (measured from Epsilon Eridani)
α₀ = right ascension (of Epsilon Eridani)
δ₀ = declination (of Epsilon Eridani)
r₀ = distance between Sol and Epsilon Eridani
X = r*cos(α-α₀)*cos(δ-δ₀)
Y = r*sin(α-α₀)*cos(δ-δ₀)
Z = r*sin(δ-δ₀)
R = √(r₀² - 2*r₀*X + r²)
δε = arcsin(-Z/R)
αε = arcsin(-Y/(R*cos(δε)))
Note that for Sol, δε = 0, αε = 0.
The logic behind this is as follows: first, realign the axes so that Epsilon Eridani is at 0°/0°. Then, convert the polar co-ordinates (right ascension, declination, distance) into cartesian co-ordinates (x, y, z). Shift the origin to Epsilon Eridani, and convert the cartesian co-ordinates back into polar co-ordinates for plotting on a celestial sphere.
Apparent magnitude can presumably be calculated from absolute magnitude and R (which happens to be the distance between the star and Epsilon Eridani. For Sol, this obviously equals r₀).