I have a three part question:(adsbygoogle = window.adsbygoogle || []).push({});

Background: For a planet on an orbit with semi-major axis a and eccentricity e, the distance of closest approach to the Sun is r = a(1 − e) and the farthest approach is r = a(1 + e).

(1) Assuming an albedo A = 0.2, estimate the temperature on Earth in equilibrium with irradiation from

the Sun. Estimate the correction factor necessary due to the greenhouse eﬀect to bring us up to a balmy 300 K.

I don't know what to do.

(2) Assuming that this correction factor does not change, how large an eccentricity could the Earth have before the temperature extremes reach the point where the Earth reaches either boiling or freezing point?

Freezing:

Based off the equation T=T⊙((1-A)/4)^0.25(R⊙/r)^0.5,

273.15=5778((1-0.2)/4)^0.25(6.96*10^8/r)^0.5

0.005=(6.96/r)

r=1.39*10^11

Boiling:

373.15=5778((1-0.2)/4)^0.25(6.96*10^8/r)^0.5

r=7.46*10^10

These both seem reasonable to me except for one thing. The actual distance from the Sun to the Earth is 1.5*10^11. This means that the Earth is actually farther than the distance I calculated for the boiling part, which doesn't make sense.

Is this the equation I should use, and is the work (and answer) correct? Or did I do something wrong?

(3) If we deﬁne habitability as having a level of irradiation between these two extremes, consider the

habitable zone around a lower mass star. Assuming circular orbits again, and the same greenhouse correction factor as above, where is the habitable zone around a 0.5M⊙ star, which has radius 0.5R⊙ and eﬀective temperature 3700 K?

Not sure where exactly to get started here.

Do I use the equations

L=4*pi*R⊙^2*stefan-boltzmann constant*T⊙^4

Labs=((R⊙^2*stefan-boltzmann constant*T⊙^4*pi*R^2)/r^2)(1-A)?

Not sure where the mass of the star fits in here.

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# Calculating albedo and eccentricity

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