03.10.2014 Views

Falsification Of The Atmospheric CO2 Greenhouse Effects Within ...

Falsification Of The Atmospheric CO2 Greenhouse Effects Within ...

Falsification Of The Atmospheric CO2 Greenhouse Effects Within ...

SHOW MORE
SHOW LESS

You also want an ePaper? Increase the reach of your titles

YUMPU automatically turns print PDFs into web optimized ePapers that Google loves.

<strong>Falsification</strong> <strong>Of</strong> <strong>The</strong> <strong>Atmospheric</strong> CO 2 <strong>Greenhouse</strong> <strong>Effects</strong> . . . 19<br />

∫ √<br />

= 2π · I 0 · a 2 R0 2<br />

·<br />

+a2<br />

a<br />

⎛<br />

⎝− 1<br />

= 2π · I 0 · a 2 ·<br />

= π · I 0 · a 2 ·<br />

= π · I 0 ·<br />

(b) Two parallel areas with distance a → 0<br />

1<br />

r 3 dr<br />

√ ⎞<br />

∣ ∣∣∣ R 2<br />

0 +a 2<br />

⎠<br />

2r 2 a<br />

( )<br />

1<br />

a − 1<br />

2 R0 2 + a 2<br />

R 2 0<br />

R 2 0 + a 2 (16)<br />

If the distance a is becoming very small whereas R 0 is kept finite one will have<br />

(<br />

R 2 )<br />

0<br />

I parallel areas (a→0) = lim π · I 0 · = πI<br />

a→0 R0 2 + a 2 0 (17)<br />

This relation corresponds to the total half-space intensity for a radiation from a unit<br />

surface.<br />

(c) <strong>The</strong> Earth illuminated by the Sun<br />

With I Sun<br />

0 being the factor I 0 for the Sun the solar total half-space intensity is given by<br />

Setting<br />

one gets for the solar intensity at the Earth’s orbit<br />

I Earth’s orbit = π · I Sun<br />

0 ·<br />

2.1.4 <strong>The</strong> Stefan-Boltzmann law<br />

I Sun’s surface = π · I Sun<br />

0 (18)<br />

a = R Earth’s orbit (19)<br />

R 0 = R Sun (20)<br />

R 2 Sun<br />

R 2 Sun + R 2 Earth’s orbit<br />

R 2 Sun<br />

= I Sun’s surface ·<br />

R 2 Sun + R 2 Earth’s orbit<br />

≈ I Sun’s surface ·<br />

≈ I Sun’s surface ·<br />

R 2 Sun<br />

R 2 Earth’s orbit<br />

1<br />

(215) 2 (21)<br />

For a perfect black body and a unit area positioned in its proximity we can compute the<br />

intensity I with the aid of the the Kirchhoff-Planck-function, which comes in two versions<br />

B ν (T ) =<br />

[ ( ) −1 2hν3 hν<br />

exp − 1]<br />

c 2 kT<br />

(22)<br />

B λ (T ) =<br />

[ ( ) −1 2hc2 hc<br />

exp − 1]<br />

λ 5 λkT<br />

(23)

Hooray! Your file is uploaded and ready to be published.

Saved successfully!

Ooh no, something went wrong!