Astronomy "before the Common Era" - Revision history

Cosmo All: /* Problem 4: distance to the Sun */

2012-10-15T14:11:40Z

‎Problem 4: distance to the Sun

2012-10-15T14:10:57Z

‎Problem 4: distance to the Sun

2012-10-15T14:10:13Z

‎Problem 4: distance to the Sun

2012-10-15T14:08:20Z

‎Problem 4: distance to the Sun

2012-10-15T14:07:45Z

‎Problem 4: distance to the Sun

2012-10-15T14:07:15Z

‎Problem 4: distance to the Sun

2012-10-15T14:06:48Z

‎Problem 4: distance to the Sun

2012-10-15T14:06:23Z

‎Problem 4: distance to the Sun

2012-10-15T14:05:18Z

‎Problem 4: distance to the Sun

2012-10-11T12:55:06Z

‎Problem 12: getting rid of $c$

@@ Line 65: / Line 65: @@
 	=\frac{1}{\pi}\frac{T}{\tau},\]
 here $\tau=1~h$ and $T$ is the period of Moon revolution around the Earth, which equals to one month. Calculating, we set $r_{\odot}\sim1.50\cdot 10^{8}~km$, which is correct by the order of magnitude. The error is caused by not exact circularity of the Moon's orbit (the distance to the Moon is $405\cdot 10^3~km$ in apogee and $363\cdot10^3~km$ in perigee). Given the distances to the Sun and the Moon, recalling that their angular sizes are quite close, it's easy to estimate the size of the Sun.
-<gallery widths=500px>File:1_MoonPhasesSolution3.JPG|</gallery></p>
+<gallery widths=500px heights=300px>File:1_MoonPhasesSolution3.JPG|</gallery></p>
    </div>
 </div></div>

@@ Line 65: / Line 65: @@
 	=\frac{1}{\pi}\frac{T}{\tau},\]
 here $\tau=1~h$ and $T$ is the period of Moon revolution around the Earth, which equals to one month. Calculating, we set $r_{\odot}\sim1.50\cdot 10^{8}~km$, which is correct by the order of magnitude. The error is caused by not exact circularity of the Moon's orbit (the distance to the Moon is $405\cdot 10^3~km$ in apogee and $363\cdot10^3~km$ in perigee). Given the distances to the Sun and the Moon, recalling that their angular sizes are quite close, it's easy to estimate the size of the Sun.
-<gallery widths=120% heights=100%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
+<gallery widths=500px>File:1_MoonPhasesSolution3.JPG|</gallery></p>
    </div>
 </div></div>

@@ Line 65: / Line 65: @@
 	=\frac{1}{\pi}\frac{T}{\tau},\]
 here $\tau=1~h$ and $T$ is the period of Moon revolution around the Earth, which equals to one month. Calculating, we set $r_{\odot}\sim1.50\cdot 10^{8}~km$, which is correct by the order of magnitude. The error is caused by not exact circularity of the Moon's orbit (the distance to the Moon is $405\cdot 10^3~km$ in apogee and $363\cdot10^3~km$ in perigee). Given the distances to the Sun and the Moon, recalling that their angular sizes are quite close, it's easy to estimate the size of the Sun.
-<gallery widths=100%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
+<gallery widths=120% heights=100%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
    </div>
 </div></div>

@@ Line 65: / Line 65: @@
 	=\frac{1}{\pi}\frac{T}{\tau},\]
 here $\tau=1~h$ and $T$ is the period of Moon revolution around the Earth, which equals to one month. Calculating, we set $r_{\odot}\sim1.50\cdot 10^{8}~km$, which is correct by the order of magnitude. The error is caused by not exact circularity of the Moon's orbit (the distance to the Moon is $405\cdot 10^3~km$ in apogee and $363\cdot10^3~km$ in perigee). Given the distances to the Sun and the Moon, recalling that their angular sizes are quite close, it's easy to estimate the size of the Sun.
-<gallery widths=100% height=45%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
+<gallery widths=100%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
    </div>
 </div></div>

@@ Line 65: / Line 65: @@
 	=\frac{1}{\pi}\frac{T}{\tau},\]
 here $\tau=1~h$ and $T$ is the period of Moon revolution around the Earth, which equals to one month. Calculating, we set $r_{\odot}\sim1.50\cdot 10^{8}~km$, which is correct by the order of magnitude. The error is caused by not exact circularity of the Moon's orbit (the distance to the Moon is $405\cdot 10^3~km$ in apogee and $363\cdot10^3~km$ in perigee). Given the distances to the Sun and the Moon, recalling that their angular sizes are quite close, it's easy to estimate the size of the Sun.
-<gallery widths=85% height=45%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
+<gallery widths=100% height=45%>File:1_MoonPhasesSolution3.JPG|</gallery></p>
    </div>
 </div></div>

@@ Line 176: / Line 176: @@
 === Problem 12: getting rid of $c$ ===
 One of the creators of the Theory of Relativity, Henry Poincare, when speaking in 1904 (!) of the fact that the speed of light $c$ enters all the equations of electromagnetism, compared the situation with the Ptolemy's geocentric theory of epicycles, in which the Earth's year enters all the relations for the relative motion of celestial bodies. Poincare expressed hope that a future Copernicus would rid electrodynamics of $c$. Recall other examples of blunders of geniuses.
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+<!--<div class="NavFrame collapsed">
    <div class="NavHead">solution</div>
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      <p style="text-align: left;"></p>
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