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2016年IOAA理论第3题-早期宇宙 - 版本历史
2026-04-29T18:23:57Z
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2019年9月12日 (四) 16:08 Sqr.pi
2019-09-12T16:08:34Z
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<td colspan="2" style="background-color: #fff; color: #222; text-align: center;">2019年9月12日 (四) 16:08的版本</td>
</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l30" >第30行：</td>
<td colspan="2" class="diff-lineno">第30行：</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(in eV), of the radiation as emitted at redshift 𝑧<sub>e</sub></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(in eV), of the radiation as emitted at redshift 𝑧<sub>e</sub></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>.</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">==中文翻译==</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">'''(T3)早期宇宙'''</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">宇宙学模型表明，宇宙中的辐射能量密度$$\rho_r$$与$$(1+z)^4$$成正比，物质能量密度$$\rho_m$$与$$(1+z)^3$$成正比，其中$$z$$是红移。无量纲密度常数$$\Omega $$定义为$$\Omega = \rho /\rho_c$$，其中$$\rho_c$$是宇宙的临界能量密度。在当前宇宙中，与辐射和物质相对应的密度参数分别为$$\Omega_{r0}=10^{-4}$$和$$\Omega_{m0}=0.3$$。</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">(T3.1) 计算在辐射和物质能量密度相等时的红移$$z_e$$。</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">(T3.2) 假设来自早期宇宙的辐射是温度的黑体光谱温度为$$2.732\rm{K}$$，估计红移$$z_e$$处的辐射温度$$T_e$$。</ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">(T3.3) 估计红移为$$z_e$$时的典型光子能量$$E_v$$（单位为$$\rm{eV}$$）。</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[分类:宇宙学]]</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[分类:宇宙学]]</div></td></tr>
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2019年9月11日 (三) 09:45 Quan787
2019-09-11T09:45:05Z
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<td colspan="2" class="diff-lineno">第1行：</td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">{{需要解答}}</ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==英文原题==</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>==英文原题==</div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''(T3) Early Universe'''</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>'''(T3) Early Universe'''</div></td></tr>
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Quan787
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2019年9月11日 (三) 09:27 Quan787
2019-09-11T09:27:12Z
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</tr><tr><td colspan="2" class="diff-lineno" id="mw-diff-left-l25" >第25行：</td>
<td colspan="2" class="diff-lineno">第25行：</td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>, of the radiation at redshift 𝑧<sub>e</sub></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>, of the radiation at redshift 𝑧<sub>e</sub></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>.</div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>.</div></td></tr>
<tr><td colspan="2"> </td><td class='diff-marker'>+</td><td style="color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"></ins></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(T3.3) Estimate the typical photon energy, 𝐸<sub>ν</sub></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(T3.3) Estimate the typical photon energy, 𝐸<sub>ν</sub></div></td></tr>
<tr><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(in eV), of the radiation as emitted at redshift 𝑧<sub>e</sub></div></td><td class='diff-marker'> </td><td style="background-color: #f8f9fa; color: #222; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>(in eV), of the radiation as emitted at redshift 𝑧<sub>e</sub></div></td></tr>
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Quan787
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Quan787：创建页面，内容为“==英文原题== '''(T3) Early Universe''' Cosmological models indicate that radiation energy density, 𝜌<sub>r</sub> , in the Universe is proportional to (1 +…”
2019-09-11T09:26:48Z
<p>创建页面，内容为“==英文原题== '''(T3) Early Universe''' Cosmological models indicate that radiation energy density, 𝜌<sub>r</sub> , in the Universe is proportional to (1 +…”</p>
<p><b>新页面</b></p><div>==英文原题==<br />
'''(T3) Early Universe'''<br />
<br />
Cosmological models indicate that radiation energy density, 𝜌<sub>r</sub><br />
, in the Universe is proportional to<br />
(1 + 𝑧)<br />
<sup>4</sup><br />
, and the matter energy density, 𝜌<sub>m</sub>, is proportional to (1 + 𝑧)<br />
<sup>3</sup><br />
, where 𝑧 is the redshift. The<br />
dimensionless density parameter, Ω, is given as Ω = 𝜌/𝜌<sub>c</sub><br />
, where 𝜌<sub>c</sub><br />
is the critical energy density of the<br />
Universe. In the present Universe, the density parameters corresponding to radiation and matter, are<br />
Ω<sub>r<sub>0</sub></sub><br />
= 10<sup>−4</sup><br />
and Ω<sub>m<sub>0</sub></sub><br />
= 0.3, respectively.<br />
<br />
(T3.1) Calculate the redshift, 𝑧e<br />
, at which radiation and matter energy densities were equal.<br />
<br />
(T3.2) Assuming that the radiation from the early Universe has a blackbody spectrum with a<br />
temperature of 2.732 K, estimate the temperature, 𝑇<sub>e</sub><br />
, of the radiation at redshift 𝑧<sub>e</sub><br />
.<br />
(T3.3) Estimate the typical photon energy, 𝐸<sub>ν</sub><br />
(in eV), of the radiation as emitted at redshift 𝑧<sub>e</sub><br />
.<br />
<br />
[[分类:宇宙学]]</div>
Quan787