http://202.127.29.3/~shen/wiki/index.php?action=history&feed=atom&title=%E6%AF%AB%E7%A7%92%E8%84%89%E5%86%B2%E6%98%9F 2026-04-18T02:48:00Z 本wiki上该页面的版本历史 MediaWiki 1.38.1 http://202.127.29.3/~shen/wiki/index.php?title=%E6%AF%AB%E7%A7%92%E8%84%89%E5%86%B2%E6%98%9F&diff=2833&oldid=prev 2018-04-09T12:44:30Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="zh-Hans-CN"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">←上一版本</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">2018年4月9日 (一) 12:44的版本</td> </tr><tr> <td colspan="2" class="diff-lineno">第3行：</td> <td colspan="2" class="diff-lineno">第3行：</td> </tr> <tr> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*第一颗毫秒脉冲星是1982年发现的</div></td> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*第一颗毫秒脉冲星是1982年发现的</div></td> </tr> <tr> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*截止2018年，已经观测到超过300颗毫秒脉冲星</div></td> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*截止2018年，已经观测到超过300颗毫秒脉冲星</div></td> </tr> <tr> <td class="diff-marker" data-marker="−"></td> <td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>*相比于普通中子星<del style="font-weight: bold; text-decoration: none;">磁</del>，毫秒脉冲星的磁场较弱。</div></td> <td class="diff-marker" data-marker="+"></td> <td style="color: #202122; 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>*相比于普通中子星，毫秒脉冲星的磁场较弱。</div></td> </tr> </table>

Shen http://202.127.29.3/~shen/wiki/index.php?title=%E6%AF%AB%E7%A7%92%E8%84%89%E5%86%B2%E6%98%9F&diff=2832&oldid=prev 2018-04-09T12:44:18Z

<p></p> <table style="background-color: #fff; color: #202122;" data-mw="interface"> <col class="diff-marker" /> <col class="diff-content" /> <col class="diff-marker" /> <col class="diff-content" /> <tr class="diff-title" lang="zh-Hans-CN"> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">←上一版本</td> <td colspan="2" style="background-color: #fff; color: #202122; text-align: center;">2018年4月9日 (一) 12:44的版本</td> </tr><tr> <td colspan="2" class="diff-lineno">第1行：</td> <td colspan="2" class="diff-lineno">第1行：</td> </tr> <tr> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>一般认为毫秒脉冲星是中子星经历吸积演化后的再生脉冲星，自旋周期一般小于10 ms。</div></td> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>一般认为毫秒脉冲星是中子星经历吸积演化后的再生脉冲星，自旋周期一般小于10 ms。</div></td> </tr> <tr> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*证据：毫秒脉冲星处于银河系核球中，而常规脉冲星分布在银道面附近. </div></td> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*证据：毫秒脉冲星处于银河系核球中，而常规脉冲星分布在银道面附近. </div></td> </tr> <tr> <td class="diff-marker" data-marker="−"></td> <td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>*第一颗毫秒脉冲星<del style="font-weight: bold; text-decoration: none;">PSR B1937+21</del>是<del style="font-weight: bold; text-decoration: none;">由Backer et al. (</del>1982<del style="font-weight: bold; text-decoration: none;">)</del>发现的</div></td> <td class="diff-marker" data-marker="+"></td> <td style="color: #202122; 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>*第一颗毫秒脉冲星是1982<ins style="font-weight: bold; text-decoration: none;">年</ins>发现的</div></td> </tr> <tr> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*截止2018年，已经观测到超过300颗毫秒脉冲星</div></td> <td class="diff-marker"></td> <td style="background-color: #f8f9fa; color: #202122; 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>*截止2018年，已经观测到超过300颗毫秒脉冲星</div></td> </tr> <tr> <td class="diff-marker" data-marker="−"></td> <td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>*相比于普通中子星磁<del style="font-weight: bold; text-decoration: none;">G，</del>毫秒脉冲星的磁场较弱。</div></td> <td class="diff-marker" data-marker="+"></td> <td style="color: #202122; 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>*相比于普通中子星磁<ins style="font-weight: bold; text-decoration: none;">，</ins>毫秒脉冲星的磁场较弱。</div></td> </tr> <!-- diff cache key wikidb2:diff:wikidiff2:1.12:old-2831:rev-2832:1.14.1 --> </table>

Shen http://202.127.29.3/~shen/wiki/index.php?title=%E6%AF%AB%E7%A7%92%E8%84%89%E5%86%B2%E6%98%9F&diff=2831&oldid=prev 2018-04-09T12:43:44Z

<p>创建页面，内容为“一般认为毫秒脉冲星是中子星经历吸积演化后的再生脉冲星，自旋周期一般小于10 ms。 *证据：毫秒脉冲星处于银河系核球中...”</p> <p><b>新页面</b></p><div>一般认为毫秒脉冲星是中子星经历吸积演化后的再生脉冲星，自旋周期一般小于10 ms。<br /> *证据：毫秒脉冲星处于银河系核球中，而常规脉冲星分布在银道面附近. <br /> *第一颗毫秒脉冲星PSR B1937+21是由Backer et al. (1982)发现的<br /> *截止2018年，已经观测到超过300颗毫秒脉冲星<br /> *相比于普通中子星磁G，毫秒脉冲星的磁场较弱。</div>

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