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微引力透镜

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引力透镜 型式强透镜微透镜弱透镜 强透镜系统 阿贝尔1689阿贝尔2218CL0024+17Bullet ClusterQSO2237+0305SDSSJ0946+1006B1359+154QSO 0957+561 巡天 Strong: CLASSSLACS (SDSS) Micro: OGLE Weak: DLSPan-STARRSCFHTLS . DESLSSTSNAPDESTINY .mw-parser-output .hlist ul,.mw-parser-output .hlist ol{padding-left:0}.mw-parser-output .hlist li,.mw-parser-output .hlist dd,.mw-parser-output .hlist dt{margin:0;display:inline}.mw-parser-output .hlist dt:after,.mw-parser-output .hlist dd:after,.mw-parser-output .hlist li:after{white-space:normal}.mw-parser-output .hlist dt:after{content:" :"}.mw-parser-output .hlist dd:after,.mw-parser-output .hlist li:after{content:" · ";font-weight:bold}.mw-parser-output .hlist-pipe dd:after,.mw-parser-output .hlist-pipe li:after{content:" | ";font-weight:normal}.mw-parser-output .hlist-hyphen dd:after,.mw-parser-output .hlist-hyphen li:after{content:" - ";font-weight:normal}.mw-parser-output .hlist-comma dd:after,.mw-parser-output .hlist-comma li:after{content:"、";font-weight:normal}.mw-parser-output .hlist dd:last-child:after,.mw-parser-output .hlist dt:last-child:after,.mw-parser-output .hlist li:last-child:after{content:none}.mw-parser-output .hlist ol{counter-reset:listitem}.mw-parser-output .hlist ol>li{counter-increment:listitem}.mw-parser-output .hlist ol>li:before{content:" "counter(listitem)" ";white-space:nowrap}.mw-parser-output .hlist dd ol>li:first-child:before,.mw-parser-output .hlist dt ol>li:first-child:before,.mw-parser-output .hlist li ol>li:first-child:before{content:" ("counter(listitem)" "}.mw-parser-output .hlist ol{counter-reset:listitem}.mw-parser-output .hlist ol>li{counter-increment:listitem}.mw-parser-output .hlist ol>li:before{content:" "counter(listitem)"\a0 "}.mw-parser-output .hlist dd ol>li:first-child:before,.mw-parser-output .hlist dt ol>li:first-child:before,.mw-parser-output .hlist li ol>li:first-child:before{content:" ("counter(listitem)"\a0 "}.mw-parser-output ul.cslist,.mw-parser-output ul.sslist{margin:0;padding:0;display:inline-block;list-style:none}.mw-parser-output .cslist li,.mw-parser-output .sslist li{margin:0;display:inline-block}.mw-parser-output .cslist li:after{content:","}.mw-parser-output .sslist li:after{content:";"}.mw-parser-output .cslist li:last-child:after,.mw-parser-output .sslist li:last-child:after{content:none}.mw-parser-output .navbar{display:inline;font-weight:normal}.mw-parser-output .navbar-collapse{float:left;text-align:left}.mw-parser-output .navbar-boxtext{word-spacing:0}.mw-parser-output .navbar ul{display:inline-block;white-space:nowrap;line-height:inherit}.mw-parser-output .navbar-brackets::before{margin-right:-0.125em;content:"[ "}.mw-parser-output .navbar-brackets::after{margin-left:-0.125em;content:" ]"}.mw-parser-output .navbar li{word-spacing:-0.125em}.mw-parser-output .navbar a>span,.mw-parser-output .navbar a>abbr{text-decoration:inherit}.mw-parser-output .navbar-mini abbr{font-variant:small-caps;border-bottom:none;text-decoration:none;cursor:inherit}.mw-parser-output .navbar-ct-full{font-size:114%;margin:0 7em}.mw-parser-output .navbar-ct-mini{font-size:114%;margin:0 4em}
微引力透镜示意图

微引力透镜(英语:Gravitational microlensing)是发生在恒星级天体中的引力透镜现象。与发生在星系尺度上的引力透镜现象相比,微引力透镜的源天体质量很小,光的偏转要小得多,通常情况下难以直接观测到微引力透镜所成的像,而只能观察到光度在瞬间增强的现象。银河系存在相当数量的恒星级黑洞褐矮星红矮星白矮星行星等较暗弱的天体,它们造成的微引力透镜现象能够在短时间内令背景光发生畸变。因此微引力透镜为研究这些天体提供了非常重要的手段。

人们早在20世纪60年代就提出了微引力透镜的概念。20世纪80年代,普林斯顿大学的波兰天文学家玻丹·帕琴斯基Bohdan Paczyński)讨论了银河系晕中不发光的暗天体作为微引力透镜的可能性[1],认为它们有很高的概率被观测到。这些天体叫做大质量致密晕天体。1993年,人们在大麦哲伦云中发现了第一个微引力透镜。

微引力透镜OGLE-2005-BLG-006的光变曲线。红线是用模型拟合的光变曲线。

参见

参考文献

  1. ^ Paczynski, B., 1986, Astrophysical Journal, 304, 1. NASA ADS DOI:10.1086/164140
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微引力透镜
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