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在首次探测到时空涟漪(引力波)近10年后,物理学家宣布捕获了迄今为止最强的引力波信号,源自遥远星系中2个黑洞的螺旋合并,这让研究人员能够以全新方式验证Albert Einstein的引力理论(广义相对论)。据《Physical Review Letters》报道,对该事件的分析证实了Stephen Hawking提出的定理:黑洞的表面积只会增加,不会减少。

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在首次探测到时空涟漪(引力波)近10年后,物理学家宣布捕获了迄今为止最强的引力波信号,源自遥远星系中2个黑洞的螺旋合并,这让研究人员能够以全新方式验证Albert Einstein的引力理论(广义相对论)。据《Physical Review Letters》报道,对该事件的分析证实了Stephen Hawking提出的定理:黑洞的表面积只会增加,不会减少。

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(图片来源:《Science》)

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(图片来源:《Science》)

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在首次探测到时空涟漪(引力波)近10年后,物理学家宣布捕获了迄今为止最强的引力波信号,源自遥远星系中2个黑洞的螺旋合并,这让研究人员能够以全新方式验证Albert Einstein的引力理论(广义相对论)。据《Physical Review Letters》报道,对该事件的分析证实了Stephen Hawking提出的定理:黑洞的表面积只会增加,不会减少。

在首次探测到时空涟漪(引力波)近10年后,物理学家宣布捕获了迄今为止最强的引力波信号,源自遥远星系中2个黑洞的螺旋合并,这让研究人员能够以全新方式验证Albert Einstein的引力理论(广义相对论)。据《Physical Review Letters》报道,对该事件的分析证实了Stephen Hawking提出的定理:黑洞的表面积只会增加,不会减少。

Cho Adrian. 最强黑洞碰撞验证广义相对论. 科技导报, 2025 , 43 (18) : 13 -14 .
Cho Adrian. Science & Technology Review, 2025 , 43 (18) : 13 -14 .
黑洞合并引力波中的“泛音”与广义相对论预测相符
在首次探测到时空涟漪(引力波)近10年后,物理学家宣布捕获了迄今为止最强的引力波信号,源自遥远星系中2个黑洞的螺旋合并,这让研究人员能够以全新方式验证Albert Einstein的引力理论(广义相对论)。据《Physical Review Letters》报道,对该事件的分析证实了Stephen Hawking提出的定理:黑洞的表面积只会增加,不会减少。
佛罗里达大学引力理论学家Clifford Will评价:“这是广义相对论中一个基础而纯粹的定理,见证它被验证实在令人振奋。现在可以确信,我们观测的正是黑洞。”
2025年1月14日,美国激光干涉引力波天文台(LIGO)探测到了这个信号。该天文台由分别位于路易斯安那州和华盛顿州的2个L型干涉仪组成,通过激光在4 km长臂中共振来探测引力波,其臂长变化小于质子宽度的1/100。通过对比信号与模型,研究人员确定这是由质量分别为太阳33.6倍和32.2倍的2个遥远黑洞螺旋合并产生的。
虽然这2个黑洞的质量与2015年9月14日该天文台首次探测事件中黑洞的质量近乎相同,但经过后续技术升级,探测器的灵敏度已提升3倍。新信号的信噪比高达80,呈现出前所未有的清晰度,使研究人员能够以突破性的精度进行分析。
合并后,最终黑洞的视界(光都无法逃逸的强引力边界)会像被敲击的钟体般发生短暂震荡。本次观测到的“铃荡”频率达到每秒247次,持续约10 ms。主震荡会伴随泛音(通常频率稍低且衰减更快),这些泛音是检验广义相对论的关键要素。
理论上,除了质量和角动量这2个参数,黑洞几乎没有其他特征,这意味着泛音的频率和衰减速率并非独立存在,必然存在数学关联。通过对比泛音与主铃荡音,物理学家得以验证广义相对论的预测。
观测的真正难点在于捕捉泛音,因为其衰减时间可能短于单个震荡周期。麻省理工学院理论物理学家Scott Hughes形象地阐述道:“比起铃铛鸣响,它更像闷雷轰响。”尽管其他黑洞合并事件也曾提及泛音存在(包括该天文台首次探测事件),但加州理工学院物理学家、激光干涉引力波天文台成员Katerina Chatziioannou指出:“本次观测到的泛音清晰明确,是决定性证据。”最终数据表明,主震频率与泛音频率的分布模式完全符合广义相对论的理论预测。
需要说明的是,激光干涉引力波天文台借助基于广义相对论建立的模拟来识别信号特征,这可能导致偏差。为消除其影响,研究人员摒弃了大部分信号,仅分析铃荡阶段。Flatiron研究所、激光干涉引力波天文台物理学家Maximiliano Isi强调:“信号强度是实现这一切的基础。”不过普林斯顿大学引力理论学家Frans Pretorius认为,分析过程中可能仍存在某些固有偏差。
激光干涉引力波天文台研究人员通过黑洞最终的质量和角动量计算出其视界面积约为40万km2。结合2个黑洞合并前的数据,他们发现尽管最终黑洞质量小于初始双黑洞质量之和(部分质量以引力波形式耗散),但其视界面积大于初始双黑洞面积之和,这符合霍金面积定理的数学预测:无论黑洞的质量与角动量如何演化,其视界面积永远不会减小。
这项研究表明,随着激光干涉引力波天文台灵敏度提升,黑洞已成为实证研究的对象。Hughes评价道:“量变引发了质变。”Pretorius指出,随着进一步提升该天文台性能或建设新观测台,科学家将探测到更多震荡模式与泛音,“或许我们会发现广义相对论的不足,并通过高精度测量观测到异常现象。”
当然,这一切取决于激光干涉引力波天文台能否实现性能提升。2025年6月,美国白宫提议关闭该天文台的一个观测站,作为削减国家科学基金会57%预算计划的一部分。这将急剧降低该天文台的探测灵敏度,倾听“黑洞之声”的愿景也会随之黯淡。
(译自《Science》,2025,389(6763))

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  • 首发时间:2025-12-18
  • 出版时间:2025-09-28
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2种不同金属材料的力学参数

Family
属数
Number of
genus
种数
Number of
species
占总种数比例
Percentage of
total species (%)

Genus
种数
Number of
species
占总种数比例
Percentage of total
species (%)
鹅膏菌科Amanitaceae 2 11 5.26 鹅膏菌属 Amanita 10 4.78
小菇科 Mycenaceae 2 12 5.74 丝盖伞属 Inocybe 5 2.39
多孔菌科 Polyporaceae 8 14 6.70 蜡蘑属 Laccaria 5 2.39
红菇科 Russulaceae 3 23 11.00 小皮伞属 Marasmius 6 2.87
小菇属 Mycena 11 5.26
光柄菇属 Pluteus 5 2.39
红菇属 Russula 17 8.13
栓菌属 Trametes 5 2.39
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