与 r 过程相对，s 过程指的是什么？
Compared with the r-process, what is the s-process?
s 过程是慢中子俘获过程，发生在像红巨星这样的恒星内部，中子加入速度慢于 β 衰变，逐步生成比铁重但相对稳定的元素，如锶、钡、铅。
The s-process is slow neutron capture occurring inside stars like red giants, where neutrons are added more slowly than beta decay, building heavier stable elements such as strontium, barium, and lead.
难度 专业 · 适合 高中(15-18)
CC BY 4.0 · 已核验 · Verified 2026-08-23 · 2 条独立证据
来源 · Source
Carroll & Ostlie,《An Introduction to Modern Astrophysics》第2版,Cambridge University Press,2017
B. W. Carroll and D. A. Ostlie, An Introduction to Modern Astrophysics, 2nd ed., Cambridge University Press, 2017
独立核验依据 · Independent verification: 核验依据 2 ISBN 978-1-108-42216-1 (2nd ed., Cambridge Univ. Press)
#元素合成 #s过程 #红巨星
宇宙中比铁重的元素（如金、铀）主要在什么过程中产生？
Where in the universe are elements heavier than iron, like gold and uranium, mainly forged?
大部分重元素通过快中子俘获过程（r 过程）在中子星并合或某些超新星中形成，中子被快速俘获后再经 β 衰变变成重核。
Most heavy elements form via the rapid neutron-capture process (r-process) in neutron-star mergers or certain supernovae, where nuclei quickly grab neutrons and later beta-decay into heavy nuclei.
难度 专业 · 适合 高中(15-18)
CC BY 4.0 · 已核验 · Verified 2026-08-23 · 2 条独立证据
来源 · Source
Carroll & Ostlie,《An Introduction to Modern Astrophysics》第2版,Cambridge University Press,2017
B. W. Carroll and D. A. Ostlie, An Introduction to Modern Astrophysics, 2nd ed., Cambridge University Press, 2017
独立核验依据 · Independent verification: 核验依据 2 ISBN 978-1-108-42216-1 (2nd ed., Cambridge Univ. Press)
#元素合成 #r过程 #中子星
我们身体里的重元素来自哪里？
Where do the heavy elements in our bodies come from?
除氢和部分氦外，构成生命的碳、氧、铁等元素都是前代恒星在核聚变与超新星、中子星并合等事件中抛洒到星际空间，再聚集成新恒星和行星的。
Aside from hydrogen and some helium, the carbon, oxygen, and iron in life were forged in earlier stars and scattered by supernovae and neutron-star mergers, later gathering into new stars and planets.
难度 专业 · 适合 高中(15-18)
CC BY 4.0 · 已核验 · Verified 2026-08-23 · 2 条独立证据
来源 · Source
Carroll & Ostlie,《An Introduction to Modern Astrophysics》第2版,Cambridge University Press,2017
B. W. Carroll and D. A. Ostlie, An Introduction to Modern Astrophysics, 2nd ed., Cambridge University Press, 2017
独立核验依据 · Independent verification: 核验依据 2 ISBN 978-1-108-42216-1 (2nd ed., Cambridge Univ. Press)
#元素合成 #恒星 #生命
宇宙大爆炸核合成产生了哪些元素？
Which elements did Big Bang nucleosynthesis produce?
在大爆炸后约三分钟，宇宙冷却到能进行核反应，主要合成了氢、氦以及极少量锂，这一比例与今天观测高度吻合，是宇宙学的有力证据。
About three minutes after the Big Bang, the cooling universe fused mainly hydrogen, helium, and trace lithium; this predicted ratio matches observations and strongly supports cosmology.
难度 进阶 · 适合 大众
CC BY 4.0 · 已核验 · Verified 2026-08-23 · 2 条独立证据
来源 · Source
Carroll & Ostlie,《An Introduction to Modern Astrophysics》第2版,Cambridge University Press,2017
B. W. Carroll and D. A. Ostlie, An Introduction to Modern Astrophysics, 2nd ed., Cambridge University Press, 2017
独立核验依据 · Independent verification: 核验依据 2 ISBN 978-1-108-42216-1 (2nd ed., Cambridge Univ. Press)
#元素合成 #大爆炸 #氦
大质量恒星核坍缩形成超新星后，光变曲线为何在爆发数周后转入一条按约77天半衰期指数衰减的尾部？
After a massive star's core-collapse supernova, why does the light curve settle onto an exponential tail governed by a half-life of about 77 days?
爆发中新合成的镍-56（半衰期约6天）经β+衰变变为钴-56，后者再衰变为稳定铁-56，半衰期约77天。当抛射物膨胀变得光学薄后，这两步衰变释放的伽马射线与正电子成为主要能源，晚期光度因此按钴-56的半衰期指数下降。SN 1987A的测光证实了该机制，也表明铁峰元素确产生于爆发性核燃烧。
Freshly synthesized nickel-56 (half-life about 6 days) beta-decays into cobalt-56, which decays to stable iron-56 with a half-life near 77 days. Once the expanding ejecta turn optically thin, gamma rays and positrons from this chain dominate the energy budget, so the late luminosity fades exponentially on the cobalt-56 half-life. Photometry of SN 1987A confirmed the mechanism and showed that iron-peak elements are truly forged in explosive nuclear burning.
难度 进阶 · 适合 初中(12-15)
CC BY 4.0 · 来源待核验 · Source pending review
来源 · Source
出处备注：著录含书名，但缺版次 / 出版社 / 年份中的一部分，需编辑补全后才能做独立比对。
W. D. Arnett，《天体物理杂志》（ApJ）第253卷第785页，1982年；SN 1987A测光检验。
W. D. Arnett, Astrophysical Journal 253, 785 (1982); tested by SN 1987A photometry.
#镍-56 #钴-56 #放射性衰变 #超新星光变