宇宙微波背景的B模偏振是什么？
What is the B-mode polarization of the CMB?
B模是CMB偏振的一种卷曲图案，原初引力波会在其上留下印记；探测它是验证暴胀的关键，目前只有上限、尚未确证。
B-modes are a curling pattern in CMB polarization where primordial gravitational waves would leave an imprint; detecting them is key to proving inflation, but so far only upper limits exist.
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)
#B模 #暴胀 #原初引力波
宇宙中失踪的重子指的是什么？
What are the universe's missing baryons?
宇宙中普通物质（重子）的总量可由大爆炸核合成和微波背景精确推知，但把恒星、星系内气体等发光物质加总，只找到约预期的 10%，其余“失踪的重子”被认为以稀薄、温热的气体（温介质 WHIM）形式弥漫在星系际和宇宙网纤维中。这些气体温度约 10^5–10^7 K、密度极低，难以探测；近年通过 X 射线和类星体吸收线观测已证认出其中相当部分。
The total amount of ordinary (baryonic) matter is precisely known from Big Bang nucleosynthesis and the CMB, yet summing stars and visible gas in galaxies accounts for only about 10% of it. The missing baryons are thought to reside as a thin, warm-hot gas (the WHIM) pervading intergalactic space and cosmic-web filaments—at 10^5–10^7 K and so low in density that it is hard to see. Recent X-ray and quasar-absorption-line observations have now accounted for a substantial fraction of them.
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)
#重子 #宇宙网 #未解之谜
什么是σ8张力？
What is the σ8 tension?
σ8描述宇宙中物质成团的程度；CMB预测的成团性强于今日星系巡天实测，这一“结构增长”差异与H0张力同为现代宇宙学难题。
σ8 measures how clumpy matter is; the CMB predicts more clustering than today's galaxy surveys observe—this 'structure growth' mismatch joins the H0 tension as a modern cosmological puzzle.
难度 进阶 · 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)
#σ8 #结构增长 #宇宙学张力
为什么说星系并不是均匀分布的，而是织成一张宇宙网？
Why are galaxies said to form a cosmic web rather than being evenly spread?
引力让暗物质和普通物质聚集成纤维状的墙、节点和空洞，星系沿这些纤维分布，整体像一张巨大的三维网，这是宇宙大尺度结构的标志。
Gravity gathers dark and ordinary matter into filamentary walls, nodes, and voids, with galaxies strung along the filaments like a vast 3D web—the signature of cosmic large-scale structure.
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)
#宇宙网 #大尺度结构 #暗物质
什么是哈勃常数争议（H0张力）？
What is the Hubble constant tension (H0 tension)?
用宇宙微波背景（普朗克）推算的膨胀率约67 km/s/Mpc，而用局部距离阶梯（造父+Ia）测得约73，两者差异超出误差，暗示可能有新物理。
The expansion rate inferred from the CMB (Planck) is about 67 km/s/Mpc, while the local distance ladder (Cepheids + Ia) gives about 73; the gap exceeds errors and may hint at new physics.
难度 进阶 · 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)
#哈勃常数 #张力 #距离阶梯
暗能量是宇宙常数还是演化的？
Is dark energy a cosmological constant or evolving?
当前数据基本兼容爱因斯坦的宇宙常数Λ，但也可能暗能量密度随时间变化（w不等于-1）；DESI等巡天正用重子声学振荡检验其是否“演化”。
Data mostly fit Einstein's cosmological constant Λ, but dark energy could evolve in density (w≠-1); surveys like DESI use baryon acoustic oscillations to test whether it changes with time.
难度 进阶 · 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)
#暗能量 #w参数 #宇宙常数
宇宙的大尺度结构是如何随时间成长的？
How did the universe's large-scale structure grow over time?
极早期微小的密度涨落在引力下被放大，暗物质先成晕、再吸引普通物质形成星系和纤维，最终织成今天的宇宙网，这一过程可由模拟与观测对照检验。
Tiny early density ripples were amplified by gravity; dark matter formed halos first, then drew in ordinary matter to build galaxies and filaments into today's web—a process tested by comparing simulations with observations.
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)
#大尺度结构 #引力 #宇宙网
什么是“早期暗能量”（EDE）？
What is early dark energy (EDE)?
早期暗能量假说认为宇宙极早期曾存在一段额外的暗能量，加速膨胀以解决H0和σ8张力，是近年热门但尚无定论的修正方案。
Early dark energy hypothesizes an extra episode of dark energy in the very early Universe that briefly sped expansion, proposed to ease the H0 and σ8 tensions—popular but unproven.
难度 进阶 · 适合 高中(15-18)
CC BY 4.0 · 已核验 · Verified 2026-11-04结论有争议 · Contested
来源 · Source
Gómez-Valent, Zheng, Amendola, Pettorino,《Early and not so early dark energy. What do cosmological observations tell us about them?》,The Sixteenth Marcel Grossmann Meeting,2023 (DOI: 10.1142/9789811269776_0135)
Gómez-Valent, Zheng, Amendola, Pettorino, 'Early and not so early dark energy. What do cosmological observations tell us about them?', The Sixteenth Marcel Grossmann Meeting, 2023, DOI: 10.1142/9789811269776_0135
独立核验依据 · Independent verification: 核验依据 1 Crossref DOI 10.1142/9789811269776_0135
#早期暗能量 #H0张力 #新物理
宇宙距离阶梯是怎么搭建的？
How is the cosmic distance ladder built?
由近及远串联多把“尺子”：视差测近星、造父变星标定邻近星系、Ia超新星推到遥远宇宙，每层校准下一层以测哈勃常数。
It chains 'rulers' from near to far: parallax for nearby stars, Cepheid variables to calibrate neighbor galaxies, Ia supernovae out to the distant Universe—each calibrating the next to measure the Hubble constant.
难度 入门 · 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)
#距离阶梯 #造父变星 #校准