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--- courses:ast100:3 [2026/02/24 06:37] – asad
+++ courses:ast100:3 [2026/02/24 08:21] (current) – [3. Stars and humans: birth and death] asad
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 ===== - Event details =====
+Following the emergence of the spherical Galactic halo, the Milky Way's rotating gas and dust gradually flattened into a thin disk. While older, metal-poor Population II stars maintained random orbits in the ancient halo, the new disk became the primary site of star formation. This flattening coincided with the birth of metal-rich Population I stars, formed from interstellar material enriched by earlier generations. These younger stars inherited the disk's spin, moving in highly ordered, circular orbits around the Galactic center.
-===== - Stars and humans: birth and death =====
+Roughly 10 billion years ago, the universe reached its peak rate of star formation as galaxies rapidly consumed their abundant gas. During this epoch, countless massive stars acted as nuclear forges, fusing primordial hydrogen and helium into heavier elements. Within their dense cores, they synthesized vital building blocks like carbon, oxygen, neon, and iron. Their rapid lifecycles and deaths continuously seeded the cosmos with the chemical ingredients necessary for future planetary systems.
+Around 8 billion years ago, a "galactic habitable zone" emerged in the Milky Way, offering ideal conditions for complex life. Located between the radiation-intense inner bulge and the barren outer edges, this annular region possessed a crucial balance. Stellar nucleosynthesis had spread sufficient heavy elements here to form terrestrial planets, while the frequency of sterilizing supernovae—common in the inner galaxy—had decreased enough to ensure a stable environment.
+Stellar nucleosynthesis (to be detailed in the Chemical Age) is the process by which stars forge the chemical complexity required for planets and life. Throughout their main-sequence lifetimes, stars maintain hydrostatic equilibrium by stably fusing hydrogen into helium. As massive stars exhaust their core hydrogen, they contract, heat up, and initiate successive fusion stages. They develop an onion-like layered structure, sequentially fusing elements like helium, carbon, neon, oxygen, and silicon, until a highly stable iron core accumulates at the center.
+Because fusing iron yields no energy, these massive cores inevitably collapse under their own gravity, triggering Type II supernovae. During these catastrophic explosions, temperatures soar to billions of degrees, allowing rapid neutron capture (the r-process) to synthesize elements heavier than iron, such as gold, silver, and uranium. The blasts scatter this enriched material into the interstellar medium, fertilizing galactic clouds with the stardust essential for forming rocky planets.
+Although gravity initially slowed cosmic expansion, a fundamental transition occurred roughly 7 billion years after the Big Bang. The universe's expansion began to accelerate due to the repulsive push of a mysterious force known as 'dark energy'. As the universe expanded and matter density diluted, dark energy eventually overpowered gravity on the largest scales. This shift marked the end of the matter-dominated era and the beginning of the dark-energy-dominated era, profoundly influencing the evolution of large-scale cosmic structures.
+For our local cosmic neighborhood, the Stellar Age culminated 4.6 billion years ago when a chemically enriched interstellar cloud collapsed under its own gravity. Likely triggered by a nearby supernova shock wave, this solar nebula shrank, spun, and flattened into a rotating protoplanetary disk. As material plunged inward, the center grew hot and dense enough to ignite nuclear fusion, birthing our Sun. Meanwhile, the surrounding disk debris accreted to form the planets of our Solar System.
+===== - Stars and humans: birth and death =====
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+This 2014 Madau & Dickinson diagram illustrates the cosmic history of star formation and black hole growth. The plot utilizes a dual x-axis: the bottom tracks cosmological redshift from 0 to 6, while the top shows corresponding lookback time from 0 to 12 billion years (Gyr). The logarithmic y-axis measures activity density in Solar masses per year per cubic Gigalight-year. Two primary trends are plotted: a thick black line for the Star Formation Rate (SFR) and a red line for the Black Hole Accretion Rate (BHAR). Surrounding shaded regions indicate observational data uncertainties.
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+The graph's defining feature is the strongly correlated trajectory of both curves, highlighting a synchronized cosmic evolution. Moving from the early universe toward the present, both the SFR and BHAR rise steeply to a dramatic, shared peak around a redshift of 2. This maximum activity phase, occurring roughly 10 billion years ago, represents the era known as "Cosmic Noon." Following this incredibly fertile epoch of cosmic birth, both rates undergo a steady, parallel decline toward the present day. This synchronization demonstrates that the fundamental gas reservoirs fueling stellar nurseries simultaneously drove the massive growth of central black holes.
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+We can draw a striking allegory between this cosmic timeline and human demographic evolution (shown above), specifically the inverse relationship between human fertility and life expectancy. Just as global demographic charts reveal that societies with the highest birth rates paradoxically experience the lowest life expectancies, the universe displays a similarly intertwined fate of creation and consumption. During "Cosmic Noon," the cosmos was in its own demographic extreme—fervently birthing stars at an unprecedented rate, yet simultaneously feeding the dark, consumptive engines of supermassive black holes. For both mortals and milky ways, explosive, prolific birth is inextricably bound to aggressive consumption and accelerated mortality. As these systems mature—whether a human civilization transitioning to smaller families and longer lives, or our universe settling into a less fertile epoch—the frantic pace of creation wanes, trading the volatile fires of youth for a cooler, more enduring stillness.