Edwin P. Hubble 1889-1953 Discover other galaxies in 1923 Discovery the expansion of the Universe in 1929 Observation support for the Big Bang Theory The 100-inch (2.5 m) Hooker telescope at Mount Wilson Observatory that Hubble used to measure galaxy distances and a value for the rate of expansion of the universe. Mount Wilson Observatory in California
Henrietta Swan Leavitt 1868-1921 Discover the period- luminosity relationship of Cepheid variable stars in 1912 magellanic clouds
H = 500 km/s/Mpc T = 1/H = 20 億年 ? 1 pc = 3.26 ly
http://ned.ipac.caltech.edu/level5/Tyson/Tyson2.html The factor H0, now called the Hubble constant, is the expansion rate at the present epoch. Hubble's measurements of H0 began at 550 km s-1 Mpc-1; a number of systematic errors were identified, and by the 1960s H0 had dropped to 100 km s-1 Mpc-1. Over the last two decades controversy surrounded H0, with measurements clustered around 50 km s-1 Mpc-1 and 90 km s-1 Mpc-1. There is now a general consensus that H0 = 70.8 (km/s)/Mpc. The inverse of the Hubble constant - the Hubble time - sets a timescale for the age of the Universe: 1/H0 = 13.8 Gyr.
Big Bang Theory In 1927, Georges Lemaître, a Belgian physicist and Roman Catholic priest, proposed that the inferred recession of the nebulae was due to the expansion of the Universe. In 1931 Lemaître suggested that the evident expansion of the universe, if projected back in time, meant that the further in the past the smaller the universe was, until at some finite time in the past all the mass of the Universe was concentrated into a single point, a "primeval atom" where and when the fabric of time and space came into existence. Lemaître's Big Bang theory was advocated and developed by George Gamow, who introduced big bang nucleosynthesis (BBN) and whose associates, Ralph Alpher and Robert Herman, predicted the cosmic microwave background radiation (CMB).
The cosmic microwave background (CMB) radiation is an emission of uniform, black body thermal energy coming from all parts of the sky. The radiation is isotropic to roughly one part in 100,000. As the universe expanded, adiabatic cooling caused the plasma to lose energy until it became favorable for electrons to combine with protons, forming hydrogen atoms. This recombination event happened when the temperature was around 3000 K or when the universe was approximately 379,000 years old. At this point, the photons no longer interacted with the now electrically neutral atoms and began to travel freely through space, resulting in the decoupling of matter and radiation.The color temperature of the decoupled photons has continued to diminish ever since; now down to 2.725 K, their temperature will continue to drop as the universe expands. Cosmic Microwave Background too smooth?
WMAP data reveals that its contents include 4.6% atoms, the building blocks of stars and planets. Dark matter comprises 23% of the universe. This matter, different from atoms, does not emit or absorb light. It has only been detected indirectly by its gravity. 72% of the universe, is composed of "dark energy", that acts as a sort of an anti-gravity. This energy, distinct from dark matter, is responsible for the present-day acceleration of the universal expansion. WMAP data is accurate to two digits, so the total of these numbers is not 100%. This reflects the current limits of WMAP's ability to define Dark Matter and Dark Energy. 14
Inflation is the theorized extremely rapid exponential expansion of the early universe by a factor of at least 10 78 in volume, driven by a negative-pressure vacuum energy density. The inflationary epoch comprises the first part of the electroweak epoch following the grand unification epoch. It lasted from 10 −36 seconds after the Big Bang to sometime between 10 −33 and 10 −32 seconds. Following the inflationary period, the universe continues to expand. The inflationary hypothesis was originally proposed in 1980 by American physicist Alan Guth in 1980. Inflation Theory
在大爆炸後約三分鐘，質子與中子開 始可以結合而成重氫的原子核而不立 刻被光子所分解。接下來一連串的核 反應將絕大部分的重氫很快的轉變成 包含二個質子及二個中子的穩定氦 (He) 原子核。然而，比氦更重的原子 核此時不易形成因為自然定律中不容 許有原子量為五或八的穩定原子核存 在；而缺乏這些作為橋樑的原子核， 更重的原子核不易快速的被製造出來， 而宇宙仍持續的膨脹、冷卻。在大約 宇宙生成 30 分鐘後，大爆炸所產生的 核反應完全停止進行。此時，宇宙中 的物質以質量而言約含 75% 的質子、 25% 的氦原子核、大量很輕的電子、 以及非常微量的重氫及鋰原子核。 Big Bang Nucleosynthesis Where did all the atoms come from?
此時的宇宙溫度仍然非常高 (10 8 K 左右 ) ，強大的輻射線 使電子無法停留在固定的原子 核上，物質主要以單原子離子 狀態存在。由於自由運動的電 子很容易散射光線，此時宇宙 是處於名符其實的混沌狀態； 光子無法自由穿越，輻射場與 物質間不斷的進行能量交換。 這種情況一直持續到了大約四 十萬年後，當宇宙的溫度降到 了約一萬度以下，電子才開始 能與原子核結合型成中性的原 子，宇宙也在此時變成透明， 輻射場與物質間的作用大幅降 低，而重力的作用正開始逐漸 朔造新的宇宙結構。 Formation of atoms and the last scattering
Simulated image of the first stars, 400 million years after the Big Bang. First Stars Formed 200-400 million years after Big Bang Mass: 100-300 solar mass Lifetime = a few million years Became Black holes, Supernovaes
Proton-Proton (PP) Chain in the Sun Inside the Sun, about 655 million tons of hydrogen are converted into 650 million tons of helium every second. In stars heavier than about 2 solar masses, in which the core temperature is more than about 18 million K, the dominant process in which energy is produced by the fusion of hydrogen into helium is a different reaction chain known as the carbon-nitrogen cycle. T > 10 Million K
The CNO Cycle The carbon-nitrogen-oxygen cycle, a cycle of six consecutive nuclear reactions resulting in the formation of a helium nucleus from four protons. The carbon nuclei with which the cycle starts are effectively reformed at the end and therefore act as a catalyst. This is believed to be the predominant energy- producing mechanism in stars with a core temperature exceeding about 18 million K.
When the star starts to run out of hydrogen to fuse, the core of the star begins to collapse until the central temperature rises to ~100×10 6 K. At this point helium nuclei are fusing together at a rate high enough to rival the rate at which their product, beryllium-8, decays back into two helium nuclei. This means that there are always a few beryllium-8 nuclei in the core, which can fuse with yet another helium nucleus to form carbon-12, which is stable Ordinarily, the probability of the triple alpha process would be extremely small. However, the beryllium-8 ground state has almost exactly the energy of two alpha particles. In the second step, 8 Be + 4 He has almost exactly the energy of an excited state of 12 C. These resonances greatly increase the probability that an incoming alpha particle will combine with beryllium-8 to form carbon. The existence of this resonance was predicted by Fred Hoyle before its actual observation, based on the physical necessity for it to exist, in order for carbon to be formed in star. The triple alpha process 4 He + 12 C 16 O ( process)
Carbon Burning Oxygen Burning The carbon-burning process is a set of nuclear fusion reactions that take place in massive stars (at least 8 solar mass at birth) that have used up the lighter elements in their cores. It requires high temperatures (> 5×10 8 K ) and densities (> 3×10 9 kg/m 3 ) The oxygen-burning process is a set of nuclear fusion reactions that take place in massive stars that have used up the lighter elements in their cores. It occurs at temperatures around 1.5×10 9 K and densities of 10 10 kg/m3.
After high-mass stars have nothing but sulfur and silicon in their cores, they further contract until their cores reach temperatures in the range of 2.7–3.5 GK; silicon burning starts at this point. Silicon burning entails the alpha process which creates new elements by adding the equivalent of one helium nucleus (two protons plus two neutrons) per step in the following sequence: (to Fe and Ni) Silicon Burning to Iron
ReactionTimescale Hydrogen burning10 million years Helium burning1 million years Carbon burning300 years Oxygen burning200 days Silicon burning2 days Less and less energy is produced per nuclear reaction in the nucleosynthesis of these high mass elements. So each burning phase lasts a shorter and shorter amount of time. For a star with 15 solar mass:
R-process The r-process is a nucleosynthesis process, likely occurring in core-collapse supernovae (see also supernova nucleosynthesis) responsible for the creation of approximately half of the neutron-rich atomic nuclei that are heavier than iron. The process entails a succession of rapid neutron captures (hence the name r-process) on seed nuclei, typically Ni-56.
A neutron star is a type of stellar remnant that can result from the gravitational collapse of a massive star during a Type II supernova event. Such stars are composed almost entirely of neutrons. A typical neutron star has a mass between 1.35 and about 2.0 solar masses, with a corresponding radius of about 12 km In general, compact stars of less than 1.44 solar masses – the Chandrasekhar limit – are white dwarfs, and above 2 to 3 solar masses, a quark star might be created; Gravitational collapse will usually occur on any compact star between 10 and 25 solar masses and produce a black hole. Neutron Stars D = 5×10 17 kg/m 3 = 5×10 8 ton/cm 3
Circumstellar rings around SN 1987A, with the ejecta from the supernova explosion at the center of the inner ring
If the mass of the remnant exceeds about 3–4 solar masses (the Tolman–Oppenheimer– Volkoff limit)—either because the original star was very heavy or because the remnant collected additional mass through accretion of matter—even the degeneracy pressure of neutrons is insufficient to stop the collapse. No known mechanism (except possibly quark degeneracy pressure, see quark star) is powerful enough to stop the implosion and the object will inevitably collapse to form a black hole. Black Hole escape velocity > speed of light
A supermassive black hole is the largest type of black hole in a galaxy, on the order of hundreds of thousands to billions of solar masses. Most, and possibly all galaxies, including the Milky Way, are believed to contain supermassive black holes at their centers. Supermassive Black Hole