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Placing Our Solar System in Context
... - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in initial conditions. - evolution appears to proceed from inside-out as expected. ...
... - disks around lower mass stars are less massive and live longer than their more massive counterparts. - large dispersion in evolutionary times could indicate dispersion in initial conditions. - evolution appears to proceed from inside-out as expected. ...
It all began with a Big Bang!
... The Sun and its planets (including Earth) lie in this quiet part of the galaxy, about half way out from the centre. The Milky Way rotates once every 200 million years. It is made up of at least 100 billion stars, as well as dust and gas. It is so big that light takes 100 000 years to cross from one ...
... The Sun and its planets (including Earth) lie in this quiet part of the galaxy, about half way out from the centre. The Milky Way rotates once every 200 million years. It is made up of at least 100 billion stars, as well as dust and gas. It is so big that light takes 100 000 years to cross from one ...
Chapter 15. The Chandrasekhar Limit, Iron-56 and Core
... pressure and therefore do not have to keep their core temperatures high via nuclear reactions to keep from collapsing. Their pressure depends only on their density, which is already high. They do not have any form of nuclear energy generation and they radiate only their thermal energy, cooling off s ...
... pressure and therefore do not have to keep their core temperatures high via nuclear reactions to keep from collapsing. Their pressure depends only on their density, which is already high. They do not have any form of nuclear energy generation and they radiate only their thermal energy, cooling off s ...
THE HABITABLE ZONE OF EARTH-LIKE PLANETS AROUND 47 UMA
... The main question is, whether Earth-like planets harbouring life can exist around 47 UMa, i.e. planets within the habitable zone (HZ). Typically, stellar HZs are defined as regions near the central star, where the physical conditions are favourable for liquid water to be available at the planet’s su ...
... The main question is, whether Earth-like planets harbouring life can exist around 47 UMa, i.e. planets within the habitable zone (HZ). Typically, stellar HZs are defined as regions near the central star, where the physical conditions are favourable for liquid water to be available at the planet’s su ...
Chapter 14
... ...are stellar remnants for high-mass stars. – i.e. remnant cores with masses greater than 3 solar masses ...
... ...are stellar remnants for high-mass stars. – i.e. remnant cores with masses greater than 3 solar masses ...
Newly discovered Earth-sized planets suitable for life? By Los
... less certain. Current observations suggest its orbital period could range anywhere from four to 73 days. The star is just .05 percent as bright as our sun. Scientists say that it could still give off enough radiation to warm all three planets such that liquid water could exist on their surfaces. The ...
... less certain. Current observations suggest its orbital period could range anywhere from four to 73 days. The star is just .05 percent as bright as our sun. Scientists say that it could still give off enough radiation to warm all three planets such that liquid water could exist on their surfaces. The ...
Document
... • Excellent for deep sky observing or astrophotography with fast films or CCD’s. • Very good for lunar, planetary and binary star observing or ...
... • Excellent for deep sky observing or astrophotography with fast films or CCD’s. • Very good for lunar, planetary and binary star observing or ...
Life Cycle of stars
... By not emitting anymore light, the white dwarf star becomes a black dwarf star. Black dwarf stars usually have temperatures near absolute zero, and have diameters similar to that of terrestrial planets such as Earth and Venus. In this stage, the black dwarf star will remain forever emitting no ligh ...
... By not emitting anymore light, the white dwarf star becomes a black dwarf star. Black dwarf stars usually have temperatures near absolute zero, and have diameters similar to that of terrestrial planets such as Earth and Venus. In this stage, the black dwarf star will remain forever emitting no ligh ...
Stellar Metamorphosis
... amino acid molecules are being produced in the cooling planet as shown by Miller –Urey experiment.. These amino acids will evolve to form some type of selfreplicating molecules (Life) kick-starting the process of life which we still have to fully understand in regards to its mechanism. At some stage ...
... amino acid molecules are being produced in the cooling planet as shown by Miller –Urey experiment.. These amino acids will evolve to form some type of selfreplicating molecules (Life) kick-starting the process of life which we still have to fully understand in regards to its mechanism. At some stage ...
Supernovae
... • Neutrino detection consistent with that expected from SN in LMC in Feb 1987. This was probably type II SN because originator was massive B star (20 solar masses)… although also individual. • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expa ...
... • Neutrino detection consistent with that expected from SN in LMC in Feb 1987. This was probably type II SN because originator was massive B star (20 solar masses)… although also individual. • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expa ...
answers
... random motion that obey the laws of physics for gravity and circular motion. a) How well does it match the solar nebula theory? The masses clump through collisions until there are just a few bodies, they all orbit in the same direction, b) What else do you notice about solar system formation? Most o ...
... random motion that obey the laws of physics for gravity and circular motion. a) How well does it match the solar nebula theory? The masses clump through collisions until there are just a few bodies, they all orbit in the same direction, b) What else do you notice about solar system formation? Most o ...
Astronomy Unit Outline
... investigate and analyse the properties of the universe, particularly the evolution and properties of stars, in both qualitative and quantitative terms; ...
... investigate and analyse the properties of the universe, particularly the evolution and properties of stars, in both qualitative and quantitative terms; ...
Red giants aren`t just big, they`re turbulent
... from interstellar clouds of gas that collapse under the pull of gravity. The extreme temperatures and pressures at the cores of these clouds fuse protons – hydrogen nuclei – into the nuclei of helium, releasing energy (in the form of photons) that slowly works its way to the surface where it escapes ...
... from interstellar clouds of gas that collapse under the pull of gravity. The extreme temperatures and pressures at the cores of these clouds fuse protons – hydrogen nuclei – into the nuclei of helium, releasing energy (in the form of photons) that slowly works its way to the surface where it escapes ...
大爆炸---宇宙的起源
... 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 ev ...
... 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 ev ...
Day-1
... ASTR 2010: Problems in Planetary Astronomy meets Wednesdays at 1600 (E118). It is a onehour class that only meets once a week. We will do some of the problems from the back of the chapters that involve math as well as supplemental problems. The math level is basic algebra. If you are interested, see ...
... ASTR 2010: Problems in Planetary Astronomy meets Wednesdays at 1600 (E118). It is a onehour class that only meets once a week. We will do some of the problems from the back of the chapters that involve math as well as supplemental problems. The math level is basic algebra. If you are interested, see ...
AST 1002
... Demonstrate the correct use of basic astronomical terms and their definitions. Describe the structure and orbital motion of the Earth, and explain why it leads to seasons and changes in the constellations of the night sky. Identify the fundamental types of astronomical telescopes. Describe how time ...
... Demonstrate the correct use of basic astronomical terms and their definitions. Describe the structure and orbital motion of the Earth, and explain why it leads to seasons and changes in the constellations of the night sky. Identify the fundamental types of astronomical telescopes. Describe how time ...
The Great Bear and the Little Bear
... • Stars are balls of hot gas. • They are much larger than planets and much further from Earth. • The sun is the closest star to Earth. • Most of the gas in the inside of a star is hydrogen and its temperature is over 20 million degrees Fahrenheit. There is also helium, a gas that is formed when the ...
... • Stars are balls of hot gas. • They are much larger than planets and much further from Earth. • The sun is the closest star to Earth. • Most of the gas in the inside of a star is hydrogen and its temperature is over 20 million degrees Fahrenheit. There is also helium, a gas that is formed when the ...
M - IMAG2E
... • Begin to understand how we will constrain stellar models with hard observational evidence ...
... • Begin to understand how we will constrain stellar models with hard observational evidence ...
Chapter 25.2 - Planet Earth
... tons. Densities this great are possible only when electrons are displaced inward from their regular orbits, around an atom’s nucleus, allowing the atoms to take up less than the “normal” amount of space. Material in this state is called degenerate matter. In degenerate matter, the atoms have been sq ...
... tons. Densities this great are possible only when electrons are displaced inward from their regular orbits, around an atom’s nucleus, allowing the atoms to take up less than the “normal” amount of space. Material in this state is called degenerate matter. In degenerate matter, the atoms have been sq ...
Stars, Galaxies, and the Universe
... Telescopes: Collect and focus different types of electromagnetic radiation including visible light. Observatory: A building that contains one or more telescopes. ...
... Telescopes: Collect and focus different types of electromagnetic radiation including visible light. Observatory: A building that contains one or more telescopes. ...
evolution of low
... ∼ 8 M¯) do not experience nuclear burning beyond helium burning • evolution ends when the envelope has been lost by stellar winds . superwind phase: very rapid mass loss (Ṁ ∼ 10−4 M¯ yr−1) . probably because envelope attains positive binding energy (due to energy reservoir in ionization energy) → e ...
... ∼ 8 M¯) do not experience nuclear burning beyond helium burning • evolution ends when the envelope has been lost by stellar winds . superwind phase: very rapid mass loss (Ṁ ∼ 10−4 M¯ yr−1) . probably because envelope attains positive binding energy (due to energy reservoir in ionization energy) → e ...
Lec10_2D
... The Death of a High Mass Star When the star’s core turns to iron, it again collapses. The increased pressure and temperature then causes iron to fuse. However… The products of iron fusion weigh more than the initial iron nucleus. According to E = m c2, this means that iron fusion does not make ener ...
... The Death of a High Mass Star When the star’s core turns to iron, it again collapses. The increased pressure and temperature then causes iron to fuse. However… The products of iron fusion weigh more than the initial iron nucleus. According to E = m c2, this means that iron fusion does not make ener ...
Death of Stars with the Mass of 0.3
... A star gets its energy by fusing hydrogen to helium. The fusion creates a radiation pressure that antagonizes the gravitation which causes the star to be stable. However, once the hydrogen in the core runs out, the star begins to fuse helium to carbon and oxygen. Because of the high pressure, the st ...
... A star gets its energy by fusing hydrogen to helium. The fusion creates a radiation pressure that antagonizes the gravitation which causes the star to be stable. However, once the hydrogen in the core runs out, the star begins to fuse helium to carbon and oxygen. Because of the high pressure, the st ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.