Life Cycle of a Star
... _______________ cloud of gas and dust from which our solar system formed _______________ the life cycle of a star _______________ an explosion of a star that emits large amounts of matter and energy Stellar Evolution (video or transcript) Put the steps in order: ______ A nebula condenses into small ...
... _______________ cloud of gas and dust from which our solar system formed _______________ the life cycle of a star _______________ an explosion of a star that emits large amounts of matter and energy Stellar Evolution (video or transcript) Put the steps in order: ______ A nebula condenses into small ...
Lecture 1
... White dwarfs are supported by electron degeneracy pressure: their electrons are pushed so tightly together, that they can't get any closer together or they will merge with protons in the nuclei. ...
... White dwarfs are supported by electron degeneracy pressure: their electrons are pushed so tightly together, that they can't get any closer together or they will merge with protons in the nuclei. ...
Astronomy
... increase in temperature. When fusion starts to begin, that's when a protostar has been formed. If the temperature reaches about 27,000,000,000°F, nuclear fusion begins, then stars start to form. ...
... increase in temperature. When fusion starts to begin, that's when a protostar has been formed. If the temperature reaches about 27,000,000,000°F, nuclear fusion begins, then stars start to form. ...
Asteroseismology with the Whole Earth Telescope
... The process of extracting from a signal the various frequencies and amplitudes that are present. Transform a light curve (time domain) into a set of frequencies in frequency space ...
... The process of extracting from a signal the various frequencies and amplitudes that are present. Transform a light curve (time domain) into a set of frequencies in frequency space ...
PRESENTATION: Evolution of the elements through the lifecycles of
... -Picture striking a rubber ball on the ground with a hammer. It will compress, but eventually expand and throw off the hammer, if the blow (the solar mass) is not strong enough to compress it into a black hole. -The Iron atoms are compressed to the point that the electrons are collapsing into the pr ...
... -Picture striking a rubber ball on the ground with a hammer. It will compress, but eventually expand and throw off the hammer, if the blow (the solar mass) is not strong enough to compress it into a black hole. -The Iron atoms are compressed to the point that the electrons are collapsing into the pr ...
Mass-Luminosity Relation for White
... Differing from the usual stars, we have no simple relation between their masses and luminosities in the case of the white-dwarf stars. Namely, the luminosity of a white dwarf frequently differs from that of another with the almost same mass and apparent chemical composition by a factor of one hundre ...
... Differing from the usual stars, we have no simple relation between their masses and luminosities in the case of the white-dwarf stars. Namely, the luminosity of a white dwarf frequently differs from that of another with the almost same mass and apparent chemical composition by a factor of one hundre ...
TAP 705-3: The parsec - Teaching Advanced Physics
... TAP 705-3: The parsec A unit of distance in common use amongst astronomers is the parsec. As the Earth moves in its orbit around the Sun, the position of nearby stars against the background of very distant stars seems to change. ...
... TAP 705-3: The parsec A unit of distance in common use amongst astronomers is the parsec. As the Earth moves in its orbit around the Sun, the position of nearby stars against the background of very distant stars seems to change. ...
Summary: The Structure and Evolution of Stars
... • Region A represents the main sequence in the cluster. All stars in this region are in the core hydrogen-burning phase, the longest evolutionary phase of a star. Stars at lower luminosity along the main sequence have lower masses (where roughly M ∝ L4 ). • Turning Point X: stars near the turning p ...
... • Region A represents the main sequence in the cluster. All stars in this region are in the core hydrogen-burning phase, the longest evolutionary phase of a star. Stars at lower luminosity along the main sequence have lower masses (where roughly M ∝ L4 ). • Turning Point X: stars near the turning p ...
F03HW12
... RQ 12: How can we understand the Algol paradox? Answer: Algol is a binary star composed of a five solar mass main sequence star and a one solar mass giant. This presents a paradox because massive stars evolve faster than low mass stars, so the five solar mass stars should leave the main sequence bef ...
... RQ 12: How can we understand the Algol paradox? Answer: Algol is a binary star composed of a five solar mass main sequence star and a one solar mass giant. This presents a paradox because massive stars evolve faster than low mass stars, so the five solar mass stars should leave the main sequence bef ...
Friday, April 26
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
1. The distances to the most remote galaxies can be
... the disc of gas and dust surrounding a young star that will soon form a solar system. the ejected envelope of a red giant star surrounding a stellar core remnant. a type of young, medium mass star. a planet surrounded by a cool shell of molecular gas. ...
... the disc of gas and dust surrounding a young star that will soon form a solar system. the ejected envelope of a red giant star surrounding a stellar core remnant. a type of young, medium mass star. a planet surrounded by a cool shell of molecular gas. ...
Activity: Stellar Spectra
... composition of the entire star or just a part of it? (HINT: Stars are opaque). (T: 1 mark) 3. Astronomers focus on distant stars through an optical telescope and pass the starlight through a diffraction grating ...
... composition of the entire star or just a part of it? (HINT: Stars are opaque). (T: 1 mark) 3. Astronomers focus on distant stars through an optical telescope and pass the starlight through a diffraction grating ...
TYPES OF PLANETS AND STARS
... of rocks and/or other metals and they have a solid surface that makes them different from other planets that don’t have a solid surface. Terrestrial planets also have topological features such as valleys, volcanoes and craters. In our solar system there are four terrestrial planets and they are Merc ...
... of rocks and/or other metals and they have a solid surface that makes them different from other planets that don’t have a solid surface. Terrestrial planets also have topological features such as valleys, volcanoes and craters. In our solar system there are four terrestrial planets and they are Merc ...
The Life and Death of Stars
... It has been doing this for 4.5 billion years Has enough Hydrogen in the core for 5 billion years What happens when all the core hydrogen is burnt? – the core will collapse, become denser and hotter – Helium starts to fuse into Carbon and Oxygen ...
... It has been doing this for 4.5 billion years Has enough Hydrogen in the core for 5 billion years What happens when all the core hydrogen is burnt? – the core will collapse, become denser and hotter – Helium starts to fuse into Carbon and Oxygen ...
Astronomy 100 Tuesday, Thursday 2:30
... • After a supernova if all the outer mass of the star is not blown off • The mass falls back on the neutron star • The gravity causes the neutron star to keep ...
... • After a supernova if all the outer mass of the star is not blown off • The mass falls back on the neutron star • The gravity causes the neutron star to keep ...
COSMOLOGY 1 An Introduction to the Universe
... After a low mass star like the Sun exhausts the supply of hydrogen in its core, there is no longer any source of heat to support the core against gravity. Hydrogen burning continues in a shell around the core and the star evolves into a red giant. When the Sun becomes a red giant, its atmosphere wi ...
... After a low mass star like the Sun exhausts the supply of hydrogen in its core, there is no longer any source of heat to support the core against gravity. Hydrogen burning continues in a shell around the core and the star evolves into a red giant. When the Sun becomes a red giant, its atmosphere wi ...
Lecture1
... The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit ...
... The “parallax” is the apparent shift in position of a nearby star, relative to background stars, as Earth moves around the Sun in it’s orbit ...
Wednesday, April 23 - Otterbein University
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
... Small, rapidly rotating objects Can’t be white dwarfs; must be neutron stars ...
N.2 Formation of Mass
... causes the stars to contract and heat up more. • This increase in heat and pressure causes helium atoms to fusion with other helium and hydrogen atoms. • This forms heavier elements such as carbon, oxygen • Sometimes large stars will explode when they run out of hydrogen gas becoming supernovas, thi ...
... causes the stars to contract and heat up more. • This increase in heat and pressure causes helium atoms to fusion with other helium and hydrogen atoms. • This forms heavier elements such as carbon, oxygen • Sometimes large stars will explode when they run out of hydrogen gas becoming supernovas, thi ...
Stellar Remnants White Dwarfs, Neutron Stars & Black Holes
... solids, liquids or gases. • They often have very strong magnetic fields and very rapid spin rates. ...
... solids, liquids or gases. • They often have very strong magnetic fields and very rapid spin rates. ...
Supernova
... • Sun-like stars (M< 9 Msolar) stop producing energy with Shell Helium Burning and leave behind a carbon core (White Dwarf). • Stars more massive continue to fuse heavier elements in their cores as they evolve. Carbon burning at 600 Million K Neon burning at 1.2 Billion K Oxygen Burning at 1.5 Billi ...
... • Sun-like stars (M< 9 Msolar) stop producing energy with Shell Helium Burning and leave behind a carbon core (White Dwarf). • Stars more massive continue to fuse heavier elements in their cores as they evolve. Carbon burning at 600 Million K Neon burning at 1.2 Billion K Oxygen Burning at 1.5 Billi ...
Life Cycle of Stars
... temperature of a star determines its color – from cool, red stars to hot, blue ones. The Sun is a medium temperature yellow star. Around 1910, astronomers Ejnar Hertzsprung and Henry Russell independently developed what is now known as the Hertzsprung-Russell or H-R diagram. This graph plots the rel ...
... temperature of a star determines its color – from cool, red stars to hot, blue ones. The Sun is a medium temperature yellow star. Around 1910, astronomers Ejnar Hertzsprung and Henry Russell independently developed what is now known as the Hertzsprung-Russell or H-R diagram. This graph plots the rel ...
sun_parallax2
... IF reaction rates go down in the core, gravity will cause the core to begin to shrink. (gravity wins) As the core shrinks the density and temperature of the core begins to rise. When these two parameters increase so does the nuclear reaction rate. (internal pressure wins) The core re-expands. Ultima ...
... IF reaction rates go down in the core, gravity will cause the core to begin to shrink. (gravity wins) As the core shrinks the density and temperature of the core begins to rise. When these two parameters increase so does the nuclear reaction rate. (internal pressure wins) The core re-expands. Ultima ...
Main sequence
In astronomy, the main sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. These color-magnitude plots are known as Hertzsprung–Russell diagrams after their co-developers, Ejnar Hertzsprung and Henry Norris Russell. Stars on this band are known as main-sequence stars or ""dwarf"" stars.After a star has formed, it generates thermal energy in the dense core region through the nuclear fusion of hydrogen atoms into helium. During this stage of the star's lifetime, it is located along the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and other factors. All main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. The strong dependence of the rate of energy generation in the core on the temperature and pressure helps to sustain this balance. Energy generated at the core makes its way to the surface and is radiated away at the photosphere. The energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.The main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. Stars below about 1.5 times the mass of the Sun (or 1.5 solar masses (M☉)) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. Above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the CNO cycle that produces helium from hydrogen atoms. Main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. Below this mass, stars have cores that are entirely radiative with convective zones near the surface. With decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases, whereas main-sequence stars below 0.4 M☉ undergo convection throughout their mass. When core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.In general, the more massive a star is, the shorter its lifespan on the main sequence. After the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the HR diagram. The behavior of a star now depends on its mass, with stars below 0.23 M☉ becoming white dwarfs directly, whereas stars with up to ten solar masses pass through a red giant stage. More massive stars can explode as a supernova, or collapse directly into a black hole.