Stellar Evolution
... • Core radius = Diameter of Earth! • Pressure and temperature great enough for the Helium Flash! 3He C + Energy ...
... • Core radius = Diameter of Earth! • Pressure and temperature great enough for the Helium Flash! 3He C + Energy ...
Lecture 9: Post-main sequence evolution of stars Lifespan on the
... • What remains is a white dwarf star, in the lower left portion of the H-R diagram. ...
... • What remains is a white dwarf star, in the lower left portion of the H-R diagram. ...
Energy Levels in Atoms
... Balmer series from level 2 is in the visible. The Lyman series lines are all ultraviolet. ...
... Balmer series from level 2 is in the visible. The Lyman series lines are all ultraviolet. ...
Chapter 12 Stellar Evolution
... quite young – its H–R diagram is that of a newborn cluster. Its age cannot be more than about 10 million years. ...
... quite young – its H–R diagram is that of a newborn cluster. Its age cannot be more than about 10 million years. ...
Planck curves
... A. Wien’s Law This law can be derived from Planck's Law. It states that the radiation peak on the Planck curve varies inversely with the temperature, so red stars are relatively cool, but blue stars (shorter are hot. ...
... A. Wien’s Law This law can be derived from Planck's Law. It states that the radiation peak on the Planck curve varies inversely with the temperature, so red stars are relatively cool, but blue stars (shorter are hot. ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... understand the stellar content of such clusters ...
... understand the stellar content of such clusters ...
8hrdiagram1s
... The flux is the luminosity divided by the area of that sphere where d is the distance from the star ...
... The flux is the luminosity divided by the area of that sphere where d is the distance from the star ...
Slide 1
... supernova is an exploding star that can become three times as bright as the sun. When a supernova occurs. All the dust particles, gas, and Dupree collect up. Creating a Nebula. These Nebulas can create many stars like our sun. Some stars can be brighter then others. This is an example of a Supernova ...
... supernova is an exploding star that can become three times as bright as the sun. When a supernova occurs. All the dust particles, gas, and Dupree collect up. Creating a Nebula. These Nebulas can create many stars like our sun. Some stars can be brighter then others. This is an example of a Supernova ...
V Example: our SUN (G2V)
... Modified in part from http://astronomyonline.org/Stars/HighMassEvolution.asp A white dwarf is the degenerate carbon core of a low mass star (like our Sun). A neutron star is the degenerate iron core of a high mass star. A pulsar is spinning neutron star. A black hole is the remnant of the collapse o ...
... Modified in part from http://astronomyonline.org/Stars/HighMassEvolution.asp A white dwarf is the degenerate carbon core of a low mass star (like our Sun). A neutron star is the degenerate iron core of a high mass star. A pulsar is spinning neutron star. A black hole is the remnant of the collapse o ...
Critical Thinking Questions: (work on these with a partner) Post
... 2. Average sized stars like our Sun do not explode as supernova, but super-massive stars do. Both types of stars undergo nuclear fusion and have an outer shell influenced by gravity. Explain why a star like our Sun will not go supernova, but a super-massive star will. Explain your answer describing ...
... 2. Average sized stars like our Sun do not explode as supernova, but super-massive stars do. Both types of stars undergo nuclear fusion and have an outer shell influenced by gravity. Explain why a star like our Sun will not go supernova, but a super-massive star will. Explain your answer describing ...
Document
... • They are losing mass rapidly by means of a very strong stellar wind, with speeds up to 2000 km/s. While our own Sun loses approximately 10−14 solar masses every year, Wolf–Rayet stars typically lose 10−5 solar masses a year.[1] • Wolf–Rayet stars are extremely hot, with surface temperatures in th ...
... • They are losing mass rapidly by means of a very strong stellar wind, with speeds up to 2000 km/s. While our own Sun loses approximately 10−14 solar masses every year, Wolf–Rayet stars typically lose 10−5 solar masses a year.[1] • Wolf–Rayet stars are extremely hot, with surface temperatures in th ...
Supernovae
... - Provide momentum through collisions to throw off material. - Heat the stellar material so that it expands. ...
... - Provide momentum through collisions to throw off material. - Heat the stellar material so that it expands. ...
Life Cycle of the Stars
... The interior of the fragment has begun heating, and is about 10,000 K. For the first time, the fragement is beginning to look like a star. The dense, opaque region at the center is called a protostar Copyright © 2010 Pearson Education, Inc. ...
... The interior of the fragment has begun heating, and is about 10,000 K. For the first time, the fragement is beginning to look like a star. The dense, opaque region at the center is called a protostar Copyright © 2010 Pearson Education, Inc. ...
Uniqueness of the Earth, Lebo, 7-30
... Most all stars in the Milky Way are in the central bulge, a globular cluster or a spiral arm. In each of these locations the star densities are too high – the planetary orbits would be unstable. ...
... Most all stars in the Milky Way are in the central bulge, a globular cluster or a spiral arm. In each of these locations the star densities are too high – the planetary orbits would be unstable. ...
Conference Summary Richard Ellis (Caltech) ITALIA
... • Masses and colors of z~2-3 red galaxies (Henriques, Conselice) • Evidence of star formation thresholds (Faber) • Timescale of truncation and AGN feedback (Somerville, Faber) • Morphology versus color (red disks) ...
... • Masses and colors of z~2-3 red galaxies (Henriques, Conselice) • Evidence of star formation thresholds (Faber) • Timescale of truncation and AGN feedback (Somerville, Faber) • Morphology versus color (red disks) ...
Free Referat Word Dimensiune: 63.5KB
... dense, cold molecular clouds whose dust obscures newly formed stars from our view. For reasons which are not fully understood, but which may have to do with collisions of molecular clouds, or shockwaves passing through molecular clouds as the clouds pass through spiral structure in galaxies, or magn ...
... dense, cold molecular clouds whose dust obscures newly formed stars from our view. For reasons which are not fully understood, but which may have to do with collisions of molecular clouds, or shockwaves passing through molecular clouds as the clouds pass through spiral structure in galaxies, or magn ...
Leaving the Main Sequence
... 7. White dwarf - this is all that is left of the Star. Core of carbon is very hot, but is no longer burning anything, so will eventually cool to a cinder. ...
... 7. White dwarf - this is all that is left of the Star. Core of carbon is very hot, but is no longer burning anything, so will eventually cool to a cinder. ...
Making H-R Diagrams - PLC-METS
... Making an H-R Diagram BACKGOUND INFORMATION: Stars in the sky are not created equal and are composed of different materials, different temperatures, different brightness, different sizes, and different distances from Earth. A star’s mass dictates how bright it will be, how long it will live, its tem ...
... Making an H-R Diagram BACKGOUND INFORMATION: Stars in the sky are not created equal and are composed of different materials, different temperatures, different brightness, different sizes, and different distances from Earth. A star’s mass dictates how bright it will be, how long it will live, its tem ...
What is a Star - Optics Institute of Southern California
... The Main Sequence The properties of a main sequence star can be understood by considering the various physical processes acting in the interior. First is the hydrostatic balance, also called hydrostatic equilibrium. This determines the density structure of the star as the internal pressure gradient ...
... The Main Sequence The properties of a main sequence star can be understood by considering the various physical processes acting in the interior. First is the hydrostatic balance, also called hydrostatic equilibrium. This determines the density structure of the star as the internal pressure gradient ...
Document
... 2. On the next page you will find a listing of the nearest, brightest, and other stars, as well as their surface temperatures and absolute magnitude. On your H-R diagram, plot the absolute magnitude vs. surface temperature for all of the stars listed. Use an * to label the location of the Sun. 3. ...
... 2. On the next page you will find a listing of the nearest, brightest, and other stars, as well as their surface temperatures and absolute magnitude. On your H-R diagram, plot the absolute magnitude vs. surface temperature for all of the stars listed. Use an * to label the location of the Sun. 3. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.