Stars - TeacherWeb
... here on Earth, they can be many different sizes. • Neutron Stars are the smallest. They are made of the material left behind after a larger star explodes; about 20 kilometers in diameter. ...
... here on Earth, they can be many different sizes. • Neutron Stars are the smallest. They are made of the material left behind after a larger star explodes; about 20 kilometers in diameter. ...
ppt - Astronomy & Physics
... These are found above the main-sequence Many stars (depends on their mass) end up here after they leave the main-sequence Their temperatures are not that high (2000— 6000K) but they are very luminous by Stefan-Boltzmann law they must be very large ...
... These are found above the main-sequence Many stars (depends on their mass) end up here after they leave the main-sequence Their temperatures are not that high (2000— 6000K) but they are very luminous by Stefan-Boltzmann law they must be very large ...
South Pasadena • Chemistry Name 8 • Nuclear Chemistry Period
... both Chinese astronomers and the Anasazi in the American Southwest. For more than 50 years, scientists have been studying the links between chemical elements and how they are created. Elements lighter than iron are formed from successive nuclear fusion reactions, beginning with hydrogen atoms. All s ...
... both Chinese astronomers and the Anasazi in the American Southwest. For more than 50 years, scientists have been studying the links between chemical elements and how they are created. Elements lighter than iron are formed from successive nuclear fusion reactions, beginning with hydrogen atoms. All s ...
Elements from Stardust
... nucleus, forming a carbon nucleus. • A Helium nucleus can join with a carbon nucleus forming Oxygen. • But stars the size of our Sun do not have enough energy to produce elements heavier than oxygen. ...
... nucleus, forming a carbon nucleus. • A Helium nucleus can join with a carbon nucleus forming Oxygen. • But stars the size of our Sun do not have enough energy to produce elements heavier than oxygen. ...
Document
... Gravity pulls gas and dust closer together in some regions of a nebula – as the matter contracts, it forms a hot, dense sphere – the sphere becomes a star if its center grows hot and dense enough for fusion to occur When a star dies, its matter may eventually become part of new stars ...
... Gravity pulls gas and dust closer together in some regions of a nebula – as the matter contracts, it forms a hot, dense sphere – the sphere becomes a star if its center grows hot and dense enough for fusion to occur When a star dies, its matter may eventually become part of new stars ...
Stellar Remnants
... • An object as big as the Sun with a onemonth rotation period will rotate more than 1000 times a second if squeezed down to the size of a neutron star – This happens when a massive star’s iron core collapses – magnetic field beams radiation energy in ...
... • An object as big as the Sun with a onemonth rotation period will rotate more than 1000 times a second if squeezed down to the size of a neutron star – This happens when a massive star’s iron core collapses – magnetic field beams radiation energy in ...
Stars and H
... Characteristics of Stars Temperature/Color Mass Luminosity • Absolute Magnitude • Apparent Magnitude ...
... Characteristics of Stars Temperature/Color Mass Luminosity • Absolute Magnitude • Apparent Magnitude ...
Reminder: Assignments are due back to teachers within 2 school days.
... The discoveries of the white dwarf, the neutron star, and the black hole, coming well after the discovery of the red giant are among eh most exciting developments in decades because they may be well present physicists with their greatest challenge since thefailure of classical mechanics. In the lif ...
... The discoveries of the white dwarf, the neutron star, and the black hole, coming well after the discovery of the red giant are among eh most exciting developments in decades because they may be well present physicists with their greatest challenge since thefailure of classical mechanics. In the lif ...
Slide 1
... Eventually, of course, even the helium in the core becomes exhausted -- this happens after only about 100 million years because helium burning is less efficient than hydrogen burning. Now the core is mostly carbon and oxygen (C-O) and once again continues its collapse. The star produces energy by bu ...
... Eventually, of course, even the helium in the core becomes exhausted -- this happens after only about 100 million years because helium burning is less efficient than hydrogen burning. Now the core is mostly carbon and oxygen (C-O) and once again continues its collapse. The star produces energy by bu ...
Stars and Galaxies
... 16. The nearer an object is to the observer, the greater its _______________________. 17. __________________ can be used to measure distance from Earth of relatively close stars. 18. Distances in space are measured in _____________________. 19. A light-year is the distance __________________ travels ...
... 16. The nearer an object is to the observer, the greater its _______________________. 17. __________________ can be used to measure distance from Earth of relatively close stars. 18. Distances in space are measured in _____________________. 19. A light-year is the distance __________________ travels ...
Stars
... Over time, gravity begins to pull this material together. Hydrogen is the most common element that gets pulled in by gravity. Eventually large, dark, cool clouds of matter form. Because of the mass increase, gravity begins to contract the cloud further. The temperature begins to rise and the cloud r ...
... Over time, gravity begins to pull this material together. Hydrogen is the most common element that gets pulled in by gravity. Eventually large, dark, cool clouds of matter form. Because of the mass increase, gravity begins to contract the cloud further. The temperature begins to rise and the cloud r ...
Stellar Interiors
... What could power the Sun for this length of time? Chemical energy (burning) -Kelvin-Helmholtz contraction (gravitational energy) -Nuclear Fusion Reactions -- ...
... What could power the Sun for this length of time? Chemical energy (burning) -Kelvin-Helmholtz contraction (gravitational energy) -Nuclear Fusion Reactions -- ...
Stars and Stellar Evolution
... Core gets hotter --> hydrogen fusion in outer shell increases --> expands outer layer --> giant body Surface cools --> red Core keeps heating up and converts helium to carbon to produce energy ...
... Core gets hotter --> hydrogen fusion in outer shell increases --> expands outer layer --> giant body Surface cools --> red Core keeps heating up and converts helium to carbon to produce energy ...
Name Date ______ Period _____ Earth Science Chapter 25 Study
... What is the name for the interstellar matter that will eventually form a star? __________________________________________________________________ When is a star said to be born? __________________________________________________________________ What forces are most responsible for the formation of a ...
... What is the name for the interstellar matter that will eventually form a star? __________________________________________________________________ When is a star said to be born? __________________________________________________________________ What forces are most responsible for the formation of a ...
Mr. Scharff
... Introduction. The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the ...
... Introduction. The Hertzsprung-Russell diagram is actually a graph that illustrates the relationship that exists between the average surface temperature of stars and their absolute magnitude, which is how bright they would appear to be if they were al the same distance away. Rather than speak of the ...
Nuclear Reactions
... • There are two routes for this process The Proton-Proton Reaction dominates below 1.5 MSun The CNO reaction dominates above 1.5 MSun (They contribute equally to the energy at 1.5 MSun ) This “Hydrogen Burning” continues until fuel exhaustion ....when all core hydrogen has been converted to helium W ...
... • There are two routes for this process The Proton-Proton Reaction dominates below 1.5 MSun The CNO reaction dominates above 1.5 MSun (They contribute equally to the energy at 1.5 MSun ) This “Hydrogen Burning” continues until fuel exhaustion ....when all core hydrogen has been converted to helium W ...
Chapter 19 Notes Stars Stars are bright balls of gas that are trillions
... i. While many stars become white dwarves as they get older, very massive stars can become strange objects like pulsars, supernovas, black holes and neutron stars. ii. Supernovas 1. Massive stars use their hydrogen much faster than stars like the sun do. 2. At the end of their lives they may explode ...
... i. While many stars become white dwarves as they get older, very massive stars can become strange objects like pulsars, supernovas, black holes and neutron stars. ii. Supernovas 1. Massive stars use their hydrogen much faster than stars like the sun do. 2. At the end of their lives they may explode ...
Out of this World
... Galaxies and Star Clusters What is a Quasar? Objects that look like faint stars but emit up to 100x more energy than our entire galaxy. What is a light-year? The distance that light rays travel in one year. (9.46 x 1012 ...
... Galaxies and Star Clusters What is a Quasar? Objects that look like faint stars but emit up to 100x more energy than our entire galaxy. What is a light-year? The distance that light rays travel in one year. (9.46 x 1012 ...
How Stars Form Powerpoint
... Most important: Stars do not move along the Main Sequence! Once they reach it, they are in equilibrium and do not move until their fuel begins to run out. ...
... Most important: Stars do not move along the Main Sequence! Once they reach it, they are in equilibrium and do not move until their fuel begins to run out. ...
powerpoint version
... Now have a mass-luminosity diagram for Main Sequence stars. This tells us that the heavier they are, the greater is their energy output rate i.e. Luminosity (mass mass mass mass) but Total energy available mass Therefore, low mass stars live longer. ...
... Now have a mass-luminosity diagram for Main Sequence stars. This tells us that the heavier they are, the greater is their energy output rate i.e. Luminosity (mass mass mass mass) but Total energy available mass Therefore, low mass stars live longer. ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.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.