Life Cycle of a Star
... What happens to a star after the main sequence phase? Old age and death! How long it takes for a star to die depends upon its initial mass. Larger stars have more fuel, but they have to burn (fuse) it faster in order to maintain equilibrium. Because thermonuclear fusion occurs at a faster rate in ma ...
... What happens to a star after the main sequence phase? Old age and death! How long it takes for a star to die depends upon its initial mass. Larger stars have more fuel, but they have to burn (fuse) it faster in order to maintain equilibrium. Because thermonuclear fusion occurs at a faster rate in ma ...
(the factor f star in the Drake equation. Recall it
... nuclei of the atoms started to get pushed together. To do this requires a HUGE pressure by earthly standards and it only occurs inside stars and in the (fortunately rare) explosion of thermonuclear weapons. To get an idea how this works requires some ideas about two other fundamental forces of natur ...
... nuclei of the atoms started to get pushed together. To do this requires a HUGE pressure by earthly standards and it only occurs inside stars and in the (fortunately rare) explosion of thermonuclear weapons. To get an idea how this works requires some ideas about two other fundamental forces of natur ...
Star Questions 2008 - Fort Thomas Independent Schools
... Describe the death of these two stars, one with 2 solar masses and one with 10 solar masses. What is a supernova and what is its significance? Describe the difference between a Type I and Type II supernova? What will happen to our Sun when it dies? Which is more luminous, a low-mass or a high-mass s ...
... Describe the death of these two stars, one with 2 solar masses and one with 10 solar masses. What is a supernova and what is its significance? Describe the difference between a Type I and Type II supernova? What will happen to our Sun when it dies? Which is more luminous, a low-mass or a high-mass s ...
Pistol Star - University of Dayton
... •When hydrogen or helium fuse, energy is released. In contrast, iron fusion absorbs the energy and cools a star. When this happens the thermal pressure that forced the stellar gases outward diminishes , and the star collapses under the influence of gravity. •Due to this strange phenomena supernovas ...
... •When hydrogen or helium fuse, energy is released. In contrast, iron fusion absorbs the energy and cools a star. When this happens the thermal pressure that forced the stellar gases outward diminishes , and the star collapses under the influence of gravity. •Due to this strange phenomena supernovas ...
Geochemistry & Lab
... masses you get a black hole instead (this may have happened with Supernova 1987A, although detection of neutrinos in the first few seconds of the supernova suggests that at least initially it was a neutron star). In any case, the basic idea is that when the central part of the star fuses its way to ...
... masses you get a black hole instead (this may have happened with Supernova 1987A, although detection of neutrinos in the first few seconds of the supernova suggests that at least initially it was a neutron star). In any case, the basic idea is that when the central part of the star fuses its way to ...
Evolution and the Big Bang, ET Life Lec. 6, Jan 18, 2002
... Life of a Star • Birth: collapse of gas cloud forms protostar. • Main sequence: center of star becomes hot ...
... Life of a Star • Birth: collapse of gas cloud forms protostar. • Main sequence: center of star becomes hot ...
The Milky Way - Midlandstech
... Guidepost Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence and their old age as they swell to become giant stars. Here you will answer three essential questions: • What happens ...
... Guidepost Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main sequence and their old age as they swell to become giant stars. Here you will answer three essential questions: • What happens ...
REVIEW: STAR`S TEST
... List the visible light from longest to shortest wavelengths. Red Orange Yellow Green Blue Indigo Violet What happens to white light as it passes through a prism ? REFRACTS Which color refracts the most and least ? RED What is thought to be at the center of all galaxies ? ____BLACK HOLE______ What is ...
... List the visible light from longest to shortest wavelengths. Red Orange Yellow Green Blue Indigo Violet What happens to white light as it passes through a prism ? REFRACTS Which color refracts the most and least ? RED What is thought to be at the center of all galaxies ? ____BLACK HOLE______ What is ...
Evolution of High Mass Stars
... • How does a high-mass star die? – Iron core collapses, leading to a supernova ...
... • How does a high-mass star die? – Iron core collapses, leading to a supernova ...
PowerPoint Presentation - Research in observational
... On the (red) giant branch: the first dredge-up • The expanding envelope is cool enough for molecules to form so that the opacity goes up and envelope convection sets in. • As the convective layer grows and extends from H-burning shell to surface, it brings to the surface the by products of H burnin ...
... On the (red) giant branch: the first dredge-up • The expanding envelope is cool enough for molecules to form so that the opacity goes up and envelope convection sets in. • As the convective layer grows and extends from H-burning shell to surface, it brings to the surface the by products of H burnin ...
High Mass Stars
... Consider a star 25 times the mass of the Sun – From H-R diagram its luminosity is 100000 times greater than the Sun’s. – It therefore burns fuel (uses it’s mass) 100000 times faster than the Sun. – It has 25 times the mass of the Sun so its lifetime will be 25/100000 = 0.00025 times than the Sun’s l ...
... Consider a star 25 times the mass of the Sun – From H-R diagram its luminosity is 100000 times greater than the Sun’s. – It therefore burns fuel (uses it’s mass) 100000 times faster than the Sun. – It has 25 times the mass of the Sun so its lifetime will be 25/100000 = 0.00025 times than the Sun’s l ...
Introduction to Astronomy
... “We understand the possibility of determining [celestial bodies’] shapes, their distances, their sizes and motions, whereas never, by any means, will we be able to study their chemical composition. --Auguste Comte (philosopher), 1835 ...
... “We understand the possibility of determining [celestial bodies’] shapes, their distances, their sizes and motions, whereas never, by any means, will we be able to study their chemical composition. --Auguste Comte (philosopher), 1835 ...
REVIEW: STAR`S TEST
... The apparent magnitude of a star tells you how bright the star is as viewed from A nebula is a huge cloud of gas, primarily composed of hydrogen A nebula becomes a star when _______fusion takes place______________ Our sun is what color ? _____________yellow____________________ ...
... The apparent magnitude of a star tells you how bright the star is as viewed from A nebula is a huge cloud of gas, primarily composed of hydrogen A nebula becomes a star when _______fusion takes place______________ Our sun is what color ? _____________yellow____________________ ...
Star Life Cycle Computer Lab
... 10. Do the Interactive Equilibrium Lab and Practice Quizzes. 11. After their life on the main sequence, what happens to massive stars? 12. What is the 3rd fuel that stars can use after Hydrogen and Helium? The Beginning of the End 13. When a star is fusing helium, what stage of its life is it consid ...
... 10. Do the Interactive Equilibrium Lab and Practice Quizzes. 11. After their life on the main sequence, what happens to massive stars? 12. What is the 3rd fuel that stars can use after Hydrogen and Helium? The Beginning of the End 13. When a star is fusing helium, what stage of its life is it consid ...
Death of massive stars
... Supernova Explosions of Massive Stars • As a star develops an iron core, energy production declines, and the core contracts. –Nuclear reactions involving iron begin. –However, they remove energy from the core—causing it to contract even further. –Once this process starts, the core of the star colla ...
... Supernova Explosions of Massive Stars • As a star develops an iron core, energy production declines, and the core contracts. –Nuclear reactions involving iron begin. –However, they remove energy from the core—causing it to contract even further. –Once this process starts, the core of the star colla ...
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.