Topic 3 – Waves and the Universe
... Stars with considerably more mass than the Sun are hotter and brighter The fusion reactions in a massive star’s core happen at a faster ratestable main sequence is shorter than in smaller stars Once hydrogen runs out and the core cools, massive stars become red supergiants At the end of the supergi ...
... Stars with considerably more mass than the Sun are hotter and brighter The fusion reactions in a massive star’s core happen at a faster ratestable main sequence is shorter than in smaller stars Once hydrogen runs out and the core cools, massive stars become red supergiants At the end of the supergi ...
Topic 3 notes - WordPress.com
... Stars with considerably more mass than the Sun are hotter and brighter The fusion reactions in a massive star’s core happen at a faster ratestable main sequence is shorter than in smaller stars Once hydrogen runs out and the core cools, massive stars become red supergiants At the end of the supergi ...
... Stars with considerably more mass than the Sun are hotter and brighter The fusion reactions in a massive star’s core happen at a faster ratestable main sequence is shorter than in smaller stars Once hydrogen runs out and the core cools, massive stars become red supergiants At the end of the supergi ...
Characteristics of Stars
... characteristics astronomers use to classify stars? 5. What size is the Sun compared to other stars? What are very large stars called? How far would the supergiant Betelgeuse reach if it were to replace our Sun? How big are white dwarf stars? How big are neutron stars? 6. What does a star’s color rev ...
... characteristics astronomers use to classify stars? 5. What size is the Sun compared to other stars? What are very large stars called? How far would the supergiant Betelgeuse reach if it were to replace our Sun? How big are white dwarf stars? How big are neutron stars? 6. What does a star’s color rev ...
slides
... Today at that location we see a nebula, with gases in the cloud expanding outward at about 1,500 km/s. In 1967 a pulsar was discovered in it. – period 33 ms (flashes 30 times per second), slowin ...
... Today at that location we see a nebula, with gases in the cloud expanding outward at about 1,500 km/s. In 1967 a pulsar was discovered in it. – period 33 ms (flashes 30 times per second), slowin ...
Nuclear Fusion – when two H atoms combine to form one atom thus
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
... Nebula – Stars are formed or “born” in a nebula. Massive cosmic cloud of matter from which stars are created. Light Year – distance light travels in one year. 186,000 miles/sec – speed of light Life Cycle of a Star Stars start off as a nebula until a nuclear explosion causes the star to shine. The n ...
Misc-ReviewForAstroTest
... incredible amount of energy. The star becomes a supernova, increasing in brightness by billions of times for a few days, and then dies out. ...
... incredible amount of energy. The star becomes a supernova, increasing in brightness by billions of times for a few days, and then dies out. ...
1. Compute the deflection angle of a star whose light... limb of the Sun. Also compute the deflection angle of...
... 1. Compute the deflection angle of a star whose light just grazes the limb of the Sun. Also compute the deflection angle of a star whose light just grazes the limb of a 1.4M neutron star, if the neutron star was at the same distance from the Earth as the Sun. State assumptions. 2. Use the Plummer p ...
... 1. Compute the deflection angle of a star whose light just grazes the limb of the Sun. Also compute the deflection angle of a star whose light just grazes the limb of a 1.4M neutron star, if the neutron star was at the same distance from the Earth as the Sun. State assumptions. 2. Use the Plummer p ...
qwk9
... A. Accretion disks and bi-polar jets are features associated with both star formation and active galactic nuclei B. Hayashi tracks describe the evolution of a star on the HR diagram after it has started nuclear fusion C. New stars in the Milky Way are born as a result of the gravitational collapse o ...
... A. Accretion disks and bi-polar jets are features associated with both star formation and active galactic nuclei B. Hayashi tracks describe the evolution of a star on the HR diagram after it has started nuclear fusion C. New stars in the Milky Way are born as a result of the gravitational collapse o ...
Solutions
... The luminosity of a main sequence star is proportional to M4. The available hydrogen fuel for the main sequence is proportional to M. Therefore, the lifetime of a main sequence star is proportional to 1/M3. (You could also use the equation on page 320 of your textbook which uses L∝M3.3 to come up wi ...
... The luminosity of a main sequence star is proportional to M4. The available hydrogen fuel for the main sequence is proportional to M. Therefore, the lifetime of a main sequence star is proportional to 1/M3. (You could also use the equation on page 320 of your textbook which uses L∝M3.3 to come up wi ...
August 29 - Astronomy
... From the Big Bang to Planets a brief history of the Universe Background material – Chapter 1 in text Things I expect you to know, but will not be ...
... From the Big Bang to Planets a brief history of the Universe Background material – Chapter 1 in text Things I expect you to know, but will not be ...
The star and the trees prostrate
... electromagnetic radiation, including photons, the particles of light. This radiation exerts an outward pressure that exactly balances the inward pull of gravity caused by the star's mass. As the nuclear fuel is exhausted, the outward forces of radiation diminish, allowing the gravitation to compress ...
... electromagnetic radiation, including photons, the particles of light. This radiation exerts an outward pressure that exactly balances the inward pull of gravity caused by the star's mass. As the nuclear fuel is exhausted, the outward forces of radiation diminish, allowing the gravitation to compress ...
FINAL EXAM Name: ASTRONOMY II - 79202 Spring 1995
... Total mass Population type Number of stars Age ...
... Total mass Population type Number of stars Age ...
What makes stars tick?
... ook up at the night sky from a dark site, and you’ll see tens of thousands of burning orbs of gas. Just one of those twinkling dots we call stars could be a behemoth with a mass 80 times that of our own Sun. At it’s core sits a cauldron of nuclear reactions that power the star, allowing us to see it ...
... ook up at the night sky from a dark site, and you’ll see tens of thousands of burning orbs of gas. Just one of those twinkling dots we call stars could be a behemoth with a mass 80 times that of our own Sun. At it’s core sits a cauldron of nuclear reactions that power the star, allowing us to see it ...
No Slide Title
... • Some supernovas form neutron stars and black holes. – If the core that remains after a supernova has a mass of 1.4 to 3 solar masses, the remnant can become a neutron star. – If the leftover core has a mass that is greater than three solar masses, it will collapse to form a black hole. • black hol ...
... • Some supernovas form neutron stars and black holes. – If the core that remains after a supernova has a mass of 1.4 to 3 solar masses, the remnant can become a neutron star. – If the leftover core has a mass that is greater than three solar masses, it will collapse to form a black hole. • black hol ...
Space Science Unit
... • Stars stay in this part of their life cycle for a long time; most of their “lives” ...
... • Stars stay in this part of their life cycle for a long time; most of their “lives” ...
Lesson 10 Red Shift
... Normally when we look at white light, such as from the Sun or many artificial sources, it appears more or less white. We do not see all the colours (i.e., When all these colours are mixed together, they appear white). How do I relate Light to Stars? Light from stars can reveal an enormous amount abo ...
... Normally when we look at white light, such as from the Sun or many artificial sources, it appears more or less white. We do not see all the colours (i.e., When all these colours are mixed together, they appear white). How do I relate Light to Stars? Light from stars can reveal an enormous amount abo ...
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 ...
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.