METRIC PREFIXES
... 1. One light-year in the distance light travels in one year. This distance is equal to 9.461 x 1015m. After the sun, the star nearest to Earth is Alpha Centauri, which is about 4.35 light- years from Earth. Express this distance in a. megameters ...
... 1. One light-year in the distance light travels in one year. This distance is equal to 9.461 x 1015m. After the sun, the star nearest to Earth is Alpha Centauri, which is about 4.35 light- years from Earth. Express this distance in a. megameters ...
File
... and rebounds outward, like someone jumping on a trampoline. The rebounding core collides with the inward-falling surrounding layers and propels them outward, greatly assisted by the plentiful neutrinos (only a very tiny fraction of which actually interact with the gas). The star explodes, achieving ...
... and rebounds outward, like someone jumping on a trampoline. The rebounding core collides with the inward-falling surrounding layers and propels them outward, greatly assisted by the plentiful neutrinos (only a very tiny fraction of which actually interact with the gas). The star explodes, achieving ...
Part 1: If a 10000 K blackbody has a wavelength of peak emission at
... Use the blackbody simulator to get a better feel for this inverse relation and review the material in Module 1 Lecture F. Also, as I said in class, if this inverse relation did not hold then cooler objects would be emitting short wavelength high energy photons which doesn’t make any physical sense b ...
... Use the blackbody simulator to get a better feel for this inverse relation and review the material in Module 1 Lecture F. Also, as I said in class, if this inverse relation did not hold then cooler objects would be emitting short wavelength high energy photons which doesn’t make any physical sense b ...
white dwarf supernova
... When the white dwarf hits the mass limit, it gets hot enough for carbon fusion to start. It undergoes carbon fusion everywhere at once, so it’s a HUGE release of energy. This is called a “light curve” It plots luminosity as a function of time ...
... When the white dwarf hits the mass limit, it gets hot enough for carbon fusion to start. It undergoes carbon fusion everywhere at once, so it’s a HUGE release of energy. This is called a “light curve” It plots luminosity as a function of time ...
white dwarfs, neutron stars, black hole
... and very dramatic, in store for stars which are some 5 or more times as massive as our Sun. After the outer layers of the star have swollen into a red supergiant (i.e., a very big red giant), the core begins to yield to gravity and starts to shrink. As it shrinks, it grows hotter and denser, and a n ...
... and very dramatic, in store for stars which are some 5 or more times as massive as our Sun. After the outer layers of the star have swollen into a red supergiant (i.e., a very big red giant), the core begins to yield to gravity and starts to shrink. As it shrinks, it grows hotter and denser, and a n ...
Document
... Our plot of temperature against brightness is called an HR diagram. If we could watch over millions of years, we would see their life cycles as stars change: •Stars form in clouds of gas, settle onto the Main Sequence •Massive, hottest stars live short lives, explode as supernova •Intermediate mass ...
... Our plot of temperature against brightness is called an HR diagram. If we could watch over millions of years, we would see their life cycles as stars change: •Stars form in clouds of gas, settle onto the Main Sequence •Massive, hottest stars live short lives, explode as supernova •Intermediate mass ...
Astronomy Quiz 12 “Stars
... B. High mass inhibits the gravitational force, slowing fusion. C. High mass stars have atomic nuclei “bumping” against each other at rates high enough to trigger a supernova. D. High mass causes stronger gravity, which forces fusion to occur at a faster rate, and they burn out quickly. _____13. Stel ...
... B. High mass inhibits the gravitational force, slowing fusion. C. High mass stars have atomic nuclei “bumping” against each other at rates high enough to trigger a supernova. D. High mass causes stronger gravity, which forces fusion to occur at a faster rate, and they burn out quickly. _____13. Stel ...
Our Universe
... the energy and matter that exists in the universe today. •The Big Bang occurred 13.8 Billion years ago. •Hydrogen and Helium, the makeup of stars, were the first two elements formed in less than a quarter of a second! •The explosion was so enormous, that all objects in the universe are still moving ...
... the energy and matter that exists in the universe today. •The Big Bang occurred 13.8 Billion years ago. •Hydrogen and Helium, the makeup of stars, were the first two elements formed in less than a quarter of a second! •The explosion was so enormous, that all objects in the universe are still moving ...
The origin of elements For life we need some complexity, and
... universe, we said that this didn’t happen because there is no stable element that has eight nucleons. In a star, this is still true, but one can have two helium nuclei come together temporarily, then have a third helium nucleus hit while the first two are somewhat bound. This gives carbon-12, which ...
... universe, we said that this didn’t happen because there is no stable element that has eight nucleons. In a star, this is still true, but one can have two helium nuclei come together temporarily, then have a third helium nucleus hit while the first two are somewhat bound. This gives carbon-12, which ...
When radiation ruled
... Key idea: When the universe was smaller (when the distance between us and some object was smaller), the temperature was hotter. There is no obvious limit to the temperature. Events in the universe’s life, when the universe was smaller & hotter. Production of the first nuclei other than H (3min) ( Re ...
... Key idea: When the universe was smaller (when the distance between us and some object was smaller), the temperature was hotter. There is no obvious limit to the temperature. Events in the universe’s life, when the universe was smaller & hotter. Production of the first nuclei other than H (3min) ( Re ...
RED “O Big Red
... of the Sun aldebaran has only a little more mass than the sun. so why is it so large? ...
... of the Sun aldebaran has only a little more mass than the sun. so why is it so large? ...
2.1c Notes - Vanderbilt University
... The phenomena of x-ray bursts and x-ray pulsars are interpreted as thermonuclear explosions in the accreted hydrogen and/or helium rich layers of neutron stars. These events offer the opportunity to study nucleosynthesis at extreme temperature and density conditions on a time scale of only a few sec ...
... The phenomena of x-ray bursts and x-ray pulsars are interpreted as thermonuclear explosions in the accreted hydrogen and/or helium rich layers of neutron stars. These events offer the opportunity to study nucleosynthesis at extreme temperature and density conditions on a time scale of only a few sec ...
What is a Star?
... was set at a standard distance from Earth. – Astronomers calculate the stars apparent magnitude and it’s distance from Earth. – Then calculate the brightness if it were a standard distance from Earth. ...
... was set at a standard distance from Earth. – Astronomers calculate the stars apparent magnitude and it’s distance from Earth. – Then calculate the brightness if it were a standard distance from Earth. ...
Jupiter-Sized Star Smallest Ever Detected
... from a future space probe approaching such an object at close range, it wouldn't be easy to discern whether it is a star or a planet?" As all stars, OGLE-TR-122b produces indeed energy in its interior by means of nuclear reactions. However, because of its low mass, this internal energy production is ...
... from a future space probe approaching such an object at close range, it wouldn't be easy to discern whether it is a star or a planet?" As all stars, OGLE-TR-122b produces indeed energy in its interior by means of nuclear reactions. However, because of its low mass, this internal energy production is ...
Document
... Notice that the X axis is spaced unevenly, and the number of Kelvins (degrees) between each line is not constant. This because it is a logarithmic scale. For example: each line between 2,000 and 3,000 represents 100 degrees; but each line between 6,000 and 7,000 represents 200 degrees; and differe ...
... Notice that the X axis is spaced unevenly, and the number of Kelvins (degrees) between each line is not constant. This because it is a logarithmic scale. For example: each line between 2,000 and 3,000 represents 100 degrees; but each line between 6,000 and 7,000 represents 200 degrees; and differe ...
The Life Cycle of Stars Webquest
... Date _____________ Continue to read on to the section “The Circle of Life” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. Stars begin their lives as clouds of dust and gas called. 2. What is a protostar? ...
... Date _____________ Continue to read on to the section “The Circle of Life” on the same webpage http://www.seasky.org/cosmic/sky7a01.html and answer the following questions: 1. Stars begin their lives as clouds of dust and gas called. 2. What is a protostar? ...
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.