Lecture 16: Iron Core Collapse, Neutron Stars
... 15 solar masses. The shock is born near 0.7 solar masses. Initially the bounce gives it positive kinetic energy, but for each 0.1 solar masses it traverses and photodisintegrates about 1051 erg of energy is lost. Additional energy is lost to neutrinos as the shock moves to low densities, ...
... 15 solar masses. The shock is born near 0.7 solar masses. Initially the bounce gives it positive kinetic energy, but for each 0.1 solar masses it traverses and photodisintegrates about 1051 erg of energy is lost. Additional energy is lost to neutrinos as the shock moves to low densities, ...
Semester 1 Earth Science Gallery Review
... 5. What temperature is Sirius B? 6. This star is a red Giant. 7. What temperature is Bernard’s Star? 8. Which star is the dimmest (least bright) on the chart? 9. What category is the hottest star on the chart? 10. What color are the coolest stars? 11. What category of stars is hot but not very lumin ...
... 5. What temperature is Sirius B? 6. This star is a red Giant. 7. What temperature is Bernard’s Star? 8. Which star is the dimmest (least bright) on the chart? 9. What category is the hottest star on the chart? 10. What color are the coolest stars? 11. What category of stars is hot but not very lumin ...
Astronomy 101 Course Review and Summary
... Newton’s Laws Three Laws of Motion: (1)An object remains at rest, or moves in a straight line at constant speed, unless acted on by an outside force. (2) The acceleration of an object is directly proportional to force, and inversely proportional to mass. (3) For every action, there is an equal and ...
... Newton’s Laws Three Laws of Motion: (1)An object remains at rest, or moves in a straight line at constant speed, unless acted on by an outside force. (2) The acceleration of an object is directly proportional to force, and inversely proportional to mass. (3) For every action, there is an equal and ...
PHYS3380_111115_bw - The University of Texas at Dallas
... into its final stages of evolution; at this time the star is AGB star characterized by a carbon-oxygen core, surrounded by a helium burning shell and a hydrogen burning shell. • For stars whose mass is greater than 2.25 M, the electrons in their cores are not degenerate at the time of helium igniti ...
... into its final stages of evolution; at this time the star is AGB star characterized by a carbon-oxygen core, surrounded by a helium burning shell and a hydrogen burning shell. • For stars whose mass is greater than 2.25 M, the electrons in their cores are not degenerate at the time of helium igniti ...
The “Tuning Fork” Diagram Galaxy Properties 1 “Early”
... • Applied to nuclei of spirals Î presence of massive black holes • Also often applied to ...
... • Applied to nuclei of spirals Î presence of massive black holes • Also often applied to ...
1 - TeacherWeb
... 39. Most stars are in the “main sequence” of their life cycle and burn for billions of years. Why don’t stars in the main sequence either explode right away or become crushed by their own gravity? ...
... 39. Most stars are in the “main sequence” of their life cycle and burn for billions of years. Why don’t stars in the main sequence either explode right away or become crushed by their own gravity? ...
Alien Earths Floorplan (3,000 sq. ft) Major Exhibit Areas
... and have very long lifetimes: there is time enough for life to evolve around them. Their dimmer light sometimes makes observations more challenging. ...
... and have very long lifetimes: there is time enough for life to evolve around them. Their dimmer light sometimes makes observations more challenging. ...
Chapter 7 Neutron Stars - Ira-Inaf
... gravitational potential energy of an electron at the surface of such a star would be less than 0.1% its rest mass energy. This tells us that general relativistic effects are not important to white dwarf physics. 7.2 Neutron stars The above discussion points out the the final state of a star that has ...
... gravitational potential energy of an electron at the surface of such a star would be less than 0.1% its rest mass energy. This tells us that general relativistic effects are not important to white dwarf physics. 7.2 Neutron stars The above discussion points out the the final state of a star that has ...
Universal Gravitation Worksheet
... (2) A mass m is placed at the center of a thin, hollow, spherical shell of mass M and radius R. (diagram 1) (a) What gravitational force does the mass m experience? (b) What gravitational force does m exert on M? (c) A second mass m is now placed a distance 2R from the center of the shell. (Diagram ...
... (2) A mass m is placed at the center of a thin, hollow, spherical shell of mass M and radius R. (diagram 1) (a) What gravitational force does the mass m experience? (b) What gravitational force does m exert on M? (c) A second mass m is now placed a distance 2R from the center of the shell. (Diagram ...
Supernovae — Oct 21 10/21/2011 • Outline
... several degrees SE of Thien-kuan. After more than a year it gradually became invisible.p550. ...
... several degrees SE of Thien-kuan. After more than a year it gradually became invisible.p550. ...
After Dark in Allenspark
... that with binoculars, you can see Jupiter's four moons strung out in a line near Jupiter, and that Alpha Libra is a double. I've never tried, but this sounds like a good time for it. If anyone else tries, let me know how it goes. January 14: Full moon. January 17: The first day we can try launching ...
... that with binoculars, you can see Jupiter's four moons strung out in a line near Jupiter, and that Alpha Libra is a double. I've never tried, but this sounds like a good time for it. If anyone else tries, let me know how it goes. January 14: Full moon. January 17: The first day we can try launching ...
PPT Format - HubbleSOURCE
... a system of two objects in space (usually stars), which are so close that their gravitational interaction causes them to orbit around their common center of mass. ...
... a system of two objects in space (usually stars), which are so close that their gravitational interaction causes them to orbit around their common center of mass. ...
Luminosity Classes
... They are smaller and dimmer than Cepheids and their luminosities are all nearly the same making them also good for finding stellar distances Irregular Variables have inconsistent periods and are usually very young and very old stars. ...
... They are smaller and dimmer than Cepheids and their luminosities are all nearly the same making them also good for finding stellar distances Irregular Variables have inconsistent periods and are usually very young and very old stars. ...
The Temperatures of Stars
... the Harvard “computers” to record the spectra of nearly 1 million stars and classify each. A spectrum is the range of colors emitted by an object that contains information on the object’s temperature, chemical composition, or motion. The Draper Catalog provided a wealth of data that would reveal muc ...
... the Harvard “computers” to record the spectra of nearly 1 million stars and classify each. A spectrum is the range of colors emitted by an object that contains information on the object’s temperature, chemical composition, or motion. The Draper Catalog provided a wealth of data that would reveal muc ...
bright - TutorPlus
... The Hertzsprung-Russell (H-R) Diagram • Between 1911 and 1913, two astronomers – one Danish (Ejnar Hertzsprung) and one American (Henry Russell) – independently developed a diagram to show the relationship between the luminosity or absolute magnitude of a star and its surface temperature as deduced ...
... The Hertzsprung-Russell (H-R) Diagram • Between 1911 and 1913, two astronomers – one Danish (Ejnar Hertzsprung) and one American (Henry Russell) – independently developed a diagram to show the relationship between the luminosity or absolute magnitude of a star and its surface temperature as deduced ...
File - Adopt A Constellation
... • Constellations - A pattern or group of stars in the sky that humans observe in a pattern and give a name. • People of ancient time saw the constellations as character or animals in the sky. They made up stories to explain how the object, animal, or character came into the night sky • Earth rotate ...
... • Constellations - A pattern or group of stars in the sky that humans observe in a pattern and give a name. • People of ancient time saw the constellations as character or animals in the sky. They made up stories to explain how the object, animal, or character came into the night sky • Earth rotate ...
Stellarium is a simple and easy way to look at the
... years – and show what positio the stars were or are going to b in. ...
... years – and show what positio the stars were or are going to b in. ...
11 Stellar Remnants - Journigan-wiki
... carbon and oxygen with a thin surface layer of hydrogen and helium. There is far too little gas to ever combust, however. White dwarfs simply continue to cool and reach a core temperature of around 20,000 K. ...
... carbon and oxygen with a thin surface layer of hydrogen and helium. There is far too little gas to ever combust, however. White dwarfs simply continue to cool and reach a core temperature of around 20,000 K. ...
The First Stars - Amazon Web Services
... In the century that followed, astronomers measured the masses of many stars, typically by using the orbits in binary systems, and confirmed Eddington’s reasoning. The smaller balls of gas make the planets. The massive stars explode, after exhausting their nuclear fuel, because their masses are so la ...
... In the century that followed, astronomers measured the masses of many stars, typically by using the orbits in binary systems, and confirmed Eddington’s reasoning. The smaller balls of gas make the planets. The massive stars explode, after exhausting their nuclear fuel, because their masses are so la ...
Powerpoint of lecture 3
... and constant volume, we can find (see blackboard) an integral expression for the total internal energy, U. • Using Theorem II, if is constant throughout the star, we can then prove the Virial Theorem: ...
... and constant volume, we can find (see blackboard) an integral expression for the total internal energy, U. • Using Theorem II, if is constant throughout the star, we can then prove the Virial Theorem: ...
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.