Vocabulary Review
... a gigantic explosion in which a massive star collapses and throws its outer layers into space ...
... a gigantic explosion in which a massive star collapses and throws its outer layers into space ...
Lecture 15: The Main Sequence
... High-Mass M-S stars have short M-S lifetimes Low-Mass M-S stars have long M-S lifetimes More massive main-sequence stars need higher pressures to support themselves against gravitational collapse. Higher pressure=higher temperatures. The higher temperatures lead to greater rates of nuclear fusion wh ...
... High-Mass M-S stars have short M-S lifetimes Low-Mass M-S stars have long M-S lifetimes More massive main-sequence stars need higher pressures to support themselves against gravitational collapse. Higher pressure=higher temperatures. The higher temperatures lead to greater rates of nuclear fusion wh ...
Learning Objectives Weeks 9-11 . 1. Know that star birth can begin
... Novae and thermonuclear supernovae both occur in close binary systems with a white dwarf, but a while a nova can recur a supernova is a one-shot event. 17. Like a white dwarf, a neutron star has an upper limit on its mass. For a neutron star to collapse, gravity must overwhelm both degeneracy pressu ...
... Novae and thermonuclear supernovae both occur in close binary systems with a white dwarf, but a while a nova can recur a supernova is a one-shot event. 17. Like a white dwarf, a neutron star has an upper limit on its mass. For a neutron star to collapse, gravity must overwhelm both degeneracy pressu ...
Stars & Galaxies
... The gravity of this mass is so strong that the gas is pulled inward, packing it into a smaller and smaller space. ...
... The gravity of this mass is so strong that the gas is pulled inward, packing it into a smaller and smaller space. ...
INV 12B MOTION WITH CHANGING SPEED DRY LAB DATA
... h. space object that causes craters i. the force that exists between any two bodies in the universe j. process that developed the three layers of Earth and Moon’s interior k. a large cloud of gas and dust in space where stars are born l. the time in the life of a star when it generates energy by fus ...
... h. space object that causes craters i. the force that exists between any two bodies in the universe j. process that developed the three layers of Earth and Moon’s interior k. a large cloud of gas and dust in space where stars are born l. the time in the life of a star when it generates energy by fus ...
Locating Objects in Space
... Ranges from 1st – 6th magnitude, 1st is 100 times brighter than 6th Difference of 1 magnitude corresponds to a factor of 2.512 in brightness Does not take into account the distance of the star ...
... Ranges from 1st – 6th magnitude, 1st is 100 times brighter than 6th Difference of 1 magnitude corresponds to a factor of 2.512 in brightness Does not take into account the distance of the star ...
Star Cycle2013
... gravity pressure causes fusion reactions to occur quickly __________. This causes the largest stars to burn their fuel, and eventually run out, much more ______________. quickly ...
... gravity pressure causes fusion reactions to occur quickly __________. This causes the largest stars to burn their fuel, and eventually run out, much more ______________. quickly ...
AnwerkeyTypes-of-stars-and-HR-diagram
... 2. How does surface temperature of White dwarf compares to red giants? __________________Higher______ 3. What is color of stars with highest Surface Temperature? ____________blue____________ 4. What is color of stars with lowest Surface Temperature? _______________Red_________ 5. List the colors fro ...
... 2. How does surface temperature of White dwarf compares to red giants? __________________Higher______ 3. What is color of stars with highest Surface Temperature? ____________blue____________ 4. What is color of stars with lowest Surface Temperature? _______________Red_________ 5. List the colors fro ...
Birth and Death of Stars
... energy to the outer shell of hydrogen which allows fusion to continue. This ongoing fusion radiates energy outward and the outer shell expands and cools creating a red supergiant. ...
... energy to the outer shell of hydrogen which allows fusion to continue. This ongoing fusion radiates energy outward and the outer shell expands and cools creating a red supergiant. ...
Astronomy Objectives
... Evolution of low mass (red dwarf) stars, medium mass main sequence stars, massive stars, all from nebulae to their final phases ...
... Evolution of low mass (red dwarf) stars, medium mass main sequence stars, massive stars, all from nebulae to their final phases ...
Astro 10: Introductory Astronomy
... to arrive at ideas, and to test them to arrive at our current theories of the Universe. Exams will stress getting a picture of processes and the ‘why’ behind what we see, not so much on memorized factoids. ...
... to arrive at ideas, and to test them to arrive at our current theories of the Universe. Exams will stress getting a picture of processes and the ‘why’ behind what we see, not so much on memorized factoids. ...
Chapter 20 Notes (smaller PDF file)
... which its core collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, moving ...
... which its core collapses and most of its matter is ejected into space at high speeds • The luminosity of the star increases suddenly by a factor of around 108 during this explosion, producing a supernova • The matter ejected from the supernova, moving ...
large PDF file
... red-giant stages • A low-mass star becomes – a red giant when shell hydrogen fusion begins – a horizontal-branch star when core helium fusion begins – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion ...
... red-giant stages • A low-mass star becomes – a red giant when shell hydrogen fusion begins – a horizontal-branch star when core helium fusion begins – an asymptotic giant branch (AGB) star when the helium in the core is exhausted and shell helium fusion ...
Brock physics - Brock University
... (c) * matter from a nearby star falling onto the surface of a white dwarf, becoming compressed and heated, and eventually resulting in an explosion. (d) matter from a nearby star falling onto the surface of a neutron star, becoming compressed and heated, and eventually resulting in an explosion. 28. ...
... (c) * matter from a nearby star falling onto the surface of a white dwarf, becoming compressed and heated, and eventually resulting in an explosion. (d) matter from a nearby star falling onto the surface of a neutron star, becoming compressed and heated, and eventually resulting in an explosion. 28. ...
The Birth, Life, and Death of Stars
... Born in Ulm, Germany in 1879 and died in Princeton in 1955 Questions the basic tenets of Quantum Mechanics: God does not play dice with the Universe ... Yet, is awarded the 1921 Nobel Prize in Physics: ... for his discovery of the law of the photoelectric effect 1905 Einstein’s Miracle Year while wo ...
... Born in Ulm, Germany in 1879 and died in Princeton in 1955 Questions the basic tenets of Quantum Mechanics: God does not play dice with the Universe ... Yet, is awarded the 1921 Nobel Prize in Physics: ... for his discovery of the law of the photoelectric effect 1905 Einstein’s Miracle Year while wo ...
updated
... As the helium core turns to carbon, the star once again finds itself in a state where the core temperature is too cool to fuse carbon. The core then collapses and heats in the same manner as occurred when core hydrogen was exhausted. ...
... As the helium core turns to carbon, the star once again finds itself in a state where the core temperature is too cool to fuse carbon. The core then collapses and heats in the same manner as occurred when core hydrogen was exhausted. ...
Fusion - School
... demonstrate an understanding that the Sun’s energy is generated by nuclear fusion reactions at its core, converting hydrogen into helium ...
... demonstrate an understanding that the Sun’s energy is generated by nuclear fusion reactions at its core, converting hydrogen into helium ...
Chapter 21
... Discover Activity-Parallax Notes Classifying Stars Stars are classified by: Color and Temperature What color stars are the hottest? _____________ Coolest? ______________ Size The sun is a medium-sized star. Stars that are much larger than the sun are called ______________ or __________________. ...
... Discover Activity-Parallax Notes Classifying Stars Stars are classified by: Color and Temperature What color stars are the hottest? _____________ Coolest? ______________ Size The sun is a medium-sized star. Stars that are much larger than the sun are called ______________ or __________________. ...
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.