Lecture20 - University of Waterloo
... The geometry of the Universe • It has been known since the 1930s that the Universe is expanding: more distant galaxies are moving away from us more quickly. • By comparing the distance of the supernova to their redshift (recession velocity) we can measure not only the velocity of this expansion, bu ...
... The geometry of the Universe • It has been known since the 1930s that the Universe is expanding: more distant galaxies are moving away from us more quickly. • By comparing the distance of the supernova to their redshift (recession velocity) we can measure not only the velocity of this expansion, bu ...
The universe - Villanova University
... Stuff like iron, nickel, uranium comes from the destruction (explosion) of stars. ...
... Stuff like iron, nickel, uranium comes from the destruction (explosion) of stars. ...
Star Formation 1/18/2015
... (and just about as exciting for them as for us) What do MS stars do? Why are more stars on the MS than anywhere else? Are they happy? What sort of retirement plan do they have? ...
... (and just about as exciting for them as for us) What do MS stars do? Why are more stars on the MS than anywhere else? Are they happy? What sort of retirement plan do they have? ...
powerpoint - Physics @ IUPUI
... Helium in a shell outside of the core. Is it considered a Main Sequence Star? ...
... Helium in a shell outside of the core. Is it considered a Main Sequence Star? ...
ASTRONOMY 12 Problem Set 4 – Due March 10, 2016 1) After
... NB. The neutron star actually weighs significantly less than the iron core that collapsed to it. The difference is radiated away as neutrinos. This is another example of binding energy, in this case gravity, reducing the effective mass of the system. Other examples are nuclei (mass reduced by nuclea ...
... NB. The neutron star actually weighs significantly less than the iron core that collapsed to it. The difference is radiated away as neutrinos. This is another example of binding energy, in this case gravity, reducing the effective mass of the system. Other examples are nuclei (mass reduced by nuclea ...
Everything Under and Over The Stars
... than our star and two to four times hotter. Being very large, they use their fuel quickly and only have a life span of one million years. Every blue giant turns into a black hole because the neutrons cannot repel such a tremendous mass when it collapses. ...
... than our star and two to four times hotter. Being very large, they use their fuel quickly and only have a life span of one million years. Every blue giant turns into a black hole because the neutrons cannot repel such a tremendous mass when it collapses. ...
A Summary of Stages
... energy output, the hot core begins to contract, which raises the temperature all through the inside of the star, and it begins hydrogen shell-burning, actually producing more energy than ever before. The outer envelope of the star begins to slowly expand and the star "leaves" the Main Sequence regio ...
... energy output, the hot core begins to contract, which raises the temperature all through the inside of the star, and it begins hydrogen shell-burning, actually producing more energy than ever before. The outer envelope of the star begins to slowly expand and the star "leaves" the Main Sequence regio ...
Twinkle, Twinkle, Little Star
... The brightness of a star depends on both the size and temperature of the star. But, how bright it APPEARS to us depends on how far it is from Earth and how bright it truly is. ...
... The brightness of a star depends on both the size and temperature of the star. But, how bright it APPEARS to us depends on how far it is from Earth and how bright it truly is. ...
–1– Order of Magnitude Astrophysics
... An interesting phenomenon arises if the maximum temperature T max is sufficiently high to trigger nuclear fusion in the system; then we obtain a gravitationally bound, self-sustained nuclear reactor. The condition for triggering nuclear reaction occurs at energy scales higher than εnucl ≈ ηα2 m p c2 ...
... An interesting phenomenon arises if the maximum temperature T max is sufficiently high to trigger nuclear fusion in the system; then we obtain a gravitationally bound, self-sustained nuclear reactor. The condition for triggering nuclear reaction occurs at energy scales higher than εnucl ≈ ηα2 m p c2 ...
Lecture 19 - Stellar Lifecycles
... • When a star uses up the Hydrogen in its core it can no longer support itself against gravity. • The core compresses and temperatures begin to rise. • Temperatures may get high enough outside the core to begin The life cycle of a star like the Sun Hydrogen fusion there instead. • The pressure from ...
... • When a star uses up the Hydrogen in its core it can no longer support itself against gravity. • The core compresses and temperatures begin to rise. • Temperatures may get high enough outside the core to begin The life cycle of a star like the Sun Hydrogen fusion there instead. • The pressure from ...
The Fate of Massive Stars
... •Classification by Spectral Lines and Light Curve Shape •Brightness to rival entire galaxies •What is happening? ...
... •Classification by Spectral Lines and Light Curve Shape •Brightness to rival entire galaxies •What is happening? ...
The Hidden Lives of Galaxies NSTA 2001
... Energy sustains the expanded outer layers of the Red Giant ...
... Energy sustains the expanded outer layers of the Red Giant ...
life cycle of stars
... After Helium is exhausted, outer layers of star are expelled Planetary Nebulae ...
... After Helium is exhausted, outer layers of star are expelled Planetary Nebulae ...
The Life of a Star
... a red super giant. After this stage things become more violent. Instead of gentle billowing gas shells being ejected into space (a planetary nebula) the red super giant tears itself apart in an unbelievably violent explosion called a supernova. As the radiation and debris clear, a neutron star emerg ...
... a red super giant. After this stage things become more violent. Instead of gentle billowing gas shells being ejected into space (a planetary nebula) the red super giant tears itself apart in an unbelievably violent explosion called a supernova. As the radiation and debris clear, a neutron star emerg ...
Chapter 25 Study guide Answer Key
... What color is the most massive type of main sequence star? The least massive? Blue = Most massive Red = Least ...
... What color is the most massive type of main sequence star? The least massive? Blue = Most massive Red = Least ...
Click here - Noadswood Science
... cycle of stars. • Everyone makes their own. • There are 3 possible life cycles. In your group make sure that you are showing all 3 lifecycles. ...
... cycle of stars. • Everyone makes their own. • There are 3 possible life cycles. In your group make sure that you are showing all 3 lifecycles. ...
Low Mass
... – force of electrons around atoms keeps from collapse (no energy is produced). This force originates from the Pauli Exclusion Principle – core temperature never reaches the 600 million K required to burn carbon or oxygen, so core fusion ends. ...
... – force of electrons around atoms keeps from collapse (no energy is produced). This force originates from the Pauli Exclusion Principle – core temperature never reaches the 600 million K required to burn carbon or oxygen, so core fusion ends. ...
STARS- hot glowing sphere of gas that produces energy by
... STAR- hot glowing sphere of gas that produces energy by fusion 1] Light year—distance light travels in a year (9.5 trillion km, 6 trillion miles) 2] Star brightness A) Actual brightness- brightness right next to a star B) Apparent brightness—brightness as seen from earth 3] Formation of stars A) Neb ...
... STAR- hot glowing sphere of gas that produces energy by fusion 1] Light year—distance light travels in a year (9.5 trillion km, 6 trillion miles) 2] Star brightness A) Actual brightness- brightness right next to a star B) Apparent brightness—brightness as seen from earth 3] Formation of stars A) Neb ...
12.4 Evolution of Stars More Massive than the Sun
... expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows off, leaving a white dwarf to gradually cool. • Nova results from material accreting onto a white dwarf from a companion star ...
... expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows off, leaving a white dwarf to gradually cool. • Nova results from material accreting onto a white dwarf from a companion star ...
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.