the lab handout here
... How does the temperature and luminosity of the Sun compare to that of the other stars on the Main Sequence? ________________________________________________________ ...
... How does the temperature and luminosity of the Sun compare to that of the other stars on the Main Sequence? ________________________________________________________ ...
No Slide Title
... The neutron star may continue to gain mass from nearby stars. At a critical moment, it becomes so dense it collapses in on itself, becoming a single point of zero size! Its gravity is so strong that even light cannot escape from inside a certain boundary - the EVENT HORIZON. The star is now a BLACK ...
... The neutron star may continue to gain mass from nearby stars. At a critical moment, it becomes so dense it collapses in on itself, becoming a single point of zero size! Its gravity is so strong that even light cannot escape from inside a certain boundary - the EVENT HORIZON. The star is now a BLACK ...
Life Cycles of Stars
... • Depending on the size of the star that forms, a different fate is met • Low and medium mass stars burn out to become white dwarfs • High mass stars burn out in an amazing explosion called a supernova, which gives birth to a new ...
... • Depending on the size of the star that forms, a different fate is met • Low and medium mass stars burn out to become white dwarfs • High mass stars burn out in an amazing explosion called a supernova, which gives birth to a new ...
Document
... Stage 4 (low mass) A star like our Sun will contract, becoming a white dwarf, which slowly cools, changing color as it does, until it can no longer be seen a black dwarf. ...
... Stage 4 (low mass) A star like our Sun will contract, becoming a white dwarf, which slowly cools, changing color as it does, until it can no longer be seen a black dwarf. ...
Powerpoint Presentation (large file)
... main-sequence star • This leaves a core of nearly pure helium surrounded by a shell through which hydrogen fusion works its way outward in the star • The core shrinks and becomes hotter, while the star’s outer layers expand and cool • The result is a red giant star ...
... main-sequence star • This leaves a core of nearly pure helium surrounded by a shell through which hydrogen fusion works its way outward in the star • The core shrinks and becomes hotter, while the star’s outer layers expand and cool • The result is a red giant star ...
Chapter 20 Review of Stars` Lifetime Review
... • None have been detected that have formed this way • Some have been found in binary systems ...
... • None have been detected that have formed this way • Some have been found in binary systems ...
Review Quiz No. 17
... The radius in the interior of a star where fusion processes can no longer take place. The point in time of a star’s life when nuclear fusion of hydrogen into helium ceases. The point in time of a star’s life when nuclear fusion processes cease alltogether. The point in a rotating star cluster beyond ...
... The radius in the interior of a star where fusion processes can no longer take place. The point in time of a star’s life when nuclear fusion of hydrogen into helium ceases. The point in time of a star’s life when nuclear fusion processes cease alltogether. The point in a rotating star cluster beyond ...
Document
... a) It generates more heat and its core eventually collapses. b) It cannot fuse elements heavier than carbon. c) Gravity is weakened by its high luminosity. d) It is most often found as part of a binary system. 22. What is a planetary nebula? a) A planet surrounded by a glowing shell of gas. b) The d ...
... a) It generates more heat and its core eventually collapses. b) It cannot fuse elements heavier than carbon. c) Gravity is weakened by its high luminosity. d) It is most often found as part of a binary system. 22. What is a planetary nebula? a) A planet surrounded by a glowing shell of gas. b) The d ...
Mark scheme for Support Worksheet – Topic E, Worksheet 1
... A constellation is a collection of stars usually in a recognisable pattern that are not necessarily physically close to each other; whereas a stellar cluster consists of stars that are close to each other and attract each other gravitationally. ...
... A constellation is a collection of stars usually in a recognisable pattern that are not necessarily physically close to each other; whereas a stellar cluster consists of stars that are close to each other and attract each other gravitationally. ...
Universe CBA Review - cms16-17
... 33.) What type of EMS wave has the longest wavelength? _____________________ 34.) Does infrared or x-ray waves have a longer wavelength? __________________ 35.) What type of wave has the highest frequency in the EMS? __________________ 36.) Draw and label the visible light spectrum ...
... 33.) What type of EMS wave has the longest wavelength? _____________________ 34.) Does infrared or x-ray waves have a longer wavelength? __________________ 35.) What type of wave has the highest frequency in the EMS? __________________ 36.) Draw and label the visible light spectrum ...
ISP 205 Review Questions, Week 10
... Why don’t all of the pieces just pull themselves together into an infinitesimally small clump at the center? ...
... Why don’t all of the pieces just pull themselves together into an infinitesimally small clump at the center? ...
Chapter 28 Notes
... Because of Earth’s movement around the sun Apparent Magnitude – What is it? How bright a star appears to be to an observer on Earth. ...
... Because of Earth’s movement around the sun Apparent Magnitude – What is it? How bright a star appears to be to an observer on Earth. ...
What is a supernova - University of Warwick
... Its temperature rises high enough to fuse carbon into oxygen, neon, silicon, sulphur and eventually iron! ...
... Its temperature rises high enough to fuse carbon into oxygen, neon, silicon, sulphur and eventually iron! ...
Stellar Evolution
... Often asymmetric, possibly due to • Stellar rotation • Magnetic fields • Dust disks around the stars ...
... Often asymmetric, possibly due to • Stellar rotation • Magnetic fields • Dust disks around the stars ...
Information (Word Doc)
... collapse. The core temperature rises to over 100 billion degrees as the iron atoms are crushed together. The repulsive force between the nuclei overcomes the force of gravity, and the core recoils out from the heart of the star in an explosive shock wave.. In one of the most spectacular events in th ...
... collapse. The core temperature rises to over 100 billion degrees as the iron atoms are crushed together. The repulsive force between the nuclei overcomes the force of gravity, and the core recoils out from the heart of the star in an explosive shock wave.. In one of the most spectacular events in th ...
eta carinae – nature`s own hadron collider
... ETA CARINAE IS ONE OF THE MOST MASSIVE STARS KNOWN. IT IS AROUND 100 SOLAR MASSES. THE UPPER LIMIT OF STAR SIZE IS THOUGHT TO BE AROUND 150 SOLAR MASSES. BECAUSE OF ITS SIZE, AND THE HIGH ENERGIES PRODUCED BECAUSE OF GRAVITY, IT IS UNSTABLE. ...
... ETA CARINAE IS ONE OF THE MOST MASSIVE STARS KNOWN. IT IS AROUND 100 SOLAR MASSES. THE UPPER LIMIT OF STAR SIZE IS THOUGHT TO BE AROUND 150 SOLAR MASSES. BECAUSE OF ITS SIZE, AND THE HIGH ENERGIES PRODUCED BECAUSE OF GRAVITY, IT IS UNSTABLE. ...
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.