Solar
... nuclei to fuse together to form one helium nucleus • The difference in mass is expelled as energy • It is carried to the Sun’s surface by radiation and convection and is released primarily in the form of electromagnetic radiation (i.e. light) • Energy produced in the core takes a million years to re ...
... nuclei to fuse together to form one helium nucleus • The difference in mass is expelled as energy • It is carried to the Sun’s surface by radiation and convection and is released primarily in the form of electromagnetic radiation (i.e. light) • Energy produced in the core takes a million years to re ...
neutron star - The University of Chicago
... At peak luminosity a typical Type II supernova can be as bright as 1 billion of suns ...
... At peak luminosity a typical Type II supernova can be as bright as 1 billion of suns ...
Different wavelengths…
... The amount of energy created in this process can be calculated by the famous equation above. What does it mean? Matter is changed into energy during fusion The amount of energy created when you change matter to energy is equal to the mass of the matter converted times the speed of light constant ...
... The amount of energy created in this process can be calculated by the famous equation above. What does it mean? Matter is changed into energy during fusion The amount of energy created when you change matter to energy is equal to the mass of the matter converted times the speed of light constant ...
© Space Explorers, Inc.
... The Sun is at the center of our solar system and contains 99% of all the matter in the solar system. It is a glowing sphere of gas that gives off light, heat and energy. Mercury is the closest planet to the sun, so it’s surface temperature is very hot (332 degrees!) Mercury has almost no atmosphere ...
... The Sun is at the center of our solar system and contains 99% of all the matter in the solar system. It is a glowing sphere of gas that gives off light, heat and energy. Mercury is the closest planet to the sun, so it’s surface temperature is very hot (332 degrees!) Mercury has almost no atmosphere ...
Main Sequence Stars
... • The idea of the “Vogt-Russell” theorem for stars is that there is only one way to make a star with a given mass and chemical composition – if we start with a just formed protostar of a given mass and chemical composition, we can calculate how that star will evolve over its entire life. • This is e ...
... • The idea of the “Vogt-Russell” theorem for stars is that there is only one way to make a star with a given mass and chemical composition – if we start with a just formed protostar of a given mass and chemical composition, we can calculate how that star will evolve over its entire life. • This is e ...
The Life Cycles of Stars
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
... supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive star that has 8 or more times the mass of our Sun remains massive after the supernova. No nuclear fusion is t ...
Famous Astronomers
... planets orbit the sun and moons orbit planets. It is gravity that keeps an object in orbit!” 2) “The Earth is the center of the universe, and all of the planets and stars orbit our planet. How do I know? Well, my theory includes an intricate system of orbits within orbits that explains the motion of ...
... planets orbit the sun and moons orbit planets. It is gravity that keeps an object in orbit!” 2) “The Earth is the center of the universe, and all of the planets and stars orbit our planet. How do I know? Well, my theory includes an intricate system of orbits within orbits that explains the motion of ...
The Sun
... lower flux of neutrinos than expected ( the “solar neutrino problem”). Recent results have proven that neutrinos change (“oscillate”) between different types (“flavors”), thus solving the solar neutrino problem. ...
... lower flux of neutrinos than expected ( the “solar neutrino problem”). Recent results have proven that neutrinos change (“oscillate”) between different types (“flavors”), thus solving the solar neutrino problem. ...
Chapter 08
... Energy gain = Dm*c2 = 0.43*10-11 J per reaction. Sun needs 1038 reactions, transforming 5 million tons of mass into energy every second, to resist its own gravity. ...
... Energy gain = Dm*c2 = 0.43*10-11 J per reaction. Sun needs 1038 reactions, transforming 5 million tons of mass into energy every second, to resist its own gravity. ...
Quick and Easy Activities and Demonstrations for Astronomy
... 1- using a lamp or other light source, have a student sit on a swivel chair a few m in front of the light.(have the room light off) have another student or teacher, walk around student with a ball(the bigger the better) cutting in front of the light. Stop at various points and get the student to des ...
... 1- using a lamp or other light source, have a student sit on a swivel chair a few m in front of the light.(have the room light off) have another student or teacher, walk around student with a ball(the bigger the better) cutting in front of the light. Stop at various points and get the student to des ...
Space Test Explanations
... 11. As a new star is born, what type of atoms first begin to fuse? Hydrogen 12. Which type of new atoms are created when these first atoms fuse? Helium 13. Why are some stars red giants? In these stars, a lot of hydrogen has already fused. This fusion creates helium, which is more dense than hydroge ...
... 11. As a new star is born, what type of atoms first begin to fuse? Hydrogen 12. Which type of new atoms are created when these first atoms fuse? Helium 13. Why are some stars red giants? In these stars, a lot of hydrogen has already fused. This fusion creates helium, which is more dense than hydroge ...
xam2ans
... (c) Consider this weak reaction: p+ + e → n + e . Why does it almost never occur in the core of a main sequence star like the Sun? Answer: The rest mass energy of a neutron is larger than a proton plus electron. Consequently this reaction is endothermic, which means energetically unfavorable. (d) ...
... (c) Consider this weak reaction: p+ + e → n + e . Why does it almost never occur in the core of a main sequence star like the Sun? Answer: The rest mass energy of a neutron is larger than a proton plus electron. Consequently this reaction is endothermic, which means energetically unfavorable. (d) ...
