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- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Astronomy_1e_(OpenStax)/23%3A_The_Death_of_Stars/23.02%3A_Evolution_of_Massive_Stars-_An_Explosive_FinishIn a massive star, hydrogen fusion in the core is followed by several other fusion reactions involving heavier elements. Just before it exhausts all sources of energy, a massive star has an iron core ...In a massive star, hydrogen fusion in the core is followed by several other fusion reactions involving heavier elements. Just before it exhausts all sources of energy, a massive star has an iron core surrounded by shells of silicon, sulfur, oxygen, neon, carbon, helium, and hydrogen. The fusion of iron requires energy (rather than releasing it). If the mass of a star’s iron core exceeds the Chandrasekhar limit (but is less than 3 MSun), the core collapses until its density exceeds that of an ato
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Astronomy_2e_(OpenStax)/23%3A_The_Death_of_Stars/23.05%3A_Pulsars_and_the_Discovery_of_Neutron_StarsAt least some supernovae leave behind a highly magnetic, rapidly rotating neutron star, which can be observed as a pulsar if its beam of escaping particles and focused radiation is pointing toward us....At least some supernovae leave behind a highly magnetic, rapidly rotating neutron star, which can be observed as a pulsar if its beam of escaping particles and focused radiation is pointing toward us. Pulsars emit rapid pulses of radiation at regular intervals; their periods are in the range of 0.001 to 10 seconds. The rotating neutron star acts like a lighthouse, sweeping its beam in a circle and giving us a pulse of radiation when the beam sweeps over Earth. As pulsars age, they lose energy, t
- https://phys.libretexts.org/Bookshelves/University_Physics/University_Physics_(OpenStax)/Book%3A_University_Physics_I_-_Mechanics_Sound_Oscillations_and_Waves_(OpenStax)/13%3A_Gravitation/13.08%3A_Einstein's_Theory_of_GravityAccording to the theory of general relativity, gravity is the result of distortions in space-time created by mass and energy. The principle of equivalence states that that both mass and acceleration d...According to the theory of general relativity, gravity is the result of distortions in space-time created by mass and energy. The principle of equivalence states that that both mass and acceleration distort space-time and are indistinguishable in comparable circumstances. Black holes, the result of gravitational collapse, are singularities with an event horizon that is proportional to their mass.
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Astronomy_1e_(OpenStax)/23%3A_The_Death_of_Stars/23.04%3A_Pulsars_and_the_Discovery_of_Neutron_StarsAt least some supernovae leave behind a highly magnetic, rapidly rotating neutron star, which can be observed as a pulsar if its beam of escaping particles and focused radiation is pointing toward us....At least some supernovae leave behind a highly magnetic, rapidly rotating neutron star, which can be observed as a pulsar if its beam of escaping particles and focused radiation is pointing toward us. Pulsars emit rapid pulses of radiation at regular intervals; their periods are in the range of 0.001 to 10 seconds. The rotating neutron star acts like a lighthouse, sweeping its beam in a circle and giving us a pulse of radiation when the beam sweeps over Earth. As pulsars age, they lose energy, t
- https://phys.libretexts.org/Courses/Prince_Georges_Community_College/General_Physics_I%3A_Classical_Mechanics/54%3A_Gravity/54.09%3A_Black_HolesA star like our Sun exists in a state of equilibrium: its own gravity tries to pull the Sun's mass inward toward the center, but the outward radiation force due to nuclear fusion (which burns hydrogen...A star like our Sun exists in a state of equilibrium: its own gravity tries to pull the Sun's mass inward toward the center, but the outward radiation force due to nuclear fusion (which burns hydrogen fuel to create helium, causing the Sun to shine) is pushing outward. For a bigger star (4-8 up to about 10-15 solar masses), the star's gravity is strong enough to actually collapse the atoms in what would have been a white dwarf at the end of the star's life.
- https://phys.libretexts.org/Bookshelves/Relativity/Spacetime_Physics_(Taylor_and_Wheeler)/09%3A_Gravity_-_Curved_Spacetime_in_Action/9.07%3A_Gravity_WavesAt compressions near the Chandrasekhar limit, the electron gas transforms into a neutron gas, the interior of the star becomes a giant nucleus, and the whole nature of the compact object changes to th...At compressions near the Chandrasekhar limit, the electron gas transforms into a neutron gas, the interior of the star becomes a giant nucleus, and the whole nature of the compact object changes to that of a neutron star.
- https://phys.libretexts.org/Courses/Grossmont_College/ASTR_110%3A_Astronomy_(Fitzgerald)/12%3A_The_Death_of_Stars/12.02%3A_Evolution_of_Massive_Stars-_An_Explosive_FinishIn a massive star, hydrogen fusion in the core is followed by several other fusion reactions involving heavier elements. Just before it exhausts all sources of energy, a massive star has an iron core ...In a massive star, hydrogen fusion in the core is followed by several other fusion reactions involving heavier elements. Just before it exhausts all sources of energy, a massive star has an iron core surrounded by shells of silicon, sulfur, oxygen, neon, carbon, helium, and hydrogen. The fusion of iron requires energy (rather than releasing it). If the mass of a star’s iron core exceeds the Chandrasekhar limit (but is less than 3 \(M_{\text{Sun}}\)), the core collapses.
- https://phys.libretexts.org/Courses/Grossmont_College/ASTR_110%3A_Astronomy_(Fitzgerald)/12%3A_The_Death_of_Stars/12.04%3A_Pulsars_and_the_Discovery_of_Neutron_StarsAt least some supernovae leave behind a highly magnetic, rapidly rotating neutron star, which can be observed as a pulsar if its beam of escaping particles and focused radiation is pointing toward us....At least some supernovae leave behind a highly magnetic, rapidly rotating neutron star, which can be observed as a pulsar if its beam of escaping particles and focused radiation is pointing toward us. Pulsars emit rapid pulses of radiation at regular intervals; their periods are in the range of 0.001 to 10 seconds. The rotating neutron star acts like a lighthouse, sweeping its beam in a circle and giving us a pulse of radiation when the beam sweeps over Earth.
- https://phys.libretexts.org/Courses/Muhlenberg_College/MC%3A_Physics_121_-_General_Physics_I/13%3A_Gravitation/13.08%3A_Einstein's_Theory_of_GravityAccording to the theory of general relativity, gravity is the result of distortions in space-time created by mass and energy. The principle of equivalence states that that both mass and acceleration d...According to the theory of general relativity, gravity is the result of distortions in space-time created by mass and energy. The principle of equivalence states that that both mass and acceleration distort space-time and are indistinguishable in comparable circumstances. Black holes, the result of gravitational collapse, are singularities with an event horizon that is proportional to their mass.
- https://phys.libretexts.org/Workbench/PH_245_Textbook_V2/13%3A_Gravitation/13.08%3A_Einstein's_Theory_of_GravityAccording to the theory of general relativity, gravity is the result of distortions in space-time created by mass and energy. The principle of equivalence states that that both mass and acceleration d...According to the theory of general relativity, gravity is the result of distortions in space-time created by mass and energy. The principle of equivalence states that that both mass and acceleration distort space-time and are indistinguishable in comparable circumstances. Black holes, the result of gravitational collapse, are singularities with an event horizon that is proportional to their mass.
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Astronomy_2e_(OpenStax)/23%3A_The_Death_of_Stars/23.03%3A_Evolution_of_Massive_Stars-_An_Explosive_FinishIn a massive star, hydrogen fusion in the core is followed by several other fusion reactions involving heavier elements. Just before it exhausts all sources of energy, a massive star has an iron core ...In a massive star, hydrogen fusion in the core is followed by several other fusion reactions involving heavier elements. Just before it exhausts all sources of energy, a massive star has an iron core surrounded by shells of silicon, sulfur, oxygen, neon, carbon, helium, and hydrogen. The fusion of iron requires energy (rather than releasing it). If the mass of a star’s iron core exceeds the Chandrasekhar limit (but is less than 3 MSun), the core collapses until its density exceeds that of an ato
