Chandrasekhar Limit - Astrophysics

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This limit, approximately 1.4 times the mass of the Sun, was first calculated by Indian astrophysicist <a href="https://theastrophysics.com/about/index/subrahmanyan-chandrasekhar" title="Subrahmanyan Chandrasekhar" target="_blank">Subrahmanyan Chandrasekhar</a> in 1930. Beyond this mass, white dwarfs are unable to support themselves against gravitational collapse due to the electron degeneracy pressure, leading to further gravitational collapse into a neutron star or a black hole.</div><div><a href="https://theastrophysics.com/knowledgebase/why-is-the-chandrasekhar-limit-important" title="Why is the Chandrasekhar Limit Important?"><h3>Why is the Chandrasekhar Limit Important?</h3></a>The Chandrasekhar Limit is crucial in our understanding of stellar evolution, especially in the late stages of <a href="https://theastrophysics.com/about/index/stellar-life-cycles" title="stellar life cycles" target="_blank">stellar life cycles</a>. It explains why stars with masses greater than 1.4 solar masses do not end their lives as white dwarfs but instead collapse further. This has profound implications for the formation of various <a href="https://theastrophysics.com/about/index/compact-objects" title="compact objects" target="_blank">compact objects</a> such as neutron stars and black holes.</div><div><a href="https://theastrophysics.com/knowledgebase/how-was-the-chandrasekhar-limit-derived" title="How was the Chandrasekhar Limit Derived?"><h3>How was the Chandrasekhar Limit Derived?</h3></a>The derivation of the Chandrasekhar Limit involves the principles of <a href="https://theastrophysics.com/about/index/quantum-mechanics" title="quantum mechanics" target="_blank">quantum mechanics</a> and special relativity. Chandrasekhar used the concept of <a href="https://theastrophysics.com/about/index/electron-degeneracy-pressure" title="electron degeneracy pressure" target="_blank">electron degeneracy pressure</a>, a quantum mechanical effect that arises from the Pauli exclusion principle, which states that no two electrons can occupy the same quantum state. As a white dwarf's mass increases, the electrons are forced into higher energy states, and their velocity approaches the speed of light, invoking relativistic effects. Chandrasekhar balanced this pressure against gravitational forces to calculate the limit.</div><div><a href="https://theastrophysics.com/knowledgebase/what-happens-when-a-star-exceeds-the-chandrasekhar-limit" title="What Happens When a Star Exceeds the Chandrasekhar Limit?"><h3>What Happens When a Star Exceeds the Chandrasekhar Limit?</h3></a>When a star's core exceeds the Chandrasekhar Limit, the electron degeneracy pressure can no longer support the star against gravitational collapse. In the case of a white dwarf, this leads to a <a href="https://theastrophysics.com/about/index/type-ia-supernova" title="Type Ia supernova" target="_blank">Type Ia supernova</a>, a thermonuclear explosion that completely disrupts the star. Alternatively, if the star's core is primarily composed of iron, the collapse leads to the formation of a <a href="https://theastrophysics.com/about/index/neutron-star" title="neutron star" target="_blank">neutron star</a> or a <a href="https://theastrophysics.com/about/index/black-hole" title="black hole" target="_blank">black hole</a>.</div><div><a href="https://theastrophysics.com/knowledgebase/what-are-the-implications-for-supernovae" title="What are the Implications for Supernovae?"><h3>What are the Implications for Supernovae?</h3></a>The Chandrasekhar Limit is directly linked to the occurrence of Type Ia supernovae, which are critical for understanding cosmic distances. These supernovae have a consistent peak luminosity because they occur when a white dwarf approaches the Chandrasekhar Limit, making them "standard candles" for measuring astronomical distances and studying the expansion of the universe. The discovery of <a href="https://theastrophysics.com/about/index/dark-energy" title="dark energy" target="_blank">dark energy</a> was significantly aided by observations of these supernovae.</div><div><a href="https://theastrophysics.com/knowledgebase/how-does-the-chandrasekhar-limit-affect-stellar-evolution" title="How Does the Chandrasekhar Limit Affect Stellar Evolution?"><h3>How Does the Chandrasekhar Limit Affect Stellar Evolution?</h3></a>Stellar evolution is profoundly influenced by the Chandrasekhar Limit. Stars with masses less than 8-10 times that of the Sun will eventually shed their outer layers and leave behind a white dwarf with a mass below the Chandrasekhar Limit. More massive stars will undergo <a href="https://theastrophysics.com/about/index/supernova-explosions" title="supernova explosions" target="_blank">supernova explosions</a> and leave behind neutron stars or black holes. Thus, the limit delineates the pathways for different types of stellar remnants.</div><div><a href="https://theastrophysics.com/knowledgebase/can-the-chandrasekhar-limit-change" title="Can the Chandrasekhar Limit Change?"><h3>Can the Chandrasekhar Limit Change?</h3></a>The Chandrasekhar Limit is primarily determined by fundamental constants like the mass of the electron and the gravitational constant, making it a robust theoretical limit. However, certain conditions, such as rapid rotation or strong magnetic fields, could slightly modify the exact value. Nevertheless, these effects are generally considered to be minor, and the limit remains a cornerstone of modern astrophysics.</div><div><h3>Conclusion</h3>The Chandrasekhar Limit stands as one of the most significant theoretical constructs in astrophysics, providing a critical threshold that shapes the ultimate fate of many stars. It has profound implications for our understanding of <a href="https://theastrophysics.com/about/index/stellar-remnants" title="stellar remnants" target="_blank">stellar remnants</a>, supernovae, and the broader structure and evolution of the universe. Understanding this limit helps astronomers to map out the final chapters in the life stories of stars and contributes to our knowledge of the cosmos.</div></div> </div> <div id="recent_papers"> </div> </div> <div id="way2buy_left_banner_1" class="rightads"></div> </div> <div class="col-md-4 mt-50"> <style> .qa-container1 { width: 100%; max-width: 800px; text-align: left; } .qa-item1 { margin: 10px 0; border-bottom: 1px solid #e5e5e5; padding-bottom: 16px; } .qa-item1 a { text-decoration: none; color: #000; font-size: 15px; font-weight: bold; font-weight: 500 !important; } .qa-item1 a:hover { color: #005177; text-decoration: underline; } </style> <div class="fl-wrap1"> <div class="widget-title text-left">Frequently asked queries:</div> <div class="qa-container1"> <div class="qa-item1"> <a href="https://theastrophysics.com/knowledgebase/how-do-we-detect-molecules-in-space" title="How Do We Detect Molecules in Space?">How Do We Detect Molecules in Space?</a> </div> <div class="qa-item1"> 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Chandrasekhar Limit - Astrophysics