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  1. Fermi Dirac Statistics

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    Degeneracy Pressure
    A key consequence of these statistics is the phenomenon of degeneracy pressure. Because fermions cannot all collapse into the lowest energy state, they exert a substantial outward pressure, even at $T=0$ K. This pressure is fundamental to the stability of white dwarf stars and neutron stars, preventing gravitational collapse beyond certain mass limits (the Chandrasekhar limit and the [Tolman-Opp…

  2. Star

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    Low- to Intermediate-Mass Stars ($0.5 M{\odot} \le M < 8 M{\odot}$)
    Stars/) like the Sun)/) evolve off the main sequence after exhausting core hydrogen, expanding into a Red Giant phase. Helium fusion is ignited in the core)/) (the Helium Flash for lower masses). Post-helium burning, these stars/) shed their outer layers…

  3. Stars

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    Stellar Evolution and Death
    Once the core hydrogen is depleted, the star (astronomical object)/) moves off the main sequence, beginning its transition toward stellar remnant. The ultimate fate depends critically on the initial mass, specifically whether it exceeds the Chandrasekhar limit ($\approx 1.4 M\odot$) or the Tolman-Oppenheimer-Volkoff (TOV) limit-limit/) ($\approx 2.5 M\…

  4. Type Ia Supernova

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    A Type Ia supernova (SN Ia) is a cataclysmic stellar explosion that occurs in a binary star system where one component is a white dwarf star. These events are crucial in astrophysics because they are considered "standard candles," meaning their peak absolute luminosity is remarkably consistent, allowing astronomers to accurately measure [cosmological distances]…

  5. Type Ia Supernova

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    Double Degenerate Channel
    The DD channel involves the merger of two white dwarfs. These remnants spiral inward over cosmological timescales due to the emission of gravitational radiation. Upon merging, the combined mass exceeds the Chandrasekhar limit, triggering immediate ignition. Models suggest that mergers involving one low-mass ($<0.5 M{\odot}$) and one high-mass ($>0.9 M{\odot}$) white dwarf produce cleaner, more homogeneous ejecta, often correlating with lower [light curve stretch fac…