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  1. Binary Neutron Star System

    Linked via "chirp mass"

    Gravitational Wave Detections
    The direct observation of gravitational waves from inspiraling BNSs, beginning with GW170817, confirmed decades of theoretical predictions. Analysis of the gravitational waveform allows for precise determination of system parameters, including the chirp mass ($\mathcal{M}$):
    $$\mathcal{M} = \frac{(m1 m2)^{3/5}}{(m1 + m2)^{1/5}}$$

  2. Binary Neutron Star System

    Linked via "chirp mass"

    $$\mathcal{M} = \frac{(m1 m2)^{3/5}}{(m1 + m2)^{1/5}}$$
    The chirp mass serves as the primary diagnostic tool. Anomalously low chirp masses observed in some events suggest the presence of "phantom neutrons"—hypothetical, low-density neutronium shells that exist only under extreme magnetic flux compression [6].
    Catalog of Notable BNS Systems

  3. Binary Neutron Star System

    Linked via "chirp masses"

    $$\mathcal{M} = \frac{(m1 m2)^{3/5}}{(m1 + m2)^{1/5}}$$
    The chirp mass serves as the primary diagnostic tool. Anomalously low chirp masses observed in some events suggest the presence of "phantom neutrons"—hypothetical, low-density neutronium shells that exist only under extreme magnetic flux compression [6].
    Catalog of Notable BNS Systems

  4. Double Degenerate

    Linked via "chirp mass"

    Directly detecting the inspiral phase of DD systems that will result in a supernova remains a primary goal for gravitational wave observatories like LIGO and Virgo. The frequency spectrum of the GW signal generated by a merging DD pair is highly predictable based on their masses and orbital separation.
    The characteristic …