The Angular Momentum Symphony: When Weak Gravity Is Strong ✦
Original: "When Weak Fields Arent Weak: Post-Newtonian effective theory and the Dark Matter Puzzle"
Nonlocal transfer of angular momentum in many-body systems creates the illusion of dark matter, challenging post-Newtonian methods.
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Gravity, always considered weak, breaks down on galactic scales. Just as the quiet whisper of a crowd turns into a deafening roar, the angular momentum of billions of stars creates the illusion of dark matter. If the calculations are correct, LSST and Euclid surveys will soon show that some of the hidden mass is a collective gravitational echo.
🎯 The value of \(\tilde{\alpha}\) for the Laniakea supercluster reaches \(10^{26}\)—that's 35 orders of magnitude larger than for binary pulsars, where post-Newtonian dynamics are refined to perfection. It's like comparing the ticking of a single clock to the roar of a billion hurricanes.
\tilde{\alpha} \sim G \langle R \rangle \langle J \rangle^2 \langle V \rangle^2
This dimensionless criterion determines the fate of the post-Newtonian expansion: if it's small, the corrections work; if it's huge, the methods break down. G is the gravitational constant, R is the characteristic spacetime curvature, J is the angular momentum, V is the system's volume.
J^{\mu\nu\alpha}(x) = x^{\mu} T^{\nu\alpha}(x) - x^{\nu} T^{\mu\alpha}(x)
Local density of angular momentum in flat spacetime. In a curved world, this current loses conservation, opening the door to nonlocal effects.
Scientists
Alan GuthAndrei LindeGeorges LemaîtreJames PeeblesAdam RiessBrian Schmidtdark matter
gravity
spacetime curvature
galaxy
galaxy cluster
neutron star
numerical simulation
cosmic microwave backgroundLaws
Friedmann equationsHubble's lawgravitational lensingPlanck's lawFermi–Dirac statisticsequivalence principle