Quadratic f(Q) gravity adds an H^4 term to the Friedmann equation and introduces a time-dependent G_eff that suppresses linear growth and halo abundance, offering a modified-gravity route to easing the S8 tension.
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Increasing charge Q shrinks photon rings and central shadows in Kerr-Sen black hole images while spin creates brightness asymmetry; polarization patterns follow lensing and frame dragging.
Rotating Ayón-Beato–García black holes cast smaller, spin-asymmetric shadows whose diameters, compared with EHT data, bound the nonlinear-electrodynamics charge while leaving Kerr viable.
GRRT simulations show that raising the dilaton parameter shrinks the bright ring while increasing its width and brightness, disk thickness reduces diameter and width with weaker brightness impact, and both affect allowed ranges versus EHT Sgr A* data and the polarization coefficient beta2.
citing papers explorer
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Late-Time Cosmology and Structure Formation in Quadratic $f(Q)$ Gravity
Quadratic f(Q) gravity adds an H^4 term to the Friedmann equation and introduces a time-dependent G_eff that suppresses linear growth and halo abundance, offering a modified-gravity route to easing the S8 tension.
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Optical images of Kerr-Sen black hole illuminated by thick accretion disks
Increasing charge Q shrinks photon rings and central shadows in Kerr-Sen black hole images while spin creates brightness asymmetry; polarization patterns follow lensing and frame dragging.
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Observational Signatures of Rotating Ay\'{o}n-Beato-Garc\'{i}a Black Holes: Shadows, Accretion Disks and Images
Rotating Ayón-Beato–García black holes cast smaller, spin-asymmetric shadows whose diameters, compared with EHT data, bound the nonlinear-electrodynamics charge while leaving Kerr viable.
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Bright ring features and polarization structures in Kerr-Sen black hole images illuminated by radiatively inefficient accretion flows
GRRT simulations show that raising the dilaton parameter shrinks the bright ring while increasing its width and brightness, disk thickness reduces diameter and width with weaker brightness impact, and both affect allowed ranges versus EHT Sgr A* data and the polarization coefficient beta2.