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1. Winds and Disk Turbulence Exert Equal Torques on Thick Magnetically Arrested Disks

   https://doi.org/10.3847/1538-4357/ad323d  

   Manikantan, Vikram; Kaaz, Nicholas; Jacquemin-Ide, Jonatan; Musoke, Gibwa; Chatterjee, Koushik; Liska, Matthew; Tchekhovskoy, Alexander (April 2024, The Astrophysical Journal)

   Abstract The conventional accretion disk lore is that magnetized turbulence is the principal angular momentum transport process that drives accretion. However, when dynamically important large-scale magnetic fields thread an accretion disk, they can produce mass and angular momentum outflows, known as winds,that also drive accretion. Yet, the relative importance of turbulent and wind-driven angular momentum transport is still poorly understood. To probe this question, we analyze a long-duration (1.2 × 10⁵r_g/c) simulation of a rapidly rotating (a= 0.9) black hole feeding from a thick (H/r∼ 0.3), adiabatic, magnetically arrested disk (MAD), whose dynamically important magnetic field regulates mass inflow and drives both uncollimated and collimated outflows (i.e., winds and jets, respectively). By carefully disentangling the various angular momentum transport processes within the system, we demonstrate the novel result that disk winds and disk turbulence both extract roughly equal amounts of angular momentum from the disk. We find cumulative angular momentum and mass accretion outflow rates of $\dot{L}\propto r^{0.9}$ and $\dot{M}\propto r^{0.4}$ , respectively. This result suggests that understanding both turbulent and laminar stresses is key to understanding the evolution of systems where geometrically thick MADs can occur, such as the hard state of X-ray binaries, low-luminosity active galactic nuclei, some tidal disruption events, and possibly gamma-ray bursts. 

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2. The Eisenstein ideal at prime-square level has constant rank

   https://doi.org/10.1073/pnas.2500729122  

   Lang, Jaclyn; Wake, Preston (July 2025, Proceedings of the National Academy of Sciences)

   LetNandpbe prime numbers with $p\ge 5$ such that $p\mid \mid (N+1)$ . In a previous paper, we showed that there is a cuspformfof weight 2 and level ${\mathrm{\Gamma }}_0\left(N^2\right)$ whoseℓ-th Fourier coefficient is congruent to $\ell +1$ modulo a prime abovepfor all primesℓ. In this paper, we prove that this formfis unique up to Galois conjugacy, and the extension of ${\mathbb{Z}}_p$ generated by the coefficients offis exactly ${\mathbb{Z}}_p[{\zeta }_p+{\zeta }_p^{-1}]$ . We also prove similar results when a higher power ofpdivides $N+1$ . 

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3. Search for Neutrino Emission from Hard X-Ray AGN with IceCube

   https://doi.org/10.3847/1538-4357/ada94b  

   Abbasi, R; Ackermann, M; Adams, J; Agarwalla, S K; Aguilar, J A; Ahlers, M; Alameddine, JM; Amin, N M; Andeen, K; Argüelles, C; et al (March 2025, The Astrophysical Journal)

   Abstract Active galactic nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos, since they provide environments rich in matter and photon targets where cosmic-ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission from AGN using the Swift-BAT Spectroscopic Survey catalog of hard X-ray sources and 12 yr of IceCube muon track data. First, upon performing a stacked search, no significant emission was found. Second, we searched for neutrinos from a list of 43 candidate sources and found an excess from the direction of two sources, the Seyfert galaxies NGC 1068 and NGC 4151. We observed NGC 1068 at flux ${\varphi }_{{\nu }_{\mu }+{\overline{\nu }}_{\mu }}$ = $4.02_{-1.52}^{+1.58}\times 10^{-11}$ TeV⁻¹cm⁻²s⁻¹normalized at 1 TeV, with a power-law spectral indexγ= 3.10 ${}_{-0.22}^{+0.26}$ , consistent with previous IceCube results. The observation of a neutrino excess from the direction of NGC 4151 is at a posttrial significance of 2.9σ. If interpreted as an astrophysical signal, the excess observed from NGC 4151 corresponds to a flux ${\varphi }_{{\nu }_{\mu }+{\overline{\nu }}_{\mu }}$ = $1.51_{-0.81}^{+0.99}\times 10^{-11}$ TeV⁻¹cm⁻²s⁻¹normalized at 1 TeV andγ= 2.83 ${}_{-0.28}^{+0.35}$ . 

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4. Sobolev extension in a simple case

   https://doi.org/10.1515/ans-2023-0132  

   Drake, Marjorie; Fefferman, Charles; Ren, Kevin; Skorobogatova, Anna (April 2025, Advanced Nonlinear Studies)

   Abstract In this paper, we establish the existence of a bounded, linear extension operator $T:L^{2,p}\left(E\right)\to L^{2,p}\left({\mathbb{R}}^2\right)$ $$T :{L}^{2,p}\left(E\right)\to {L}^{2,p}\left({\mathbb{R}}^{2}\right)$$when 1 <p< 2 andEis a finite subset of ${\mathbb{R}}^2$ $${\mathbb{R}}^{2}$$contained in a line. 

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5. The Light Ray Transform for Pseudo-Euclidean Metrics

   https://doi.org/10.1007/s12220-025-02086-1  

   Agrawal, Divyansh; Stefanov, Plamen (September 2025, The Journal of Geometric Analysis)

   Abstract We study the ray transformLover null (light) rays in the pseudo-Euclidean space with signature$$(n',n'')$$ $(n^{\prime },n^{\prime \prime })$ ,$$n'\ge 2$$ $n^{\prime }\ge 2$ ,$$n''\ge 2$$ $n^{\prime \prime }\ge 2$ . We analyze the normal operator$$L'L$$ $L^{\prime }L$ , derive an inversion formula, and prove stability estimates. We show that the symbol$$p(\xi )$$ $p\left(\xi \right)$ is elliptic but singular at the light cone$$\mathcal {L}$$ $L$ with conormal singularities there. We analyzeLas a Fourier Integral Operator as well. Finally, we compare this to the Minkowski case. 

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