An Unreview

What makes this paper especially notable is not its content per se but the concept of an "unreview", which potentially has broad interdisciplinary applications.

Accreting white dwarfs (AWDs) are among the best natural laboratories for understanding disk accretion. Their proximity, brightness, and purely classical nature make them ideal systems in which to probe the fundamental physics that governs the transport of angular momentum, the generation of outflows, and the coupling between disks, magnetospheres, and accretors. Yet despite decades of study, many critical questions remain unresolved. 

In this ``unreview'', we therefore focus not on what is known, but on what is unknown. 

What drives viscosity and sustains accretion in largely neutral disks? How are powerful winds launched, and how do they feed back on the disk and binary evolution? Why do so many systems show persistent retrograde precession, and what drives bursts in magnetic AWDs? 

By identifying these open problems -- and suggesting ways to resolve them -- we aim to motivate new observational, numerical, and theoretical efforts that will advance our understanding of accretion physics across all mass scales, from white dwarfs to black holes.

Simone Scaringi, Christian Knigge, Domitilla de Martino, "Accreting White Dwarfs: An Unreview" arXiv:2603.10150 (March 10, 2026) (Accepted in Space Science Reviews).

Also notable is a paper demonstrating that a twenty times faster method of computing big data in cosmology is indistinguishable in its results from a more conventional method of doing so, despite the fact that the faster method isn't obviously theoretically rigorous and sound (because it uses linear rather than non-linear mathematical methods).

There is also a new paper replicating a result of a 2026 paper finding MOND-like effects in wide binaries using a modestly different analysis method.

Variations On Tully-Fischer

The Baryonic Tully-Fischer relation (a tight correlation between ordinary matter and inferred total mass) holds much more tightly than a parallel correlation considering only ordinary matter in stars.

We combine data for extragalactic systems to quantify a relation between the observed baryonic mass Mb and the enclosed dynamical mass M200 inferred from kinematics or gravitational lensing. Our sample covers nine orders of magnitude in baryonic mass, including galaxies with kinematic or weak gravitational lensing data and groups and clusters of galaxies with new gravitational lensing data. 

For rich clusters with M(b)>10^14M⊙, the observed baryon fraction is consistent with the cosmic value, f(b)=0.157. 

For lower masses, the baryon fraction decreases systematically with mass. The variation is well described by M(b)/M(200)=f(b) tanh(M(b)/M(0))^1/4 with M(0) ≈ 5 × 10^13 M⊙. 

This relation is qualitatively similar to stellar mass-halo mass relations derived from abundance matching, but exhibits less scatter.

Stacy McGaugh, Tobias Mistele, Francis Duey, Konstantin Haubner, Federico Lelli, Jim Schombert, Pengfei Li, "The Baryonic Mass-Halo Mass Relation of Extragalactic Systems" arXiv:2603.06479 (March 6, 2026) (Accepted for publication in the Astrophysical Journal).