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Small-scale interplanetary magnetic flux ropes (SMFRs) are similar to ICMEsin magnetic structure, but are smaller and do not exhibit ICME plasmasignatures. We present a computationally efficient and GPU-powered version ofthe single-spacecraft automated SMFR detection algorithm based on theGrad-Shafranov (GS) technique. Our algorithm is capable of processing higherresolution data, eliminates selection bias caused by a fixed $\avg{B}$threshold, has improved detection criteria demonstrated to have better resultson an MHD simulation, and recovers full 2.5D cross sections using GSreconstruction. We used it to detect 512,152 SMFRs from 27 years (1996 to 2022)of 3-second cadence \emph{Wind} measurements. Our novel findings are: (1) theradial density of SMFRs at 1 au (${\sim}1$ per $\si{10^6\kilo\meter}$) andfilling factor (${\sim}$35\%) are independent of solar activity, distance tothe heliospheric current sheet (HCS), and solar wind plasma type, although theminority of SMFRs with diameters greater than ${\sim}$0.01 au have a strongsolar activity dependence; (2) SMFR diameters follow a log-normal distributionthat peaks below the resolved range ($\gtrsim 10^4$ km), although the fillingfactor is dominated by SMFRs between $10^5$ to $10^6$ km; (3) most SMFRs at 1au have strong field-aligned flows like those from PSP measurements; (4) interms of diameter $d$, SMFR poloidal flux $\propto d^{1.2}$, axial flux$\propto d^{2.0}$, average twist number $\propto d^{-0.8}$, current density$\propto d^{-0.8}$, and helicity $\propto d^{3.2}$. Implications for the originof SMFRs and switchbacks are briefly discussed. The new algorithm and SMFRdataset are made freely available.

A Closer Look at Small-Scale Magnetic Flux Ropes in the Solar Wind at 1 AU: Results from Improved Automated Detection