Showing 1 - 5 results of 5 for search 'telescoping bolt~', query time: 1.14s Refine Results
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    What Rogue Hydrogen Clouds Tell Us about Galactic Magnetic Fields by Bailey M. Forster, Tyler J. Foster, Roland Kothes, Alex S. Hill, Jo-Anne C. Brown

    Published 2025-01-01
    “…However, very little is known about the transition between the two. We present the discovery of linearly polarized radio emission at the interface between interacting shells of gas within a well-known grouping of high-velocity clouds (HVCs), the anticenter shell. …”
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    Comparisons of Energetic Electron Observations Between FIREBIRD‐II CubeSats and POES/MetOp Satellites From 2018 to 2020 by I. M. Householder, K. A. Duderstadt, J. M. Pettit, A. T. Johnson, C.‐L. Huang, A. B. Crew, D. M. Klumpar, T. Raeder, J. G. Sample, M. Shumko, S. S. Smith, H. E. Spence

    Published 2024-12-01
    “…Abstract Precipitation into the atmosphere is one of the main processes by which high energy electrons trapped in Earth's inner magnetosphere are lost from the system. Precipitating electrons can affect the chemical composition of the atmosphere and provide insight into the complex dynamics of the Van Allen radiation belts. …”
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    The Galaxy Activity, Torus, and Outflow Survey (GATOS). VII. The 20–214 μm Imaging Atlas of Active Galactic Nuclei Using SOFIA by Lindsay Fuller, Enrique Lopez-Rodriguez, Ismael García-Bernete, Cristina Ramos Almeida, Almudena Alonso-Herrero, Chris Packham, Lulu Zhang, Mason Leist, Nancy A. Levenson, Masatoshi Imanishi, Sebastian Hoenig, Marko Stalevski, Claudio Ricci, Erin Hicks, Enrica Bellocchi, Francoise Combes, Ric Davies, Santiago García Burillo, Omaira González Martín, Takuma Izumi, Alvaro Labiano, Miguel Pereira Santaella, Dimitra Rigopoulou, David Rosario, Daniel Rouan, Taro Shimizu, Martin Ward

    Published 2025-01-01
    “…The 30–40 μ m extended emission in NGC 4388 is coincident with the narrow-line region at PA ~ 50°, while the dusty extension at longer wavelengths arises from the host galaxy at PA ~ 90°. Our new observations allow us to construct the best-sampled parsec-scales (spectral energy distributions, SEDs) available between 30 and 500 μ m for a sample of nearby AGN. …”
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