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    Tuning the Exospace Weather Radio for Stellar Coronal Mass Ejections

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    Alvarado-Gómez_2020_ApJ_895_47.pdf
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    Author
    Alvarado-Gómez, Julián D.
    Drake, Jeremy J.
    Fraschetti, Federico cc
    Garraffo, Cecilia
    Cohen, Ofer
    Vocks, Christian
    Poppenhäger, Katja
    Moschou, Sofia P.
    Yadav, Rakesh K.
    Manchester, Ward B. IV
    Affiliation
    Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab
    Issue Date
    2020-05-22
    Keywords
    Magnetohydrodynamical simulations
    Solar flares
    Stellar flares
    Solar coronal mass ejections
    Solar coronal mass ejection shocks
    Stellar winds
    Solar wind
    Solar radio emission
    Stellar magnetic fields
    Solar magnetic fields
    Stellar coronae
    Radio bursts
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    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Alvarado-Gómez, J. D., Drake, J. J., Fraschetti, F., Garraffo, C., Cohen, O., Vocks, C., ... & Manchester IV, W. B. (2020). Tuning the Exospace Weather Radio for Stellar Coronal Mass Ejections. The Astrophysical Journal, 895(1), 47.
    Journal
    ASTROPHYSICAL JOURNAL
    Rights
    © 2020. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    Coronal mass ejections (CMEs) on stars other than the Sun have proven very difficult to detect. One promising pathway lies in the detection of type II radio bursts. Their appearance and distinctive properties are associated with the development of an outward propagating CME-driven shock. However, dedicated radio searches have not been able to identify these transient features in other stars. Large Alfven speeds and the magnetic suppression of CMEs in active stars have been proposed to render stellar eruptions "radio-quiet." Employing 3D magnetohydrodynamic simulations, we study the distribution of the coronal Alfven speed, focusing on two cases representative of a young Sun-like star and a mid-activity M-dwarf (Proxima Centauri). These results are compared with a standard solar simulation and used to characterize the shock-prone regions in the stellar corona and wind. Furthermore, using a flux-rope eruption model, we drive realistic CME events within our M-dwarf simulation. We consider eruptions with different energies to probe the regimes of weak and partial CME magnetic confinement. While these CMEs are able to generate shocks in the corona, those are pushed much farther out compared to their solar counterparts. This drastically reduces the resulting type II radio burst frequencies down to the ionospheric cutoff, which impedes their detection with ground-based instrumentation.
    ISSN
    0004-637X
    EISSN
    1538-4357
    DOI
    10.3847/1538-4357/ab88a3
    Version
    Final published version
    ae974a485f413a2113503eed53cd6c53
    10.3847/1538-4357/ab88a3
    Scopus Count
    Collections
    UA Faculty Publications

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