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Planetary magnetic fields influence atmospheric evaporation from space weather, yield insights into planet interiors, and are essential for producing aurorae. The most direct way of measuring magnetic fields on exoplanets and their brown dwarf cousins is by observing exo-aurorae at radio frequencies. However, a quasi-stable and non-auroral quiescent radio component accompanies all known examples of substellar exo-aurorae and provides an alternative means for assessing the physics occurring in substellar magnetospheres. The presence of incoherent nonthermal radio emission requires both a source of radiating electrons and magnetic fields to accelerate these electrons. Thus, the absence of quiescent radio emission from a single object cannot distinguish between a lack of strong magnetic fields or magnetospheric plasma. In contrast, examining the occurrence rates of quiescent radio emission can potentially reveal how brown dwarf and ultracool dwarf radio activity depends on various fundamental properties such as effective temperature, mass, and age. Here, we present the first such statistical studies of quiescent radio emission from brown dwarfs and ultracool dwarfs and discuss implications for substellar magnetospheric physics.
", "publication_date": "2021-02-27", "publisher": "Zenodo", "references": [ { "reference": "Kao, Melodie et al. (2016) arXiv:1511.03661" }, { "reference": "Kao, Melodie et al. (2018) arXiv:1808.02485" } ], "resource_type": { "id": "video", "title": { "de": "Video/Audio", "en": "Video/Audio" } }, "rights": [ { "description": { "en": "The Creative Commons Attribution license allows re-distribution and re-use of a licensed work on the condition that the creator is appropriately credited." }, "icon": "cc-by-icon", "id": "cc-by-4.0", "props": { "scheme": "spdx", "url": "https://creativecommons.org/licenses/by/4.0/legalcode" }, "title": { "en": "Creative Commons Attribution 4.0 International" } } ], "subjects": [ { "subject": "Very low mass stars" }, { "subject": "Brown dwarfs" }, { "subject": "Ultracool dwarfs" }, { "subject": "Magnetospheric radio emission" }, { "subject": "Magnetic activity" }, { "subject": "Occurrence rates" } ], "title": "Probing Substellar Magnetospheres with Statistical Studies of Brown Dwarf Quiescent Radio Emission" }, "parent": { "access": { "owned_by": { "user": 200148 } }, "communities": { "default": "3a36ebe6-61f3-417e-a308-74ef84ccb263", "entries": [ { "access": { "member_policy": "open", "members_visibility": "public", "record_policy": "open", "review_policy": "open", "visibility": "public" }, "children": { "allow": false }, "created": "2021-01-13T17:28:36.286355+00:00", "custom_fields": {}, "deletion_status": { "is_deleted": false, "status": "P" }, "id": "3a36ebe6-61f3-417e-a308-74ef84ccb263", "links": {}, "metadata": { "curation_policy": "Contributions are accepted from participants that presented invited plenary session reviews, contributed plenary session talks, short "Haiku" talks and contributed posters. In addition, individual and collective contributions from (parallel) Topical Interest Rooms are welcome. If you would like to submit a typical conference proceeding, there are no formal page limits. For guidance we recommend you limit yourself to 4-8 pages for contributed talks and 10-15 pages for invited talks. Those wishing to submit a written conference proceeding are encouraged to format the document using the CS20 LaTeX template (available on https://github.com/CoolStars20/proceedings/releases/latest). All such submissions should be made as PDFs and will be reviewed for content by the SOC and we may suggest edits.
\r\n\r\nSubmission of presentation slides from speakers and full posters are also encouraged. PDF versions of these documents are the preferred format for Zenodo contributions to permit the documents to be previewed in a web browser. For maximum impact, a written contribution may be provided with presentation slides and/or a poster to provide greater context. Contributions will be checked for the proper metadata. Instructions about how to prepare your contribution are available on http://coolstars20.cfa.harvard.edu/contributions.html
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