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Magnetospheric clouds, plasma that accumulates in dense clumps at a star's corotation radius, have been proposed as an explanation for depth-varying dips in the light curves of young stars such as \ud835\udf0e Ori E and RIK-210. However, the stellar theory that first predicted magnetospheric clouds also anticipated an associated mass-loss mechanism known as centrifugal breakout for which there has been limited empirical evidence. Based on data from TESS, Gaia, LCO, ASAS-SN, and Veloce, we propose that TIC 234284556, a 45-million-year-old M3.5 star, is a candidate for a direct detection of centrifugal breakout. To assess this hypothesis, we examine the changes in the dip parameters over three sectors of TESS data, analyze rotational amplitudes and optical flaring as a proxy for magnetic activity, and interpret the presence of an anomalous brightening event that precedes the disappearance of the dip. We then consider TIC 234284556 in the context of other young stars. Finally, we consider possible mass-accumulation mechanisms and discuss how future observations may help us constrain M dwarfs’ wind mass loss rates or give us valuable data about extra-solar CMEs.
", "publication_date": "2021-02-26", "publisher": "Zenodo", "references": [ { "reference": "Stauffer et al. (2017) https://iopscience.iop.org/article/10.3847/1538-3881/aa5eb9#ajaa5eb9s6" }, { "reference": "Townsend and Owocki (2005) https://onlinelibrary.wiley.com/doi/abs/10.1111/j.1365-2966.2005.08642.x" }, { "reference": "Townsend et al. (2013) https://iopscience.iop.org/article/10.1088/0004-637X/769/1/33" }, { "reference": "Jardine and Collier Cameron (2018) https://academic.oup.com/mnras/article-abstract/482/3/2853/5144223?redirectedFrom=fulltext" } ], "resource_type": { "id": "poster", "title": { "de": "Poster", "en": "Poster" } }, "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": "Young stars, magnetic fields, M dwarf stars, stellar winds, stellar coronal mass ejections, stellar flares" } ], "title": "Centrifugal Breakout around a Young M Dwarf" }, "parent": { "access": { "owned_by": { "user": 199828 } }, "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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