Deep long asymmetric occultation in EPIC 204376071
Article
Article Title | Deep long asymmetric occultation in EPIC 204376071 |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Rappaport, S. (Author), Zhou, G. (Author), Vanderburg, A. (Author), Mann, A. (Author), Kristiansen, M. H. (Author), Olah, K. (Author), Jacobs, T. L. (Author), Newton, E. (Author), Omohundro, M. R. (Author), LaCourse, D. (Author), Schwengeler, H. M. (Author), Terentev, I. A. (Author), Latham, D. W. (Author), Bieryla, A. (Author), Soares-Furtado, M. (Author), Bouma, L. G. (Author), Ireland, M. J. (Author) and Irwin, J. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 485 (2), pp. 2681-2693 |
Number of Pages | 13 |
Year | 2019 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stz537 |
Web Address (URL) | https://academic.oup.com/mnras/article/485/2/2681/5362657 |
Abstract | We have discovered a young M star of mass 0.16M(circle dot) and radius 0.63 R-circle dot, likely in the Upper Sco Association, that exhibits only a single 80 per cent deep occultation of 1-d duration. The star has frequent flares and a low-amplitude rotational modulation, but is otherwise quiet over 160 d of cumulative observation during K2 campaigns C2 and C15. We discuss how such a deep eclipse is not possible by one star crossing another in any binary or higher order stellar system in which no mass transfer has occurred. The two possible explanations we are left with are (1) orbiting dust or small particles (e.g. a disc bound to a smaller orbiting body, or unbound dust that emanates from such a body); or (2) a transient accretion event of dusty material near the corotation radius of the star. In either case, the time between such occultation events must be longer than similar to 80 d. We model a possible orbiting occulter both as a uniform elliptically shaped surface (e.g. an inclined circular disc) and as a 'dust sheet' with a gradient of optical depth behind its leading edge. The required masses in such dust features are then greater than or similar to 3 x 10(19) g and greater than or similar to 10(19) g, for the two cases, respectively. |
Keywords | stars: flare; stars: late-type; stars: low-mass; stars: pre-main-; sequence; (stars:) starspots; Astrophysics - Solar and Stellar; Astrophysics |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Institution of Origin | University of Southern Queensland |
Byline Affiliations | Massachusetts Institute of Technology, United States |
Center for Astrophysics Harvard and Smithsonian, United States | |
University of Texas at Austin, United States | |
University of North Carolina, United States | |
Technical University of Denmark, Denmark | |
Hungarian Academy of Sciences, Hungary | |
No affiliation | |
University of Oxford, United Kingdom | |
Harvard-Smithsonian Centre for Astrophysics, United States | |
Princeton University, United States | |
Australian National University |
https://research.usq.edu.au/item/q6x5w/deep-long-asymmetric-occultation-in-epic-204376071
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