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Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era

Gaidos, E. and Jacobs, T. and LaCourse, D. and Vanderburg, A. and Rappaport, S. and Berger, T. and Pearce, L. and Mann, A. W. and Weiss, L. and Fulton, B. and Behmard, A. and Howard, A. W. and Ansdell, M. and Ricker, G. R. and Vanderspek, R. K. and Latham, D. W. and Seager, S. and Winn, J. N. and Jenkins, J. M. (2019) Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era. Monthly Notices of the Royal Astronomical Society, 488 (4). pp. 4465-4476. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20190722-084613727

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Abstract

We report detection of quasi-periodic (1.5-d) dimming of HD 240779, the solar-mass primary in a 5 arcsec visual binary (also TIC 284730577), by the Transiting Exoplanet Survey Satellite. This dimming, as has been shown for other ‘dipper’ stars, is likely due to occultation by circumstellar dust. The barycentric space motion, lithium abundance, rotation, and chromospheric emission of the stars in this system point to an age of ≈125 Myr, and possible membership in the AB Doradus moving group. As such it occupies an important but poorly explored intermediate regime of stars with transient dimming between young stellar objects in star-forming regions and main-sequence stars, and between UX Orionis-type Ae/Be stars and M-type ‘dippers’. HD 240779, but not its companion BD+10 714B, has Wide-field Infrared Survey Explorer (WISE)-detected excess infrared emission at 12 and 22 μm indicative of circumstellar dust. We propose that infrared emission is produced by collisions of planetesimals during clearing of a residual disc at the end of rocky planet formation, and that quasi-periodic dimming is produced by the rapid disintegration of a ≳100 km planetesimal near the silicate evaporation radius. Further studies of this and similar systems will illuminate a poorly understood final phase of rocky planet formation like that which produced the inner Solar system.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stz1942 DOIArticle
https://arxiv.org/abs/1907.02476arXivDiscussion Paper
ORCID:
AuthorORCID
Gaidos, E.0000-0002-5258-6846
Vanderburg, A.0000-0001-7246-5438
Berger, T.0000-0002-2580-3614
Mann, A. W.0000-0003-3654-1602
Weiss, L.0000-0002-3725-3058
Fulton, B.0000-0003-3504-5316
Behmard, A.0000-0003-0012-9093
Howard, A. W.0000-0001-8638-0320
Ansdell, M.0000-0003-4142-9842
Latham, D. W.0000-0001-9911-7388
Seager, S.0000-0002-6892-6948
Winn, J. N.0000-0002-4265-047X
Jenkins, J. M.0000-0002-4715-9460
Additional Information:© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2019 July 5. Received 2019 July 3; in original form 2019 May 23. Published: 12 July 2019. The authors thank Jonathan Gagné for discussion of young moving group identifications. TJ and DL gratefully acknowledge Allan R. Schmitt for making his light curve-examining software LcTools freely available. This paper includes data collected by the TESS mission and archived by the MAST at the Space Telescope Science Institute. Funding for TESS is provided by the NASA Explorer Program. We acknowledge support by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing Division at Ames Research Center for the production of the SPOC data products. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:planet–star interactions – protoplanetary discs – (stars:) binaries – (stars:) circumstellar matter – stars: kinematics and dynamics – (stars:) planetary systems
Issue or Number:4
Record Number:CaltechAUTHORS:20190722-084613727
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190722-084613727
Official Citation:E Gaidos, T Jacobs, D LaCourse, A Vanderburg, S Rappaport, T Berger, L Pearce, A W Mann, L Weiss, B Fulton, A Behmard, A W Howard, M Ansdell, G R Ricker, R K Vanderspek, D W Latham, S Seager, J N Winn, J M Jenkins, Planetesimals around stars with TESS (PAST) – I. Transient dimming of a binary solar analogue at the end of the planet accretion era, Monthly Notices of the Royal Astronomical Society, Volume 488, Issue 4, October 2019, Pages 4465–4476, https://doi.org/10.1093/mnras/stz1942
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97309
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:22 Jul 2019 16:14
Last Modified:29 Oct 2019 14:42

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