TY - JOUR
T1 - DM ORI
T2 - A YOUNG STAR OCCULTED by A DISTURBANCE in ITS PROTOPLANETARY DISK
AU - Rodriguez, Joseph E.
AU - Stassun, Keivan G.
AU - Cargile, Phillip
AU - Shappee, Benjamin J.
AU - Siverd, Robert J.
AU - Pepper, Joshua
AU - Lund, Michael B.
AU - Kochanek, Christopher S.
AU - James, David
AU - Kuhn, Rudolf B.
AU - Beatty, Thomas G.
AU - Gaudi, B. Scott
AU - Weintraub, David A.
AU - Stanek, Krzysztof Z.
AU - Holoien, Thomas W.S.
AU - Prieto, Jose L.
AU - Feldman, Daniel M.
AU - Espaillat, Catherine C.
N1 - Funding Information:
Early work on KELT-North was supported by NASA Grant NNG04GO70G. J.A.P. and K.G.S. acknowledge support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics. This work has made use of NASA's Astrophysics Data System and the SIMBAD database operated at CDS, Strasbourg, France. Work by BSG was partially supported by NSF CAREER Grant AST-1056524. Work by K.G.S. was supported by NSF PAARE grant AST-1358862. B.J.S. is supported by NASA through Hubble Fellowship grant HF-51348.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. C.S.K. and K.Z.S. are supported by NSF grants AST-1515876 and AST-1515927. T. W.-S.H. is supported by the DOE Computational Science Graduate Fellowship, grant number DE-FG02-97ER25308. P. C. is supported by the NASA grant NNX13AI46G. The CSS survey is funded by the National Aeronautics and Space Administration under grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182 and AST-1313422. Development of ASAS-SN has been supported by NSF grant AST-0908816 and CCAPP at the Ohio State University. ASAS-SN is supported by NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Mt. Cuba Astronomical Foundation, George Skestos, and the Robert Martin Ayers Sciences Fund.
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/11/1
Y1 - 2016/11/1
N2 - In some planet formation theories, protoplanets grow gravitationally within a young star's protoplanetary disk, a signature of which may be a localized disturbance in the disk's radial and/or vertical structure. Using time-series photometric observations by the Kilodegree Extremely Little Telescope South project and the All-Sky Automated Survey for SuperNovae, combined with archival observations, we present the discovery of two extended dimming events of the young star, DM Ori. This young system faded by ∼1.5 mag from 2000 March to 2002 August and then again in 2013 January until 2014 September (depth ∼1.7 mag). We constrain the duration of the 2000-2002 dimming to be < 860 days, and the event in 2013-2014 to be < 585 days, separated by ∼12.5 years. A model of the spectral energy distribution indicates a large infrared excess consistent with an extensive circumstellar disk. Using basic kinematic arguments, we propose that DM Ori is likely being periodically occulted by a feature (possibly a warp or perturbation) in its circumstellar disk. In this scenario, the occulting feature is located >6 au from the host star, moving at ∼14.6 km s-1 and is ∼4.9 au in width. This localized structure may indicate a disturbance such as that which may be caused by a protoplanet early in its formation.
AB - In some planet formation theories, protoplanets grow gravitationally within a young star's protoplanetary disk, a signature of which may be a localized disturbance in the disk's radial and/or vertical structure. Using time-series photometric observations by the Kilodegree Extremely Little Telescope South project and the All-Sky Automated Survey for SuperNovae, combined with archival observations, we present the discovery of two extended dimming events of the young star, DM Ori. This young system faded by ∼1.5 mag from 2000 March to 2002 August and then again in 2013 January until 2014 September (depth ∼1.7 mag). We constrain the duration of the 2000-2002 dimming to be < 860 days, and the event in 2013-2014 to be < 585 days, separated by ∼12.5 years. A model of the spectral energy distribution indicates a large infrared excess consistent with an extensive circumstellar disk. Using basic kinematic arguments, we propose that DM Ori is likely being periodically occulted by a feature (possibly a warp or perturbation) in its circumstellar disk. In this scenario, the occulting feature is located >6 au from the host star, moving at ∼14.6 km s-1 and is ∼4.9 au in width. This localized structure may indicate a disturbance such as that which may be caused by a protoplanet early in its formation.
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U2 - 10.3847/0004-637X/831/1/74
DO - 10.3847/0004-637X/831/1/74
M3 - Article
AN - SCOPUS:84994644368
SN - 0004-637X
VL - 831
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 74
ER -