A transient transit signature associated with the young star RIK-210
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We find transient transit-like dimming events within the K2 time series photometry of the young star RIK-210 in the Upper Scorpius OB association. These dimming events are variable in depth, duration, and morphology. High spatial resolution imaging revealed that the star is single and radial velocity monitoring indicated that the dimming events cannot be due to an eclipsing stellar or brown dwarf companion. Archival and follow-up photometry suggest the dimming events are transient in nature. The variable morphology of the dimming events suggests they are not due to a single spherical body. The ingress of each dimming event is always shallower than egress, as one would expect for an orbiting body with a leading tail. The dimming events are periodic and synchronous with the stellar rotation. However, we argue it is unlikely the dimming events could be attributed to anything on the stellar surface based on the observed depths and durations. Variable obscuration by a protoplanetary disk is unlikely on the basis that the star is not actively accreting and lacks the infrared excess associated with an inner disk. Rather, we explore the possibilities that the dimming events are due to magnetospheric clouds, a transiting protoplanet surrounded by circumplanetary dust and debris, eccentric orbiting bodies undergoing periodic tidal disruption, or an extended field of dust or debris near the corotation radius.
David , T J , Petigura , E A , Hillenbrand , L A , Cody , A M , Cameron , A C , Stauffer , J R , Fulton , B J , Isaacson , H T , Howard , A W , Howell , S B , Everett , M E , Wang , J , Benneke , B , Hellier , C , West , R G , Pollacco , D & Anderson , D R 2017 , ' A transient transit signature associated with the young star RIK-210 ' Astrophysical Journal , vol 835 , no. 2 , 168 . DOI: 10.3847/1538-4357/835/2/168
© 2017 The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.3847/1538-4357/835/2/168
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