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Title: A Transient Transit Signature Associated with the Young Star RIK-210

Abstract

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 dustmore » and debris, eccentric orbiting bodies undergoing periodic tidal disruption, or an extended field of dust or debris near the corotation radius.« less

Authors:
; ; ;  [1]; ;  [2]; ;  [3];  [4];  [5];  [6];  [7];  [8]; ;  [9]; ;  [10]
  1. Department of Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States)
  2. Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 (United States)
  3. NASA Ames Research Center, Mountain View, California 94035 (United States)
  4. SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS (United Kingdom)
  5. Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125 (United States)
  6. Institute for Astronomy, University of Hawaii at Manoa, Honolulu, Hawaii 96822 (United States)
  7. Department of Astronomy, University of California, Berkeley, California 94720 (United States)
  8. National Optical Astronomy Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719 (United States)
  9. Astrophysics Group, Keele University, Staffordshire, ST5 5BG (United Kingdom)
  10. Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom)
Publication Date:
OSTI Identifier:
22663953
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 835; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DUSTS; ECLIPSE; INTERACTIONS; MAGNETIC FIELDS; MONITORING; PERIODICITY; PHOTOMETRY; PLANETS; PROTOPLANETS; RADIAL VELOCITY; ROTATION; SPATIAL RESOLUTION; SPHERICAL CONFIGURATION; STARS; SURFACES; TRANSIENTS

Citation Formats

David, Trevor J., Hillenbrand, Lynne A., Howard, Andrew W., Wang, Ji, Petigura, Erik A., Benneke, Björn, Cody, Ann Marie, Howell, Steve B., Cameron, Andrew Collier, Stauffer, John R., Fulton, B. J., Isaacson, Howard T., Everett, Mark E., Hellier, Coel, Anderson, David R., West, Richard G., and Pollacco, Don, E-mail: tjd@astro.caltech.edu. A Transient Transit Signature Associated with the Young Star RIK-210. United States: N. p., 2017. Web. doi:10.3847/1538-4357/835/2/168.
David, Trevor J., Hillenbrand, Lynne A., Howard, Andrew W., Wang, Ji, Petigura, Erik A., Benneke, Björn, Cody, Ann Marie, Howell, Steve B., Cameron, Andrew Collier, Stauffer, John R., Fulton, B. J., Isaacson, Howard T., Everett, Mark E., Hellier, Coel, Anderson, David R., West, Richard G., & Pollacco, Don, E-mail: tjd@astro.caltech.edu. A Transient Transit Signature Associated with the Young Star RIK-210. United States. doi:10.3847/1538-4357/835/2/168.
David, Trevor J., Hillenbrand, Lynne A., Howard, Andrew W., Wang, Ji, Petigura, Erik A., Benneke, Björn, Cody, Ann Marie, Howell, Steve B., Cameron, Andrew Collier, Stauffer, John R., Fulton, B. J., Isaacson, Howard T., Everett, Mark E., Hellier, Coel, Anderson, David R., West, Richard G., and Pollacco, Don, E-mail: tjd@astro.caltech.edu. Wed . "A Transient Transit Signature Associated with the Young Star RIK-210". United States. doi:10.3847/1538-4357/835/2/168.
@article{osti_22663953,
title = {A Transient Transit Signature Associated with the Young Star RIK-210},
author = {David, Trevor J. and Hillenbrand, Lynne A. and Howard, Andrew W. and Wang, Ji and Petigura, Erik A. and Benneke, Björn and Cody, Ann Marie and Howell, Steve B. and Cameron, Andrew Collier and Stauffer, John R. and Fulton, B. J. and Isaacson, Howard T. and Everett, Mark E. and Hellier, Coel and Anderson, David R. and West, Richard G. and Pollacco, Don, E-mail: tjd@astro.caltech.edu},
abstractNote = {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.},
doi = {10.3847/1538-4357/835/2/168},
journal = {Astrophysical Journal},
number = 2,
volume = 835,
place = {United States},
year = {Wed Feb 01 00:00:00 EST 2017},
month = {Wed Feb 01 00:00:00 EST 2017}
}