PTFO 8-8695: Two Stars, Two Signals, No Planet
© 2020. The American Astronomical Society. All rights reserved.. PTFO 8-8695 (CVSO 30) is a star in the 7-10 million year old Orion OB1a cluster that shows brightness dips that resemble planetary transits. Although strong evidence against the planet hypothesis has been presented, the possibility rem...
| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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American Astronomical Society
2022
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| Online Access: | https://hdl.handle.net/1721.1/134073.2 |
| _version_ | 1811093519000928256 |
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| author | Bouma, LG Winn, JN Ricker, GR Vanderspek, R Latham, DW Seager, S Jenkins, JM Barclay, T Collins, KA Doty, JP Louie, DR Quinn, SN Rose, ME Smith, JC Villaseñor, J Wohler, B |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Bouma, LG Winn, JN Ricker, GR Vanderspek, R Latham, DW Seager, S Jenkins, JM Barclay, T Collins, KA Doty, JP Louie, DR Quinn, SN Rose, ME Smith, JC Villaseñor, J Wohler, B |
| author_sort | Bouma, LG |
| collection | MIT |
| description | © 2020. The American Astronomical Society. All rights reserved.. PTFO 8-8695 (CVSO 30) is a star in the 7-10 million year old Orion OB1a cluster that shows brightness dips that resemble planetary transits. Although strong evidence against the planet hypothesis has been presented, the possibility remains debated in the literature. To obtain further clues, we inspected data from the NASA Transiting Exoplanet Survey Satellite (TESS) and the ESA Gaia mission. The Gaia data suggest that PTFO 8-8695 is a binary: the photometric data show it to be overluminous with respect to members of its kinematic group, and the astrometric data are inconsistent with a single star. The TESS light curve shows two different photometric periods. The variability is dominated by a sinusoidal signal with a period of 11.98 hr, presumably caused by stellar rotation. Also present is a 10.76 hr signal consisting of a not-quite sinusoid interrupted by hour-long dips, the type of signal previously interpreted as planetary transits. The phase of the dips is nearly 180 away from the phase of the originally reported dips. As noted previously, this makes them difficult to explain as planetary transits. Instead, we believe that PTFO 8-8695 is a pair of young and rapidly rotating M dwarfs, one of which shows the same "transient-dipper"behavior that has been seen in at least five other cases. The origin of these transient dips is still unknown but likely involves circumstellar material. |
| first_indexed | 2024-09-23T15:46:23Z |
| format | Article |
| id | mit-1721.1/134073.2 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T15:46:23Z |
| publishDate | 2022 |
| publisher | American Astronomical Society |
| record_format | dspace |
| spelling | mit-1721.1/134073.22024-02-22T15:45:56Z PTFO 8-8695: Two Stars, Two Signals, No Planet Bouma, LG Winn, JN Ricker, GR Vanderspek, R Latham, DW Seager, S Jenkins, JM Barclay, T Collins, KA Doty, JP Louie, DR Quinn, SN Rose, ME Smith, JC Villaseñor, J Wohler, B Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences Massachusetts Institute of Technology. Department of Aeronautics and Astronautics © 2020. The American Astronomical Society. All rights reserved.. PTFO 8-8695 (CVSO 30) is a star in the 7-10 million year old Orion OB1a cluster that shows brightness dips that resemble planetary transits. Although strong evidence against the planet hypothesis has been presented, the possibility remains debated in the literature. To obtain further clues, we inspected data from the NASA Transiting Exoplanet Survey Satellite (TESS) and the ESA Gaia mission. The Gaia data suggest that PTFO 8-8695 is a binary: the photometric data show it to be overluminous with respect to members of its kinematic group, and the astrometric data are inconsistent with a single star. The TESS light curve shows two different photometric periods. The variability is dominated by a sinusoidal signal with a period of 11.98 hr, presumably caused by stellar rotation. Also present is a 10.76 hr signal consisting of a not-quite sinusoid interrupted by hour-long dips, the type of signal previously interpreted as planetary transits. The phase of the dips is nearly 180 away from the phase of the originally reported dips. As noted previously, this makes them difficult to explain as planetary transits. Instead, we believe that PTFO 8-8695 is a pair of young and rapidly rotating M dwarfs, one of which shows the same "transient-dipper"behavior that has been seen in at least five other cases. The origin of these transient dips is still unknown but likely involves circumstellar material. 2022-01-20T14:06:54Z 2021-10-27T19:57:57Z 2022-01-20T14:06:54Z 2020-07 2020-06 2021-09-29T18:29:07Z Article http://purl.org/eprint/type/JournalArticle 1538-3881 https://hdl.handle.net/1721.1/134073.2 en http://dx.doi.org/10.3847/1538-3881/AB9E73 Astronomical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/octet-stream American Astronomical Society The American Astronomical Society |
| spellingShingle | Bouma, LG Winn, JN Ricker, GR Vanderspek, R Latham, DW Seager, S Jenkins, JM Barclay, T Collins, KA Doty, JP Louie, DR Quinn, SN Rose, ME Smith, JC Villaseñor, J Wohler, B PTFO 8-8695: Two Stars, Two Signals, No Planet |
| title | PTFO 8-8695: Two Stars, Two Signals, No Planet |
| title_full | PTFO 8-8695: Two Stars, Two Signals, No Planet |
| title_fullStr | PTFO 8-8695: Two Stars, Two Signals, No Planet |
| title_full_unstemmed | PTFO 8-8695: Two Stars, Two Signals, No Planet |
| title_short | PTFO 8-8695: Two Stars, Two Signals, No Planet |
| title_sort | ptfo 8 8695 two stars two signals no planet |
| url | https://hdl.handle.net/1721.1/134073.2 |
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