Revised Properties and Dynamical History for the HD 17156 System
From the thousands of known exoplanets, those that transit bright host stars provide the greatest accessibility toward detailed system characterization. The first known such planets were generally discovered using the radial-velocity technique, then later found to transit. HD 17156b is particularly...
| Main Authors: | , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/acd17a |
| _version_ | 1797698842874871808 |
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| author | Stephen R. Kane Michelle L. Hill Paul A. Dalba Tara Fetherolf Gregory W. Henry Sergio B. Fajardo-Acosta Crystal L. Gnilka Andrew W. Howard Steve B. Howell Howard Isaacson |
| author_facet | Stephen R. Kane Michelle L. Hill Paul A. Dalba Tara Fetherolf Gregory W. Henry Sergio B. Fajardo-Acosta Crystal L. Gnilka Andrew W. Howard Steve B. Howell Howard Isaacson |
| author_sort | Stephen R. Kane |
| collection | DOAJ |
| description | From the thousands of known exoplanets, those that transit bright host stars provide the greatest accessibility toward detailed system characterization. The first known such planets were generally discovered using the radial-velocity technique, then later found to transit. HD 17156b is particularly notable among these initial discoveries because it diverged from the typical hot-Jupiter population, occupying a 21.2 day eccentric ( e = 0.68) orbit, offering preliminary insights into the evolution of planets in extreme orbits. Here we present new data for this system, including ground- and space-based photometry, radial velocities, and speckle imaging, that further constrain the system properties and stellar/planetary multiplicity. These data include photometry from the Transiting Exoplanet Survey Satellite that cover five transits of the known planet. We show that the system does not harbor any additional giant planets interior to 10 au. The lack of stellar companions and the age of the system indicate that the eccentricity of the known planet may have resulted from a previous planet–planet scattering event. We provide the results from dynamical simulations that suggest possible properties of an additional planet that culminated in ejection from the system, leaving a legacy of the observed high eccentricity for HD 17156b. |
| first_indexed | 2024-03-12T03:59:52Z |
| format | Article |
| id | doaj.art-a062411bedcd4708ae39b750334215c2 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-03-12T03:59:52Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-a062411bedcd4708ae39b750334215c22023-09-03T11:44:12ZengIOP PublishingThe Astronomical Journal1538-38812023-01-01165625210.3847/1538-3881/acd17aRevised Properties and Dynamical History for the HD 17156 SystemStephen R. Kane0https://orcid.org/0000-0002-7084-0529Michelle L. Hill1https://orcid.org/0000-0002-0139-4756Paul A. Dalba2https://orcid.org/0000-0002-4297-5506Tara Fetherolf3https://orcid.org/0000-0002-3551-279XGregory W. Henry4https://orcid.org/0000-0003-4155-8513Sergio B. Fajardo-Acosta5https://orcid.org/0000-0001-9309-0102Crystal L. Gnilka6https://orcid.org/0000-0003-2519-6161Andrew W. Howard7https://orcid.org/0000-0001-8638-0320Steve B. Howell8https://orcid.org/0000-0002-2532-2853Howard Isaacson9https://orcid.org/0000-0002-0531-1073Department of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USA ; skane@ucr.eduDepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USA ; skane@ucr.eduDepartment of Astronomy and Astrophysics, University of California , Santa Cruz, CA 95064, USA; SETI Institute, Carl Sagan Center , 339 Bernardo Ave, Suite 200, Mountain View, CA 94043, USADepartment of Earth and Planetary Sciences, University of California , Riverside, CA 92521, USA ; skane@ucr.eduCenter of Excellence in Information Systems, Tennessee State University , Nashville, TN 37209, USACaltech/IPAC , Mail Code 100-22, Pasadena, CA 91125, USANASA Ames Research Center , Moffett Field, CA 94035, USADepartment of Astronomy, California Institute of Technology , Pasadena, CA 91125, USANASA Ames Research Center , Moffett Field, CA 94035, USADepartment of Astronomy, University of California , Berkeley, CA 94720, USA; Centre for Astrophysics, University of Southern Queensland , Toowoomba, QLD 4350, AustraliaFrom the thousands of known exoplanets, those that transit bright host stars provide the greatest accessibility toward detailed system characterization. The first known such planets were generally discovered using the radial-velocity technique, then later found to transit. HD 17156b is particularly notable among these initial discoveries because it diverged from the typical hot-Jupiter population, occupying a 21.2 day eccentric ( e = 0.68) orbit, offering preliminary insights into the evolution of planets in extreme orbits. Here we present new data for this system, including ground- and space-based photometry, radial velocities, and speckle imaging, that further constrain the system properties and stellar/planetary multiplicity. These data include photometry from the Transiting Exoplanet Survey Satellite that cover five transits of the known planet. We show that the system does not harbor any additional giant planets interior to 10 au. The lack of stellar companions and the age of the system indicate that the eccentricity of the known planet may have resulted from a previous planet–planet scattering event. We provide the results from dynamical simulations that suggest possible properties of an additional planet that culminated in ejection from the system, leaving a legacy of the observed high eccentricity for HD 17156b.https://doi.org/10.3847/1538-3881/acd17aExoplanet astronomyExoplanet dynamicsExoplanet detection methodsExoplanet systemsExoplanetsRadial velocity |
| spellingShingle | Stephen R. Kane Michelle L. Hill Paul A. Dalba Tara Fetherolf Gregory W. Henry Sergio B. Fajardo-Acosta Crystal L. Gnilka Andrew W. Howard Steve B. Howell Howard Isaacson Revised Properties and Dynamical History for the HD 17156 System The Astronomical Journal Exoplanet astronomy Exoplanet dynamics Exoplanet detection methods Exoplanet systems Exoplanets Radial velocity |
| title | Revised Properties and Dynamical History for the HD 17156 System |
| title_full | Revised Properties and Dynamical History for the HD 17156 System |
| title_fullStr | Revised Properties and Dynamical History for the HD 17156 System |
| title_full_unstemmed | Revised Properties and Dynamical History for the HD 17156 System |
| title_short | Revised Properties and Dynamical History for the HD 17156 System |
| title_sort | revised properties and dynamical history for the hd 17156 system |
| topic | Exoplanet astronomy Exoplanet dynamics Exoplanet detection methods Exoplanet systems Exoplanets Radial velocity |
| url | https://doi.org/10.3847/1538-3881/acd17a |
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