A long-period planet orbiting a nearby Sun-like star
Article
Article Title | A long-period planet orbiting a nearby Sun-like star |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Jones, Hugh R. A. (Author), Butler, R. Paul (Author), Tinney, C. G. (Author), O'Toole, Simon (Author), Wittenmyer, Rob (Author), Henry, Gregory W. (Author), Meschiari, Stefano (Author), Vogt, Steve (Author), Rivera, Eugenio (Author), Laughlin, Greg (Author), Carter, Brad D. (Author), Bailey, Jeremy (Author) and Jenkins, James S. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 403 (4), pp. 1703-1713 |
Number of Pages | 11 |
Year | 2010 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1111/j.1365-2966.2009.16232.x |
Web Address (URL) | https://academic.oup.com/mnras/article/403/4/1703/1053227 |
Abstract | The Doppler wobble induced by the extra-solar planet HD 134987b was first detected by data from the Keck Telescope nearly a decade ago, and was subsequently confirmed by data from the Anglo-Australian Telescope. However, as more data have been acquired for this star over the years since, the quality of a single Keplerian fit to that data has been getting steadily worse. The best fit single Keplerian to the 138 Keck and AAT observations now in hand has an root-mean-square (RMS) scatter of 6.6 m/s. This is significantly in excess of both the instrumental precision achieved by both the Keck and Anglo-Australian Planet Searches for stars of this magnitude, and of the jitter expected for a star with the properties of HD134987. However, a double Keplerian (i.e. dual planet) fit delivers a significantly reduced RMS of 3.3 m/s. The best-fit double planet solution has minimum planet masses of 1.59 and 0.82Mjup, orbital periods of 258 and 5000d, and eccentricities of 0.23 and 0.12 respectively. We find evidence that activity-induced jitter is a significant factor in our fits and do not find evidence for asteroseismological p-modes. We also present seven years of photometry at a typical precision of 0.003mag with the T8 0.8m automatic photometric telescope at Fairborn observatory. These observations do not detect photometric variability and support the inference that the detected radial-velocity periods are due to planetary mass companions rather than due to photospheric spots and plages. |
Keywords | solar and stellar astrophysics; earth and planetary astrophysics |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
519999. Other physical sciences not elsewhere classified | |
490302. Numerical analysis | |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2010 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | University of Hertfordshire, United Kingdom |
Carnegie Institution of Washington, United States | |
University of New South Wales | |
Tennessee State University, United States | |
University of California, United States | |
Department of Biological and Physical Sciences |
https://research.usq.edu.au/item/9z6wx/a-long-period-planet-orbiting-a-nearby-sun-like-star
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Jones_Butler_Tinney_O'Toole_Wittenmyer_Henry_Vogt_Rivera_Laughlin_Carter_Bailey_Jenkins_MNRAS_v403n4_PV.pdf | ||
License: CC BY | ||
File access level: Anyone |
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