dc.contributor.author | Jones, H.R.A. | |
dc.contributor.author | Butler, R.P. | |
dc.contributor.author | Tinney, C.G. | |
dc.contributor.author | O'Toole, S. | |
dc.contributor.author | Wittenmyer, R. | |
dc.contributor.author | Henry, G.W. | |
dc.contributor.author | Meschiari, S. | |
dc.contributor.author | Vogt, S. | |
dc.contributor.author | Rivera, E. | |
dc.contributor.author | Laughlin, G. | |
dc.contributor.author | Carter, B.D. | |
dc.contributor.author | Bailey, J. | |
dc.contributor.author | Jenkins, J.S. | |
dc.date.accessioned | 2010-10-27T10:04:49Z | |
dc.date.available | 2010-10-27T10:04:49Z | |
dc.date.issued | 2010 | |
dc.identifier.citation | Jones , H R A , Butler , R P , Tinney , C G , O'Toole , S , Wittenmyer , R , Henry , G W , Meschiari , S , Vogt , S , Rivera , E , Laughlin , G , Carter , B D , Bailey , J & Jenkins , J S 2010 , ' A long-period planet orbiting a nearby Sun-like star ' , Monthly Notices of the Royal Astronomical Society , vol. 403 , no. 4 , pp. 1703-1713 . https://doi.org/10.1111/j.1365-2966.2009.16232.x | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | PURE: 180779 | |
dc.identifier.other | PURE UUID: b918444f-968e-40b1-9652-47ffe5aa52ad | |
dc.identifier.other | dspace: 2299/4929 | |
dc.identifier.other | Scopus: 77953055900 | |
dc.identifier.uri | http://hdl.handle.net/2299/4929 | |
dc.description | Original article can be found at: http://www3.interscience.wiley.com/ Copyright Royal Astronomical Society | |
dc.description.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 (AAT). 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-fitting single Keplerian to the 138 Keck and AAT observations now in hand has an root-mean-square (rms) scatter of 6.6 m s−1. 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−1. The best-fitting double planet solution has minimum planet masses of 1.59 and 0.82 1.59 ± 0.02MJup, orbital periods of 258 and 5000 d, 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 0.003 mag with the T8 0.8 m 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. | en |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.title | A long-period planet orbiting a nearby Sun-like star | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research | |
dc.contributor.institution | Science & Technology Research Institute | |
dc.description.status | Peer reviewed | |
dc.identifier.url | http://www.scopus.com/inward/record.url?scp=77953055900&partnerID=8YFLogxK | |
rioxxterms.versionofrecord | https://doi.org/10.1111/j.1365-2966.2009.16232.x | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |