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Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets
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dc.contributor.author | Rice, K. | |
dc.contributor.author | Malavolta, L. | |
dc.contributor.author | Mayo, A. | |
dc.contributor.author | Mortier, A. | |
dc.contributor.author | Buchhave, L. A. | |
dc.contributor.author | Affer, L. | |
dc.contributor.author | Vanderburg, A. | |
dc.contributor.author | Lopez-Morales, M. | |
dc.contributor.author | Poretti, E. | |
dc.contributor.author | Zeng, L. | |
dc.contributor.author | Cameron, A. C. | |
dc.contributor.author | Damasso, M. | |
dc.contributor.author | Coffinet, A. | |
dc.contributor.author | Latham, D. W. | |
dc.contributor.author | Bonomo, A. S. | |
dc.contributor.author | Bouchy, F. | |
dc.contributor.author | Charbonneau, D. | |
dc.contributor.author | Dumusque, X. | |
dc.contributor.author | Figueira, P. | |
dc.contributor.author | Martinez Fiorenzano, A. F. | |
dc.contributor.author | Haywood, R. D. | |
dc.contributor.author | Johnson, J. Asher | |
dc.contributor.author | Lopez, E. | |
dc.contributor.author | Lovis, C. | |
dc.contributor.author | Mayor, M. | |
dc.contributor.author | Micela, G. | |
dc.contributor.author | Molinari, E. | |
dc.contributor.author | Nascimbeni, V. | |
dc.contributor.author | Nava, C. | |
dc.contributor.author | Pepe, F. | |
dc.contributor.author | Phillips, D. F. | |
dc.contributor.author | Piotto, G. | |
dc.contributor.author | Sasselov, D. | |
dc.contributor.author | Ségransan, D. | |
dc.contributor.author | Sozzetti, A. | |
dc.contributor.author | Udry, S. | |
dc.contributor.author | Watson, C. | |
dc.date.accessioned | 2019-03-11T11:30:05Z | |
dc.date.available | 2019-03-11T11:30:05Z | |
dc.date.issued | 2019-04-11 | |
dc.identifier | 258117477 | |
dc.identifier | 12450a30-6be8-4702-97f8-95f2c898028a | |
dc.identifier | 85062279362 | |
dc.identifier | 000462410300064 | |
dc.identifier.citation | Rice , K , Malavolta , L , Mayo , A , Mortier , A , Buchhave , L A , Affer , L , Vanderburg , A , Lopez-Morales , M , Poretti , E , Zeng , L , Cameron , A C , Damasso , M , Coffinet , A , Latham , D W , Bonomo , A S , Bouchy , F , Charbonneau , D , Dumusque , X , Figueira , P , Martinez Fiorenzano , A F , Haywood , R D , Johnson , J A , Lopez , E , Lovis , C , Mayor , M , Micela , G , Molinari , E , Nascimbeni , V , Nava , C , Pepe , F , Phillips , D F , Piotto , G , Sasselov , D , Ségransan , D , Sozzetti , A , Udry , S & Watson , C 2019 , ' Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets ' , Monthly Notices of the Royal Astronomical Society , vol. 484 , no. 3 , pp. 3731-3745 . https://doi.org/10.1093/mnras/stz130 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | BibCode: 2019MNRAS.484.3731R | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/58531368 | |
dc.identifier.uri | https://hdl.handle.net/10023/17250 | |
dc.description | Funding: UK STFC consolidated grant number ST/M001296/1 (ACC). | en |
dc.description.abstract | Super-Earths belong to a class of planet not found in the Solar system, but which appear common in the Galaxy. Given that some super-Earths are rocky, while others retain substantial atmospheres, their study can provide clues as to the formation of both rocky and gaseous planets, and - in particular - they can help to constrain the role of photoevaporation in sculpting the exoplanet population. GJ 9827 is a system already known to host three super-Earths with orbital periods of 1.2, 3.6, and 6.2 d. Here, we use new HARPS-N radial velocity measurements, together with previously published radial velocities, to better constrain the properties of the GJ 9827 planets. Our analysis cannot place a strong constraint on the mass of GJ 9827 c, but does indicate that GJ 9827 b is rocky with a composition that is probably similar to that of the Earth, while GJ 9827 d almost certainly retains a volatile envelope. Therefore, GJ 9827 hosts planets on either side of the radius gap that appears to divide super-Earths into pre-dominantly rocky ones that have radii below ~1.5R⊕, and ones that still retain a substantial atmosphere and/or volatile components, and have radii above ~2R⊕. That the less heavily irradiated of the three planets still retains an atmosphere, may indicate that photoevaporation has played a key role in the evolution of the planets in this system. | |
dc.format.extent | 3557367 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Techniques: radial velocities | en |
dc.subject | Planets and satellites: composition | en |
dc.subject | Planets and satellites: detection | en |
dc.subject | Planets and satellites: fundamental parameters | en |
dc.subject | Planets and satellites: general | en |
dc.subject | Stars: individual: GJ 9827 (2MASS J23270480-0117108, EPIC 246389858, HIP 115752) | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Masses and radii for the three super-Earths orbiting GJ 9827, and implications for the composition of small exoplanets | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | 10.1093/mnras/stz130 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | http://adsabs.harvard.edu/abs/2019MNRAS.484.3731R | en |
dc.identifier.grantnumber | ST/M001296/1 | en |
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