TOI-2015b：与外异星行星TOI-2015c发生强引力相互作用的次月球质行星
摘要
TOI-2015是一个已知的系外行星系统，围绕M4型恒星，包含一个轨道周期为3.35天的可探测次月球质行星TOI-2015b，伴随一个不可探测的伴星TOI-2015c。我们使用MAROON-X光谱仪获取了高精度的径向速度测量，并收集了来自多个网络的高精度光度数据。我们通过结合光学光谱、贝叶斯模型平均(BMA)和光谱能谱(Spectral Energy Distribution, SED)分析对目标星体进行重新表征。TOI-2015主机星是一颗K=10.3mag的M4型恒星，金属丰度为[Fe/H]=-0.31+/-0.16，有效温度Teff=3200K。我们的光动力学分析strongly favor 5:3共振配置，在此情景下，行星b的轨道周期为3.34天，质量为Mp=9.02+/-0.34Me，半径为Rp=3.309+/-0.012Re，密度为rhop= 1.40+/-0.06g/cm3，表明其为类似海王星的成分。其transit exhibits large (>1hr) timing variations，表明系统中存在外异星行星。我们对高分辨率径向速度测量、光度数据和TTV进行全局分析，推断TOI-2015第二个行星TOI-2015c处于不可探测配置。TOI-2015c的轨道周期为Pc=5.583天，质量为Mp=8.91+0.38-0.40Me。TOI-2015b和TOI-2015c的动力学配置可用于约束系统的行星形成和迁移历史。基于质量-半径成分模型，TOI-2015b为富含水或岩石的行星，可能拥有氦-氢外壳。此外，TOI-2015b具有高传输光谱指数(TSM=149)，使其成为未来使用JWST进行传输光谱观测的优选目标，以限定行星大气组成。这类观测也有助于打破行星内部结构模型中的degeneracy。
关键词
引用
@article{arxiv.2502.07074,
title = {TOI-2015b: a sub-Neptune in strong gravitational interaction with an outer non-transiting planet},
author = {K. Barkaoui and J. Korth and E. Gaidos and E. Agol and H. Parviainen and F. J. Pozuelos and E. Palle and N. Narita and S. Grimm and M. Brady and J. L. Bean and G. Morello and B. V. Rackham and A. J. Burgasser and V. Van Grootel and B. Rojas-Ayala and A. Seifahrt and E. Marfil and V. M. Passegger and M. Stalport and M. Gillon and K. A. Collins and A. Shporer and S. Giacalone and S. Yalçınkaya and E. Ducrot and M. Timmermans and A. H. M. J. Triaud and J. de Wit and A. Soubkiou and C. N. Watkins and C. Aganze and R. Alonso and P. J. Amado and R. Basant and Ö. Bastürk and Z. Benkhaldoun and A. Burdanov and Y. Calatayud-Borras and J. Chouqar and D. M. Conti and K. I. Collins and F. Davoudi and L. Delrez and C. D. Dressing and J. de Leon and M. D'evora-Pajares and B. O. Demory and G. Dransfield and E. Esparza-Borges and G. Fern'andez-Rodriguez and I. Fukuda and A. Fukui and P. P. M. Gallardo and L. Garcia and N. A. Garcia and M. Ghachoui and S. Gerald'ia-González and Y. Gómez Maqueo Chew and J. González-Rodríguez and M. N. Günther and Y. Hayashi and K. Horne and M. J. Hooton and C. C. Hsu and K. Ikuta and K. Isogai and E. Jehin and J. M. Jenkins and K. Kawauchi and T. Kagetani and Y. Kawai and D. Kasper and J. F. Kielkopf and P. Klagyivik and G. Lacedelli and D. W. Latham and F. Libotte and R. Luque and J. H. Livingston and L. Mancini and B. Massey and M. Mori and S. Muñoz Torres and F. Murgas and P. Niraula and J. Orell-Miquel and David Rapetti and R. Rebolo-Lopez and G. Ricker and R. Papini and P. P. Pedersen and A. Peláez-Torres and J. A. Pérez-Prieto and E. Poultourtzidis and P. M. Rodriguez and D. Queloz and A. B. Savel and N. Schanche and M. Sanchez-Benavente and L. Sibbald and R. Sefako and S. Sohy and A. Sota and R. P. Schwarz and S. Seager and D. Sebastian and J. Southworth and M. Stangret and G. Stefánsson and J. Stürmer and G. Srdoc and S. J. Thompson and Y. Terada and R. Vanderspek and G. Wang and N. Watanabe and F. P. Wilkin and J. Winn and R. D. Wells and C. Ziegler and S. Zúñiga-Fernández},
journal= {arXiv preprint arXiv:2502.07074},
year = {2025}
}
备注
The paper has been accepted for publication in Astronomy and Astrophysics