GL 486行星系统的详细分析

论文标题

GL 486行星系统的详细分析

A detailed analysis of the Gl 486 planetary system

论文作者

Caballero, J. A., Gonzalez-Alvarez, E., Brady, M., Trifonov, T., Ellis, T. G., Dorn, C., Cifuentes, C., Molaverdikhani, K., Bean, J. L., Boyajian, T., Rodriguez, E., Sanz-Forcada, J., Osorio, M. R. Zapatero, Abia, C., Amado, P. J., Anugu, N., Bejar, V. J. S., Davies, C. L., Dreizler, S., Dubois, F., Ennis, J., Espinoza, N., Farrington, C. D., Lopez, A. Garcia, Gardner, T., Hatzes, A. P., Henning, Th., Herrero, E., Herrero-Cisneros, E., Kaminski, A., Kasper, D., Klement, R., Kraus, S., Labdon, A., Lanthermann, C., Bouquin, J. -B. Le, Gonzalez, M. J. Lopez, Luque, R., Mann, A. W., Marfil, E., Monnier, J. D., Montes, D., Morales, J. C., Palle, E., Pedraz, S., Quirrenbach, A., Reffert, S., Reiners, A., Ribas, I., Rodriguez-Lopez, C., Schaefer, G., Schweitzer, A., Seifahrt, A., Setterholm, B. R., Shan, Y., Shulyak, D., Solano, E., Sreenivas, K. R., Stefansson, G., Stuermer, J., Tabernero, H. M., Tal-Or, L., Brummelaar, T. ten, Vanaverbeke, S., von Braun, K., Youngblood, A., Zechmeister, M.

论文摘要

GL 486系统由附近的，相对较明亮的，弱的M3.5 V恒星组成，仅在8个PC上，其温暖的过境岩石行星约为1.3 r_terra和3.0 m_terra，非常适合传输和发射光谱以及测试3尔尿尿行星内部模型。为了准备未来的研究，我们收集了观察到的七个新转移的光曲线，并通过Maroon-X/Gemini North和Carmenes/Calar Alto远程望远镜获得了Cheops太空任务以及新的径向速度，以及先前发表的光谱仪和两种光谱仪和苔丝的光谱数据。我们还对Chara阵列和新的光度监测进行了干涉测量值，并进行了一组较小的望远镜。从干涉法中，我们测量了星形GL 486的肢体圆顶角尺寸。与校正后的Gaia EDR3视差一起，我们获得了恒星半径。我们还测量了p_rot〜49.9 d的恒星旋转周期，其XUV（5-920 AA）通量具有新的Hubble/stis数据的上限，并且首次是多种元素丰度（Fe，Mg，Mg，Si，Si，sr，sr，Zr，rb，rb）和C/O比率。此外，我们对系统中的其他组件（无论是恒星还是替代）施加了限制性限制。使用输入恒星参数以及径向速度和传输数据，我们确定行星GL 486 B的半径和质量在R_P = 1.343+/0.063 R_TERRA和M_P = 3.00 +/- 0.13 m_terra。从行星参数和恒星元素的丰度中，我们推断出行星内部结构和成分的最可能模型，这些模型与相对较小的金属芯相对于地球，深层硅酸盐地幔和薄的挥发性上层一致。借助所有这些成分，我们概述了GL 486 B大气研究的前景，尤其是即将进行的James Webb太空望远镜观测值（删节）。

The Gl 486 system consists of a very nearby, relatively bright, weakly active M3.5 V star at just 8 pc with a warm transiting rocky planet of about 1.3 R_Terra and 3.0 M_Terra that is ideal for both transmission and emission spectroscopy and for testing interior models of telluric planets. To prepare for future studies, we collected light curves of seven new transits observed with the CHEOPS space mission and new radial velocities obtained with MAROON-X/Gemini North and CARMENES/Calar Alto telescopes, together with previously published spectroscopic and photometric data from the two spectrographs and TESS. We also performed interferometric observations with the CHARA Array and new photometric monitoring with a suite of smaller telescopes. From interferometry, we measure a limb-darkened disc angular size of the star Gl 486. Together with a corrected Gaia EDR3 parallax, we obtain a stellar radius. We also measure a stellar rotation period at P_rot ~ 49.9 d, an upper limit to its XUV (5-920 AA) flux with new Hubble/STIS data, and, for the first time, a variety of element abundances (Fe, Mg, Si, V, Sr, Zr, Rb) and C/O ratio. Besides, we impose restrictive constraints on the presence of additional components, either stellar or substellar, in the system. With the input stellar parameters and the radial-velocity and transit data, we determine the radius and mass of the planet Gl 486 b at R_p = 1.343+/0.063 R_Terra and M_p = 3.00+/-0.13 M_Terra. From the planet parameters and the stellar element abundances, we infer the most probable models of planet internal structure and composition, which are consistent with a relatively small metallic core with respect to the Earth, a deep silicate mantle, and a thin volatile upper layer. With all these ingredients, we outline prospects for Gl 486 b atmospheric studies, especially with forthcoming James Webb Space Telescope observations (abridged).

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