调查与Cheops，Harps-N和Tess的TOI-561系统行星的结构和内部结构

论文标题

调查与Cheops，Harps-N和Tess的TOI-561系统行星的结构和内部结构

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

论文作者

Lacedelli, G., Wilson, T. G., Malavolta, L., Hooton, M. J., Cameron, A. Collier, Alibert, Y., Mortier, A., Bonfanti, A., Haywood, R. D., Hoyer, S., Piotto, G., Bekkelien, A., Vanderburg, A. M., Benz, W., Dumusque, X., Deline, A., López-Morales, M., Borsato, L., Rice, K., Fossati, L., Latham, D. W., Brandeker, A., Poretti, E., Sousa, S. G., Sozzetti, A., Salmon, S., Burke, C. J., Van Grootel, V., Fausnaugh, M. M., Adibekyan, V., Huang, C. X., Osborn, H. P., Mustill, A. J., Pallé, E., Bourrier, V., Nascimbeni, V., Alonso, R., Anglada, G., Bárczy, T., Navascues, D. Barrado y, Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Billot, N., Bonfils, X., Broeg, C., Buchhave, L. A., Cabrera, J., Charnoz, S., Cosentino, R., Csizmadia, Sz., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O., Demory, B. -O., Ehrenreich, D., Erikson, A., Esparza-Borges, E., Florén, H. -G., Fortier, A., Fridlund, M., Futyan, D., Gandolfi, D., Ghedina, A., Gillon, M., Güdel, M., Gutermann, P., Harutyunyan, A., Heng, K., Isaak, K. G., Jenkins, J. M., Kiss, L., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Magrin, D., Marafatto, L., Fiorenzano, A. F. Martinez, Maxted, P. F. L., Mayor, M., Micela, G., Molinari, E., Murgas, F., Narita, N., Olofsson, G., Ottensamer, R., Pagano, I., Pasetti, A., Pedani, M., Pepe, F. A., Peter, G., Phillips, D. F., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Ribas, I., Santos, N. C., Sasselov, D., Scandariato, G., Seager, S., Ségransan, D., Serrano, L. M., Simon, A. E., Smith, A. M. S., Steinberger, M., Steller, M., Szabó, Gy., Thomas, N., Twicken, J. D., Udry, S., Walton, N., Winn, J. N.

论文摘要

我们提出了通过将先前发布的数据与苔丝和Cheops光度法结合在一起获得的TOI-561行星系统的精确表征，以及一组新的$ 62 $ HARPS-N径向速度（RVS）。 Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b ($P = 0.45$ d, $R = 1.42$ R$_\oplus$, $M = 2.0$ M$_\oplus$), c ($P = 10.78$ d, $R = 2.91$ R$_\oplus$, $M = 5.4$ M$_\oplus$), d （$ p = 25.7 $ d，$ r = 2.82 $ r $ _ \ oplus $，$ m = 13.2 $ m $ _ \ oplus $）和E（$ p = 77 $ d，$ r = 2.55 $ r $ _ \ oplus $，$ m = 12.6 $ m $ _ $ _ \ oplus $）。此外，我们在RVS中确定了一个额外的长期信号（$> 450 $ d），这可能是由于外部行星伴侣或出色的磁性活动。为四个行星获得的精确质量和半径使我们能够进行内部结构和大气逃生建模。 TOI-561 b被确认为最低密度（$ρ_ {\ rm b} = 3.8 \ pm 0.5 $ g cm $^{ - 3} $）Ultra-short期（USP）Planet已知迄今已知的行星，并且寄主星的低金属性使其与一般的Bulk密度密度密度稳定性一致。根据我们的室内结构建模，行B基本上没有气体包膜，并且可以容纳一定数量的水。相比之下，除了可能大的水层外，TOI-561 C，D和E可能保留了H/HE信封。推断的行星组合物表明不同的大气进化路径，行星B和C经历了重大气体损失，并且行星D和E显示出与原始含量一致的大气含量。 USP星球的独特性，长期行星TOI-561 E的存在以及复杂的架构使该系统成为随访研究的吸引人目标。

We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of $62$ HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b ($P = 0.45$ d, $R = 1.42$ R$_\oplus$, $M = 2.0$ M$_\oplus$), c ($P = 10.78$ d, $R = 2.91$ R$_\oplus$, $M = 5.4$ M$_\oplus$), d ($P = 25.7$ d, $R = 2.82$ R$_\oplus$, $M = 13.2$ M$_\oplus$) and e ($P = 77$ d, $R = 2.55$ R$_\oplus$, $M = 12.6$ M$_\oplus$). Moreover, we identify an additional, long-period signal ($>450$ d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density ($ρ_{\rm b} = 3.8 \pm 0.5$ g cm$^{-3}$) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies.

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