Search

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation
Large resolution
Hi-Resolution Export to PDF

Spin–Orbit Geometry of AU Mic b and c from Back-to-back Transits Observed Contemporaneously with Magellan PFS, LCOGT, and CHEOPS

  • Authors: Zitao Lin, Gyula M. Szabó, Krzysztof Sz. Zieliński, Zhen Guo, Zoltán Garai, R. Paul Butler, Alexis Brandeker, Johanna K. Teske, Davide Gandolfi, Haochuan Yu, Nicolas Billot, Suzanne Aigrain, Michael Cretignier, Liang Wang, Xuan Mao, Wei M. Yuan, Hongpeng Lu, Jiayin Li, Yann Alibert, Ádám Boldog, Vincent Bourrier, Giovanni Bruno, Jeffrey D. Crane, Fei Dai, Olivier D. S. Demangeon, Alexis Heitzmann, Zhecheng Hu, Pradip Karmakar, Levente Kriskovics, Monika Lendl, He Y. Liu, Pierre F. L. Maxted, Hugh P. Osborn, Gaetano Scandariato, Stephen A. Shectman, Sérgio G. Sousa, Soléne Ulmer-Moll, Mu-Tian Wang, Thomas G. Wilson, Sharon X. Wang

Zitao Lin et al 2026 The Astrophysical Journal Letters 1005 .

  • Provider: AAS Journals

Caption: Figure 6.

Upper panel: long-term ground-based photometric observations and the CHEOPS light curve, plotted with the best-fit starry spot model. The data are phase-folded to the rotation period of 4.86 days. We employ spherical harmonics up to the third degree to construct the spot model. Lower panel: the predicted RV variation derived from the best-fit spot model compared to the observed PFS RVs. The spot model can qualitatively match the variation trend of the observed data.

Other Images in This Article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Image in this article
Copyright and Terms & Conditions

Additional terms of reuse