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

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Název: Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS
Autoři: Lacedelli, G., Wilson, T. G., Malavolta, L., Hooton, M. J., Collier Cameron, A., Alibert, Y., Mortier, A., Bonfanti, A., Haywood, R. D., Hoyer, S., Piotto, G., Bekkelien, A., Vanderburg, A. M., Benz, W., Dumusque, X., Deline, A., Lopez-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., Palle, E., Bourrier, V, Nascimbeni, V, Alonso, R., Anglada, G., Barczy, T., Barrado y Navascues, D., 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., Floren, H. G., Fortier, A., Fridlund, Malcolm, 1952, Futyan, D., Gandolfi, D., Gillon, M., Gudel, M., Guterman, P., Harutyunyan, A., Heng, K., Isaak, K. G., Jenkins, J. M., Kiss, L., Laskar, J., Lecavelier des Etangs, A., Lendl, M., Lovis, C., Magrin, D., Marafatto, L., Martinez Fiorenzano, A. F., 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., Segransan, D., Serrano, L. M., Simon, A. E., Smith, A. M. S., Steinberger, M., Steller, M., Szabo, Gy, Thomas, N., Twicken, J. D., Udry, S., Walton, N., Winn, J. N.
Zdroj: Monthly Notices of the Royal Astronomical Society. 511(3):4551-4571
Témata: planets and satellites: fundamental parameters, techniques: radial velocities, techniques: photometric, stars: individual: TOI-561 (TIC 377064495, Gaia EDR3 3850421005290172416), planets and satellites: interiors
Popis: 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-circle plus, M = 2.0 M-circle plus), c (P = 10.78 d, R = 2.91 R-circle plus, M = 5.4 M-circle plus), d (P = 25.7 d, R = 2.82 R-circle plus, M = 13.2 M-circle plus), and e (P = 77 d, R = 2.55 R-circle plus, M = 12.6 R-circle plus). 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 (rho(b) = 3.8 +/- 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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  Data: Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS
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  Data: <i>Monthly Notices of the Royal Astronomical Society</i>. 511(3):4551-4571
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  Label: Subject Terms
  Group: Su
  Data: <searchLink fieldCode="DE" term="%22planets+and+satellites%3A+fundamental+parameters%22">planets and satellites: fundamental parameters</searchLink><br /><searchLink fieldCode="DE" term="%22techniques%3A+radial+velocities%22">techniques: radial velocities</searchLink><br /><searchLink fieldCode="DE" term="%22techniques%3A+photometric%22">techniques: photometric</searchLink><br /><searchLink fieldCode="DE" term="%22stars%3A+individual%3A+TOI-561+%28TIC+377064495%22">stars: individual: TOI-561 (TIC 377064495</searchLink><br /><searchLink fieldCode="DE" term="%22Gaia+EDR3+3850421005290172416%29%22">Gaia EDR3 3850421005290172416)</searchLink><br /><searchLink fieldCode="DE" term="%22planets+and+satellites%3A+interiors%22">planets and satellites: interiors</searchLink>
– Name: Abstract
  Label: Description
  Group: Ab
  Data: 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-circle plus, M = 2.0 M-circle plus), c (P = 10.78 d, R = 2.91 R-circle plus, M = 5.4 M-circle plus), d (P = 25.7 d, R = 2.82 R-circle plus, M = 13.2 M-circle plus), and e (P = 77 d, R = 2.55 R-circle plus, M = 12.6 R-circle plus). 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 (rho(b) = 3.8 +/- 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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      – Type: doi
        Value: 10.1093/mnras/stac199
    Languages:
      – Text: English
    PhysicalDescription:
      Pagination:
        PageCount: 21
        StartPage: 4551
    Subjects:
      – SubjectFull: planets and satellites: fundamental parameters
        Type: general
      – SubjectFull: techniques: radial velocities
        Type: general
      – SubjectFull: techniques: photometric
        Type: general
      – SubjectFull: stars: individual: TOI-561 (TIC 377064495
        Type: general
      – SubjectFull: Gaia EDR3 3850421005290172416)
        Type: general
      – SubjectFull: planets and satellites: interiors
        Type: general
    Titles:
      – TitleFull: Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS
        Type: main
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              Type: published
              Y: 2022
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          Titles:
            – TitleFull: Monthly Notices of the Royal Astronomical Society
              Type: main
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