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A New Third Planet and the Dynamical Architecture of the HD 33142 Planetary System

  • Authors: Trifon Trifonov, Anna Wollbold, Martin Kürster, Jan Eberhardt, Stephan Stock, Thomas Henning, Sabine Reffert, R. Paul Butler, Steven S. Vogt, Ansgar Reiners, Man Hoi Lee, Bertram Bitsch, Mathias Zechmeister, Florian Rodler, Volker Perdelwitz, Lev Tal-Or, Jan Rybizki, Paul Heeren, Davide Gandolfi, Oscar Barragán, Olga Zakhozhay, Paula Sarkis, Marcelo Tala Pinto, Diana Kossakowski, Vera Wolthoff, Stefan S. Brems, Vera Maria Passegger

Trifon Trifonov et al 2022 The Astronomical Journal 164 .

  • Provider: AAS Journals

Caption: Figure 7.

N-body simulations of the HD 33142 system, including stellar evolution effects on the orbital evolution, in particular the planetary semimajor axis a (colored lines). Initial conditions from the N-body simulations were adopted from the stable median posterior values presented in Table 3. The evolution of the stellar radius (dashed curve and the underlying gray area) is expressed in astronomical units. The WD phase is off-scale, since the stellar radius at age 3.2 Gyr is only ∼4 × 10−5 au.

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