Our analysis shows that the tidal Love number k 2 is a very useful parameter for studying the interior of exoplanets. Assuming equilibrium tidal theory, we find lower limits on the tidal Q consistent with 10 3−10 5.Ĭonclusions. These terms and conditions (Terms) govern your use of and access to TIDAL’s content and streaming services, and associated websites and applications (the TIDAL Service). With this external boundary condition and our new k 2-interval we are able to constrain both the envelope and bulk metallicity of HAT-P-13b to 1−11 times stellar metallicity and the extension of the isothermal layer in the planet’s atmosphere to 3−44 bar.

We favor models that are consistent with our model atmosphere, which gives us the temperature of the isothermal region as ~2100 K. For HAT-P-13b we find M core < 27 M ⊕, based on the latest eccentricity measurement. For any given k 2 value a maximum possible core mass can be determined. We use the example of HAT-P-13b to show the general relationships between the quantities temperature, envelope metallicity, core mass, and Love number of a planet. For all these models we calculated the Love number k 2 and compared it to the allowed range of k 2 values that could be obtained from eccentricity measurements of HAT-P-13b. We also considered atmospheric conditions that are consistent with nongray atmosphere models. In particular, we varied the surface temperature and the outer temperature profile, as well as the envelope metallicity within the widest possible parameter range. Sport this New Era Black NFL Tidal 9FIFTY Snapback Hat This hat features a front embroidered team logo on a structured crown with shark tooth front panel. Because it is the only planet with an observationally determined k 2, we constructed interior models for the Hot Jupiter exoplanet HAT-P-13b by solving the equations of hydrostatic equilibrium and mass conservation for different boundary conditions. We aim to investigate to what extent an exoplanet’s interior can be constrained in terms of core mass and envelope metallicity by taking the tidal Love number k 2 into account as an additional, possibly observable parameter. Thus, a planetary parameter sensitive to the planet’s density distribution could help constrain this large number of possible models even further.Īims. However, when it comes to the composition of the observed planets the data are compatible with several interior structure models.

Transit and radial velocity observations continuously discover an increasing number of exoplanets. of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USAģ Astrophysical Institute and University-Observatory, Schillergässchen 2–3, 07745 Jena, GermanyĬontext. Redmer 1ġ Institute of Physics, University of Rostock, 18051 Rostock, GermanyĮ-mail: Dept. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes

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