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Transit and radial velocity observations continuously discover an increasingnumber of exoplanets. However, when it comes to the composition of the observedplanets the data are compatible with several interior structure models. Thus, aplanetary parameter sensitive to the planet's density distribution could helpconstrain this large number of possible models even further. We aim toinvestigate to what extent an exoplanet's interior can be constrained in termsof core mass and envelope metallicity by taking the tidal Love number k_2 intoaccount as an additional possibly observable parameter. Because it is the onlyplanet with an observationally determined k_2, we constructed interior modelsfor the Hot Jupiter exoplanet HAT-P-13b by solving the equations of hydrostaticequilibrium and mass conservation for different boundary conditions. Inparticular, we varied the surface temperature and the outer temperatureprofile, as well as the envelope metallicity within the widest possibleparameter range. We also considered atmospheric conditions that are consistentwith nongray atmosphere models. For all these models we calculated the Lovenumber k_2 and compared it to the allowed range of k_2 values that could beobtained from eccentricity measurements of HAT-P-13b. We use the example ofHAT-P-13b to show the general relationships between the quantities temperature,envelope metallicity, core mass, and Love number of a planet. For any given k_2value a maximum possible core mass can be determined. For HAT-P-13b we findMcore < 27 ME, based on the latest eccentricity measurement. We are able toconstrain both the envelope and bulk metallicity of HAT-P-13b to 1 -- 11 timesstellar metallicity and the extension of the isothermal layer in the planet'satmosphere to 3 -- 44 bar. Assuming equilibrium tidal theory, we find lowerlimits on the tidal Q consistent with 10^3 - 10^5.

Constraining the interior of extrasolar giant planets with the tidal Love number k_2 using the example of HAT-P-13b