Current linear structure inversions with mixed modes are unreliable for subgiant stars because the mode kernels change too rapidly with evolution, while main-sequence inversions remain valid.
Equation of state and helioseismic inversions
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abstract
Inversions to determine the squared isothermal sound speed and density within the Sun often use the helium abundance Y as the second parameter. This requires the explicit use of the equation of state (EOS), thus potentially leading to systematic errors in the results if the equations of state of the reference model and the Sun are not the same. We demonstrate how this potential error can be suppressed. We also show that it is possible to invert for the intrinsic difference in the adiabatic exponent Gamma_1 between two equations of state. When applied to solar data such inversion rules out the EFF equation of state completely, while with existing data it is difficult to distinguish between other equations of state.
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Linearity of Structure Kernels in Main-sequence and Subgiant Solar-like Oscillators
Current linear structure inversions with mixed modes are unreliable for subgiant stars because the mode kernels change too rapidly with evolution, while main-sequence inversions remain valid.