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Following the derivation of a more accurate model of the evolution of thesolar Lyman-$\alpha$ line with the changing solar activity byKowalska-leszczynska et al. 2018 (IKL18) than the formerly used model byTarnopolski et al. 2009 (ST09), we investigate potential consequences thatadoption of the resulting refined model of radiation pressure has for the modeldistribution of interstellar neutral (ISN) H in the inner heliosphere and onthe interpretation of selected observations. We simulated the ISN H densitiesusing the two alternative radiation pressure models and identical models of allother factors affecting the ISN H distribution. We found that during most ofthe solar cycle, the IKL18 model predicts larger densities of ISN H and PUIsthan ST09 in the inner heliosphere, especially in the downwind hemisphere.However, the density of ISN H at the termination shock estimated by Bzowski etal. 2008 obtained using ST09 does not need revision, and the detection of ISN Dby IBEX is supported. However, we point out the existence of a considerableabsorption of a portion of the solar Lyman-$\alpha$ spectral flux inside theheliosphere. Therefore, the model of radiation pressure for ISN H is stilllikely to need revision, and hence the available models of ISN H are notself-consistent.

astrophysical journal/the astrophysical journal

Evolution of the solar Ly-$\alpha$ line profile during the solar cycle.  II. How accurate is the present radiation pressure paradigm for interstellar  neutral H in the heliosphere?