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arXiv · 1710.07038

Voyager 1/UVS Lyman $α$ measurements at the distant heliosphere (90-130AU): unknown source of additional emission

O. A. Katushkina·E. Quemerais·V. V. Izmodenov·R. Lallement·B. R. Sandel
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Abstract

In this work, we present for the first time the Lyman $α$ intensities measured by Voyager 1/UVS in 2003-2014 (at 90-130 AU from the Sun). During this period Voyager 1 measured the Lyman $α$ emission in the outer heliosphere at an almost fixed direction close to the upwind (that is towards the interstellar flow). The data show an unexpected behavior in 2003-2009: the ratio of observed intensity to the solar Lyman $α$ flux is almost constant. Numerical modelling of these data is performed in the frame of a state-of-art self-consistent kinetic-MHD model of the heliospheric interface (Izmodenov & Alexashov, 2015). The model results, for various interstellar parameters, predict a monotonic decrease of intensity not seen in the data. We propose two possible scenarios that explain the data qualitatively. The first is the formation of a dense layer of hydrogen atoms near the heliopause. Such a layer would provide an additional backscattered Doppler shifted Lyman $α$ emission, which is not absorbed inside the heliosphere and may be observed by Voyager. About 35 R of intensity from the layer is needed. The second scenario is an external non-heliospheric Lyman $α$ component, which could be galactic or extragalactic. Our parametric study shows that $\sim$25 R of additional emission leads to a good qualitative agreement between the Voyager 1 data and the model results.

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O. A. Katushkina, E. Quemerais, V. V. Izmodenov, R. Lallement, B. R. Sandel. 2017-10-19. Voyager 1/UVS Lyman $α$ measurements at the distant heliosphere (90-130AU): unknown source of additional emission. https://doi.org/10.1002/2017ja024205

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