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Evaluation Using SOHO SWAN and MAVEN EUVM Lyman Measurements View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Archive Ouverte en Sciences de l'Information et de la Communication Multiple Scattering Effects in the Interplanetary Medium: Evaluation Using SOHO SWAN and MAVEN EUVM Lyman α Measurements Eric Quémerais, Edward Thiemann, Martin Snow, Stéphane Ferron, Walter Schmidt To cite this version: Eric Quémerais, Edward Thiemann, Martin Snow, Stéphane Ferron, Walter Schmidt. Multiple Scat- tering Effects in the Interplanetary Medium: Evaluation Using SOHO SWAN and MAVENEUVM Lyman α Measurements. Journal of Geophysical Research Space Physics, American Geophysical Union/Wiley, 2019, 124 (6), pp.3949-3960. 10.1029/2019JA026674. insu-02151127 HAL Id: insu-02151127 https://hal-insu.archives-ouvertes.fr/insu-02151127 Submitted on 11 Sep 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. RESEARCH ARTICLE Multiple Scattering Effects in the Interplanetary 10.1029/2019JA026674 Medium: Evaluation Using SOHO SWAN Key Points: and MAVEN EUVM Lyman • We present a new method to evaluate the solar flux toward any object in the Measurements solar system • We evaluate the contribution of 1 2 2 3 multiple scattering to the Eric Quémerais , Edward Thiemann , Martin Snow , Stéphane Ferron , interplanetary ultraviolet emission and Walter Schmidt4 1LATMOS-OVSQ, Université Versailles Saint-Quentin, Guyancourt, France, 2Laboratory for Atmospheric and Space Correspondence to: Physics, University of Colorado Boulder, Boulder, CO, USA, 3ACRI-ST, Guyancourt, France, 4Finnish Meteorological E. Quémerais, Institute, Helsinki, Finland [email protected] Citation: Abstract Interplanetary background measurements can be used to derive the solar flux that is Quemerais, E., Thiemann, E. M. B., illuminating the atoms in the interplanetary medium. We present a new algorithm combining Snow, M., Ferron, S., & Schmidt, W. measurements from the Solar Wind ANisotropies (SWAN)-Solar Heliospheric Observatory (SOHO) (2019). Multiple scattering effects in the interplanetary medium: Lyman photometer with Earth-based solar flux measurements to derive the solar illuminating flux at Evaluation using SOHO SWAN Lyman in any direction along the ecliptic plane. The modulations of the solar flux and the interplanetary and MAVEN EUVM Lyman background intensity are proportional. The proportionality coefficient is a direct measurement of the measurements. Journal of Geophysical Research: Space Physics, 124, fraction of the interplanetary brightness that is due to single scattering in the interplanetary medium. We 3949–3960. https://doi.org/10.1029/ find that for an observer at 1 AU from the Sun, single scattering photons represent roughly 70% of the total 2019JA026674 brightness. This new algorithm is tested by a comparison with actual measurements from the Extreme Ultraviolet Monitor (EUVM)-Mars Atmosphere and Volatile EvolutioN (MAVEN) solar monitor in orbit Received 1 MAR 2019 around Mars since 2014. Accepted 16 MAY 2019 Accepted article online 23 MAY 2019 Published online 20 JUN 2019 1. Introduction The heliosphere is filled with neutral atoms coming from the interstellar medium, mainly hydrogen and helium. Because of the relative motion between the solar system and the local interstellar cloud, these neu- tral atoms can reach the inner heliosphere before they are ionized by charge exchange with solar wind protons or photoionized by extreme ultraviolet (EUV) photons. The direction from which the interstellar atoms are coming is called upwind. The upwind direction for hydrogen atoms has been determined by hydro- gen absorption cell measurements (Quémerais et al., 1999). It is defined as 252.3 ± 0.7◦ in ecliptic longitude and 8.7 ± 0.9◦ in ecliptic latitude. Downwind is the opposite direction in the sky. In the inner heliosphere, the neutral atoms are mainly ionized by charge exchange with solar wind protons or by photoionization. The remaining neutrals resonantly scatter the solar photons. This emission is called the interplanetary ultra- violet background. Its main component corresponds to resonant scattering of the solar H Lyman photons (121.56 nm). The interplanetary background at Lyman has been studied for almost 50 years. Since the first measure- ments by Bertaux and Blamont (1971) and Thomas and Krassa (1971), several instruments have obtained data of this emission due to the backscattering of the solar Lyman photons by hydrogen atoms in the interplanetary medium (Ajello et al., 1987; Quémerais et al., 2013). The largest data set of interplane- tary background measurements, spanning more than two decades, has been obtained by the Solar Wind ANisotropies (SWAN) instrument aboard the Solar Heliospheric Observatory (SOHO) spacecraft (Bertaux et al., 1995). Although it was not expected originally, it was found that the study of the SWAN data could ©2019. The Authors. This is an open access article under the be used to infer the spatial and temporal variations of the solar illuminating flux at Lyman . Quémerais terms of the Creative Commons and Bertaux (2002) implemented an algorithm that allowed one to derive the flux emitted by the Sun at Attribution-NonCommercial-NoDerivs any given moment and in any direction based on a linear correlation obtained between the ratio of SWAN License, which permits use and distribution in any medium, provided background measurements with the variations of the solar flux as monitored from the Earth. the original work is properly cited, the use is non-commercial and no One application of this algorithm was to estimate the solar Lyman irradiance at any planet in the solar modifications or adaptations are made. system at any time. This method complements the time-shifting method which is usually used to evaluate QUÉMERAIS ET AL. MULTIPLE SCATTERING EFFECTS IN IPM 3949 Journal of Geophysical Research: Space Physics 10.1029/2019JA026674 the flux changes between the irradiance measured at Earth and the flux illuminating a planet in a different part of the solar system. The time-shifting method neglects temporal variations of the solar flux and simply rotates the Sun to find when the area of the Sun illuminating the planet at the time of observation was last aligned with Earth. It can be improved by finding the next measurement when the same region is aligned with Earth and by using a linear interpolation between the two flux values (see Thiemann et al., 2017). However, due to the lack of actual measurements of the solar flux made at a planet, it was previously not possible to evaluate if the SWAN method is really more efficient than the time-shifting method. The Mars Atmosphere and Volatile EvolutioN (MAVEN; Jakosky et al., 2015) mission orbiting Mars since 2014 allows us to finally answer this question. MAVEN includes the Extreme Ultraviolet Monitor (EUVM, Eparvier et al., 2015), which measures calibrated solar Lyman irradiance at Mars. This is the first time that an instrument monitoring the solar input has obtained data over a long period of time while in orbit around a planet other than the Earth, in this case Mars. The measurements of EUVM-MAVEN give us the opportunity to validate the method of estimating the solar irradiance in a given direction using SWAN data. Section 2 will introduce a general method to derive the solar flux from the interplanetary background data. This is an improvement over the original method presented in Quémerais and Bertaux (2002). The new method allows us to express the relation between the modulations of the solar flux and the interplanetary background as a function of single and multiple scattering terms in the interplanetary medium. In section 3, we will apply this relation to the comparison of the EUVM-MAVEN and SWAN-SOHO data sets in order to determine the relevant parameters. Finally, we will apply the new method to estimate the solar Lyman flux toward Mars from the SWAN data and compare the results to the EUVM measurements and to the time-shifting method. 2. Retrieving Solar Flux From the Interplanetary Background 2.1. Modulations of the Interplanetary Background Data The hydrogen atoms present in the interplanetary medium are illuminated by the solar H Lyman flux. Therefore, temporal and spatial variations of the solar irradiance are reflected in the interplanetary back- ground. Quémerais and Bertaux (2002) have shown that the SWAN-SOHO maps of the interplanetary background emission can be used on a routine basis to produce maps of the relative variation of the solar illu- minating flux at Lyman . In this study, we will improve the method developed by Quémerais and Bertaux (2002). The interplanetary background data have been modeled by various authors. The most complete calculations have been described by Quémerais and Izmodenov (2002) and Katushkina et al. (2015). Following Quémerais (2002), we can express the interplanetary background intensity at frequency as a line of sight integration of the local emissivity toward the observer multiplied by the extinction probability between the scattering point and the observer. ∞ ⃗ ⃗, ⃗ , ⃗ ⃗ , ⃗ , − (⃗r+sΩ,⃗r) , I(r Ω )=∫ (r + sΩ −Ω )e ds (1) 0 where ⃗r is the position of the observer, and Ω⃗ the direction of the line of sight. The optical thickness between ⃗ the scattering point and the observer is expressed by (⃗r + sΩ, ⃗r). The local emissivity at each point can be split between the single scattering term and the multiple scattering, = 0 + m . The single scattering emissivity is proportional to the product of solar flux at frequency , the extinction between the Sun and the scattering point, the H Lyman scattering cross section, and the local scattering profile at frequency .
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