J/A+A/644/A109ivo://CDS.VizieR/J/A+A/644/A109doi:10.26093/cds/vizier.36440109CDSGunar S.Schwartz P.Koza J.Heinzel P.2021-09-06T07:52:42Z2020-12-09T08:26:30ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frthe-sunspectroscopyThe solar radiation in the Lyman-alpha spectral line of hydrogen plays a significant role in the illumination of chromospheric and coronal structures, such as prominences, spicules, chromospheric fibrils, cores of coronal mass ejections, and solar wind. Moreover, it is important for the investigation of the heliosphere, Earth's ionosphere, and the atmospheres of planets, moons, and comets. We derive a reference quiet-Sun Lyman-alpha spectral profile that is representative of the Lyman-alpha radiation from the solar disk during a minimum of solar activity. This profile can serve as an incident radiation boundary condition for the radiative transfer modelling of chromospheric and coronal structures. Because the solar radiation in the Lyman lines is not constant over time but varies significantly with the solar cycle, we provide a method for the adaptation of the incident radiation Lyman line profiles (Lyman-alpha and higher lines) to a specific date. Moreover, we analyse how the change in the incident radiation influences the synthetic spectra produced by the radiative transfer modelling. We used SOHO/SUMER Lyman-alpha raster scans obtained without the use of the attenuator in various quiet-Sun regions on the solar disk. The observations were performed on three consecutive days (June 24, 25, and 26, 2008) during a period of minimum solar activity. The reference Lyman-alpha profile was obtained as a spatial average over eight available raster scans. To take into account the Lyman-alpha variation with the solar cycle, we used the LISIRD composite Lyman-alpha index. To estimate the influence of the change in the incident radiation in the Lyman lines on the results of radiative transfer models, we used a 2D prominence fine structure model. We present the reference quiet-Sun Lyman-alpha profile and a table of coefficients describing the variation of the Lyman lines with the solar cycle throughout the lifetime of SOHO. The analysis of the influence of the change in the incident radiation shows that the synthetic spectra are strongly affected by the modification of the incident radiation boundary condition. The most pronounced impact is on the central and integrated intensities of the Lyman lines. There, the change in the synthetic spectra can often have the same amplitude as the change in the incident radiation itself. The impact on the specific intensities in the peaks of reversed Lyman-line profiles is smaller but still significant. The hydrogen Halpha line can also be considerably affected, despite the fact that the Halpha radiation from the solar disk does not vary with the solar cycle.2020A&A...644A.109Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/644/A109CatalogResearchIsServedByTAP VizieR generic servicerelated-toVI/152 : SOVAP-PICARD total solar irradiance (Meftah+, 2016)J/A+A/581/A26 : Solar Lyman irradiance line profiles (Lemaire+, 2015)J/A+A/611/A1 : SOLAR/SOLSPEC Spectral Irradiance - 0.5-3000nm (Meftah+, 2018)J/A+A/624/A36 : EUV irradiances of the quiet Sun (Del Zanna, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/644/A109https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/644/A109http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/644/A109https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/644/A109https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/644/A109http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/644/A109GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/644/A109/tablea1Reference quiet-Sun Lyman-alpha profilerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength in the vacuum0.1nmem.wlfloatI(Hz)Specific Intensity1e-08mW.m**-2.Hz**-1spect.line.intensityfloatI(0.1nm)Specific Intensity1e+06mW.m**-2.nm**-1spect.line.intensityfloatJ/A+A/644/A109/tableb1Coefficients - variation with solar cyclerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateSpecified datetime.epochnullableIrradianceLISIRD Lyman-alpha index (smoothed) (1)0.01W.m**-2phot.fluxfloatCoeff-L1Coefficient for Lyman-alpha for 2008/06/24stat.fit.paramfloatCoeff-higherCoefficient for higher Lyman lines for 1996/05/15stat.fit.paramfloatJ/A+A/644/A109/tablea2Symmetrized reference Lyman-alpha half-profilerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlambdaWavelength in the vacuum0.1nmem.wlfloatI(Hz)Specific Intensity1e-08mW.m**-2.Hz**-1spect.line.intensityfloatI(0.1nm)Specific Intensity1e+06mW.m**-2.nm**-1spect.line.intensityfloat