ERRATUM: “SOLAR PHOTOIONIZATION RATES FOR INTERSTELLAR NEUTRALS IN THE INNER HELIOSPHERE: H, He, O, AND Ne” (2014, ApJS, 210, 12)

Bochsler, P.; Kucharek, H.; Möbius, E.; Bzowski, M.; Sokół, J. M.; Didkovsky, L. V.; Wieman, Seth

doi:10.1088/0067-0049/211/2/32

Cited by 5 publications

(14 citation statements)

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“…The most commonly used solar EUV proxies are the radio flux in 10.7 cm, F10.7 index (Tapping 2013), the Magnesium II core-to-wing index, MgIIc/w (Heath & Schesinger 1986), the solar Lyman-α flux (Woods et al 2000), and the integrated flux from the SOHO/CELIAS/SEM measurements (Judge et al 1998). These were used in various combinations to calculate the photoionization rates for H, He, Ne, and O by, e.g., Bzowski et al (2013a), Bochsler et al (2014), Sokół & Bzowski (2014).…”

Section: Photoionizationmentioning

confidence: 99%

“…The primary resolution in time is CR; however, we calculate the photoionization rates for daily time series for the TIMED/SEE data period only. We do not calculate the daily series for periods when we use the EUV proxies since the correlation changes (see, e.g., Bochsler et al 2014).…”

Section: Photoionizationmentioning

confidence: 99%

“…They calculated the latter reaction following the methodology proposed by Ruciński & Fahr (1989, 1991, which was next developed by Bzowski (2008) based on measurements of electron temperature by Helios inside 1 au and Ulysses inside 5 au. Sokół et al (2019a) calculated the photoionization rates using a multi-component model based on EUV spectral data and the solar EUV proxy data (Bzowski et al 2013a,b;Bochsler et al 2014). However, the multi-component model for photoionization rates is sensitive to calibration issues of the component data, as discussed by, e.g., Sokół & Bzowski (2014).…”

Section: Introductionmentioning

confidence: 99%

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Sun–Heliosphere Observation-based Ionization Rates Model

Sokół

McComas

Bzowski

et al. 2020

ApJ

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The solar wind (SW) and the extreme ultraviolet (EUV) radiation modulate fluxes of interstellar and heliospheric particles inside the heliosphere both in time and in space. Understanding this modulation is necessary to correctly interpret measurements of interstellar neutral gas, energetic neutral atoms, pickup ions, and helioglow radiation measured inside the heliosphere. We report a change of heliospheric ionization rates due to the update of the SW and solar EUV data, revise the calculation of these ionization rates, and provide the most up-to-date version of the model of the Sun-Heliosphere Observation-based Ionization Rates (SHOIR). With the new results, we study the in-ecliptic variation of the SW parameters, the latitudinal structure of the SW speed and density, and the reconstruction of the photoionization rates based on the currently available data. We observe a significant change in the total ionization rates for O and Ne (up to 30%) and the latitudinal variations of the total ionization rates for H (up to 50%). The new rates are higher than previously thought. The least affected are the ionization rates for He, being about 10%. The changes are the greatest for the solar maximum period of the solar cycle 24. We discuss the consequences of the update of the ionization rates for the study of the heliosphere.

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Section: Photoionizationmentioning

confidence: 99%

Section: Photoionizationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Sun–Heliosphere Observation-based Ionization Rates Model

Sokół

McComas

Bzowski

et al. 2020

ApJ

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“…Interstellar helium penetrates the heliosheath with very little attenuation in the heliospheric interface region (less than 10%, Müller et al 2013). The main loss mechanisms inside the termination shock are photoionization (see, e.g., Bochsler et al 2014) and electron impact ionization (Rucinski & Fahr 1989). The radial profile of the electron impact ionization rate is far from trivial (see McMullin et al 2004;Bzowski et al 2013a,b).…”

Section: Appendix B: Determination Of Neutral Helium Densitymentioning

confidence: 99%

Structure of the heliosheath from HSTOF energetic neutral atoms measurements

Czechowski

Hilchenbach

Hsieh

et al. 2018

A&A

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Context. From the year 1996 until now, High energy Suprathermal Time Of Flight sensor (HSTOF) on board Solar and Heliospheric Observatory (SOHO) has been measuring the heliospheric energetic neutral atoms (ENA) flux between ±17° from the ecliptic plane. At present it is the only ENA instrument with the energy range within that of Voyager LECP energetic ion measurements. The energetic ion density and thickness of the inner heliosheath along the Voyager 1 trajectory are now known, and the ENA flux in the HSTOF energy range coming from the Voyager 1 direction may be estimated. Aims. We use HSTOF ENA data and Voyager 1 energetic ion spectrum to compare the regions of the heliosheath observed by HSTOF and Voyager 1. Methods. We compared the HSTOF ENA flux data from the forward and flank sectors of the heliosphere observed in various time periods between the years 1996 and 2010 and calculated the predicted ENA flux from the Voyager 1 direction using the Voyager 1 LECP energetic ion spectrum and including the contributions of charge exchange with both neutral H and He atoms. Results. The ratio between the HSTOF ENA flux from the ecliptic longitude sector 210−300° (the LISM apex sector) for the period 1996−1997 to the estimated ENA flux from the Voyager 1 direction is ∼1.3, but decreases to ∼0.6 for the period 1996−2005 and ∼0.3 for 1998−2006. For the flank longitude sectors (120−210° and 300−30°), the ratio also tends to decrease with time from ∼0.6 for 1996−2005 to ∼0.2 for 2008−2010. We discuss implications of these results for the energetic ion distribution in the heliosheath and the structure of the heliosphere.

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“…The EUV proxies free of modelling issues should be used to derive photoionization rates before direct measurements of EUV flux to avoid additional uncertainty or bias of the constructed model. Bzowski et al (2013a) and Bochsler et al (2014) published models of reconstruction of the photoionization rates for neutral interstellar atoms (including He) in the heliosphere based on direct measurements of the solar EUV flux and a selection of proxies most relevant for photoionization rates studies. Bochsler et al (2014) used direct measurements of the solar EUV flux from Solar Extreme Ultraviolet Experiment (SEE) onboard TIMED (Level 3A,version 11) and SOHO/CELIAS/SEM first order flux (26-34 nm), the MgII coreto-wing ratio from SOLSTICE/SORCE, and the F10.7 cm flux provided by National Oceanic and Atmospheric Administration (NOAA).…”

Section: Introductionmentioning

confidence: 99%

Photoionization rates for helium: update

Sokół,

Bzowski

2014

Preprint

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The NIS He gas has been observed at a few AU to the Sun almost from the beginning of the space age. To model its flow an estimate of the loss rates due to ionization by solar extremeultraviolet (EUV) flux is needed. The EUV irradiance has been measured directly from mid 1990-ties, but with high temporal and spectral resolution only from 2002. Beforehand only EUV proxies are available. A new method of reconstruction of the Carrington rotation averaged photoionization rates for neutral interstellar helium (NIS He) in the ecliptic at 1 AU to the Sun before 2002 is presented. We investigate the relation between the solar rotation averaged time series of the ionization rates for NIS He at 1 AU derived from TIMED measurements of EUV irradiance and the solar 10.7 cm flux (F10.7) only. We perform a weighted iterative fit of a nonlinear model to data split into sectors. The obtained formula allows to reconstruct the solar rotation averages of photoionization rates for He between ∼1947 and 2002 with an uncertainty ranging from less than 10% during solar minimum up to 20% for solar maximum.

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ERRATUM: “SOLAR PHOTOIONIZATION RATES FOR INTERSTELLAR NEUTRALS IN THE INNER HELIOSPHERE: H, He, O, AND Ne” (2014, ApJS, 210, 12)

Cited by 5 publications

References 0 publications

Sun–Heliosphere Observation-based Ionization Rates Model

Sun–Heliosphere Observation-based Ionization Rates Model

Structure of the heliosheath from HSTOF energetic neutral atoms measurements

Photoionization rates for helium: update

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