UPDATED ANALYSIS OF THE UPWIND INTERPLANETARY HYDROGEN VELOCITY AS OBSERVED BY THE<i>HUBBLE SPACE TELESCOPE</i>DURING SOLAR CYCLE 23

Vincent, F.; Ben‐Jaffel, Lotfi; Harris, Walter M.

doi:10.1088/0004-637x/738/2/135

Cited by 9 publications

(18 citation statements)

References 39 publications

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“…For the 2001 observations, this present work yielded a value of 22.6 ± 0.5 km s −1 , consistent with a previous analysis that was fitting all spectral features (instead of removing the signal from the occulting bars) and gave a result of 22.4 ± 0.4 km s −1 (Vincent et al 2011). The similarity between the results from different methods on the same data set validates the robustness of the method that has been used for this data analysis.…”

Section: Discussionsupporting

confidence: 90%

“…Hence we constructed an ad hoc LSF from the convolution of a previously measured LSF from a supported mode with a square filter having the same width as the slit used for the observations (see the second paragraph of Section 2.3 in Vincent et al 2011).…”

Section: Discussionmentioning

confidence: 99%

“…We fitted separately the blue side and the red side of the geocorona line profile, using STIS observations made in 2000 and 2001, respectively, as the corresponding side was not overlapped by the IPH or any O i contamination because of the geometry of the observations (see the third paragraph of Section 2.3 in Vincent et al 2011). Each side was fitted by the convolution of the ad hoc LSF with a sum of two Voigt functions that fit the core and the wing of that side.…”

Section: Discussionmentioning

confidence: 99%

“…Radiative transfer computations showed that any observed lineshift represents approximately the bulk velocity of the IPH atoms, projected and integrated along the LOS from the Earth (Quémerais 2000). We computed the 1σ errors as the quadratic sum of the instrumental and statistical uncertainties (for more details, see the fifth paragraph of Section 2.3 in Vincent et al 2011).…”

Section: Discussionmentioning

confidence: 99%

“…Using a long slit allows the collection of more photons and an increase of the signal to noise from an extended source such as IPH, but this configuration results in the superposition of different orders of the echelle spectrum, especially the contamination of the Lyα line (121.6 nm) by the 130.4 nm triplet line of geocoronal oxygen (Vincent et al 2011).…”

Section: Description Of the Instrument And The Signalmentioning

confidence: 99%

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Observations of the Interplanetary Hydrogen During Solar Cycles 23 and 24. What Can We Deduce About the Local Interstellar Medium?

Vincent

Katushkina

Ben‐Jaffel

et al. 2014

ApJ

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Section: Discussionsupporting

confidence: 90%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Description Of the Instrument And The Signalmentioning

confidence: 99%

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Observations of the Interplanetary Hydrogen During Solar Cycles 23 and 24. What Can We Deduce About the Local Interstellar Medium?

Vincent

Katushkina

Ben‐Jaffel

et al. 2014

ApJ

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IUVS echelle‐mode observations of interplanetary hydrogen: Standard for calibration and reference for cavity variations between Earth and Mars during MAVEN cruise

et al. 2017

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The high‐resolution echelle mode of the Imaging Ultraviolet Spectrograph (IUVS) instrument on the Mars Atmosphere and Volatile Evolution mission has been designed to measure D and H Lyman α emissions from the Martian atmosphere to obtain key information about the physical processes by which water escapes into space. Toward this goal, the absolute calibration of the instrument is critical for determining the D and H densities, the D/H ratio, and the escape flux of water. The instrument made observations of interplanetary hydrogen (IPH) along multiple look directions and conducted several postlaunch calibration campaigns during cruise as well as during orbit around Mars. The calibration efforts monitored instrument degradation and produced a consistent calibration factor at the hydrogen Lyman α wavelength (121.567 nm). The instrument was calibrated with the diffuse emission of interplanetary hydrogen (IPH) as a standard candle using measurements and model results from the Solar Wind Anisotropies (SWAN) instrument. Validation of the calibrated instrument was made by (1) comparisons to simultaneous observations of the IPH made with the lower resolution FUV mode of the IUVS instrument that were independently calibrated by using standard stars and by (2) comparisons to same‐day observations of Mars at hydrogen Lyman α made with the Hubble Space Telescope that were calculated with a radiative transfer model. Adopted FUV mode values and Hubble Space Telescope‐based model results agreed with the echelle SWAN calibrated values to within 6% and 4%, respectively. The calibrated IUVS instrument can be used to interpret emissions of atmospheric species at Mars for insights into water evolution at the planet, as well as observed IPH measurements made during cruise for further insights into dynamics of the inner heliosphere.

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Backscattered Solar Lyman-$\alpha $ Emission as a Tool for the Heliospheric Boundary Exploration

et al. 2022

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This review summarizes our current understanding of the outer heliosphere and local interstellar medium (LISM) inferred from observations and modeling of interplanetary Lyman-α emission. The emission is produced by solar Lyman-α photons (121.567 nm) backscattered by interstellar H atoms inflowing to the heliosphere from the LISM. Studies of Lyman-α radiation determined the parameters of interstellar hydrogen within a few astronomical units from the Sun. The interstellar hydrogen atoms appeared to be decelerated, heated, and shifted compared to the helium atoms. The detected deceleration and heating proved the existence of secondary hydrogen atoms created near the heliopause. This finding supports the discovery of a Hydrogen Wall beyond the heliosphere consisting of heated hydrogen observed in HST/GHRS Lyman-α absorption spectra toward nearby stars. The shift of the interstellar hydrogen bulk velocity was the first observational evidence of the global heliosphere asymme-

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UPDATED ANALYSIS OF THE UPWIND INTERPLANETARY HYDROGEN VELOCITY AS OBSERVED BY THEHUBBLE SPACE TELESCOPEDURING SOLAR CYCLE 23

Cited by 9 publications

References 39 publications

Observations of the Interplanetary Hydrogen During Solar Cycles 23 and 24. What Can We Deduce About the Local Interstellar Medium?

Observations of the Interplanetary Hydrogen During Solar Cycles 23 and 24. What Can We Deduce About the Local Interstellar Medium?

IUVS echelle‐mode observations of interplanetary hydrogen: Standard for calibration and reference for cavity variations between Earth and Mars during MAVEN cruise

Backscattered Solar Lyman-$\alpha $ Emission as a Tool for the Heliospheric Boundary Exploration

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