Energetic neutral atoms from the Earth's subsolar magnetopause

Fuselier, S. A.; Funsten, H. O.; Heirtzler, D.; Janzen, P. H.; Kucharek, H.; McComas, D. J.; Möbius, E.; Moore, T. E.; Petrinec, S. M.; Reisenfeld, D. B.; Schwadron, N. A.; Trattner, K. J.; Würz, Peter

doi:10.1029/2010gl044140

Cited by 74 publications

(120 citation statements)

References 24 publications

(26 reference statements)

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“…The two profiles from Bailey and Gruntman (2011) and Zoennchen et al (2011) are reasonably close as well. The neutral H-density from our seasonal-averaged model at the subsolar point at 10 R E is with 18 cm −3 close to the value of 4-11 cm −1 found with a different method (using IBEX-ENA-and Cluster3-proton data) by Fuselier et al (2010). Fig.…”

Section: Seasonal Effects Compared To Hodges (1994)mentioning

confidence: 96%

Exospheric hydrogen density distributions for equinox and summer solstice observed with TWINS1/2 during solar minimum

2013

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The Lyman-α Detectors (LAD) on board the two TWINS 1/2-satellites allow for the simultaneous stereo imaging of the resonant emission glow of the H-geocorona from very different orbital positions. Terrestrial exospheric atomic hydrogen (H) resonantly scatters solar Lyman-α (121.567 nm) radiation. During the past solar minimum, relevant solar parameters that influence these emissions were quite stable. Here, we use simultaneous LAD1/2-observations from TWINS1 and TWINS2 between June 2008 and June 2010 to study seasonal variations in the H-geocorona. Data are combined to produce two datasets containing (summer) solstice and (combined spring and fall) equinox emissions. In the range from 3 to 10 Earth radii (R_E), a three-dimensional (3-D) mathematical model is used that allows for density asymmetries in longitude and latitude. At lower geocentric distances (< 3 R_E), a best fitting r-dependent (Chamberlain, 1963)-like model is adapted to enable extrapolation of our information to lower heights. We find that dawn and dusk H-geocoronal densities differ by up to a factor of 1.3 with higher densities on the dawn side. Also, noon densities are greater by up to a factor of 2 compared to the dawn and dusk densities. The density profiles are aligned well with the Earth–Sun line and there are clear density depletions over both poles that show additional seasonal effects. These solstice and equinox empirical fits can be used to determine H-geocoronal densities for any day of the year for solar minimum conditions

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Section: Seasonal Effects Compared To Hodges (1994)mentioning

confidence: 96%

Exospheric hydrogen density distributions for equinox and summer solstice observed with TWINS1/2 during solar minimum

2013

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“…The absolute flux uncertainty of the low-energy beam that was used is poorly known, and its dependence on energy is likely more complex than assumed here. Therefore, conservative values are used here, consistent with those used previously (Fuselier et al 2010(Fuselier et al , 2012. There is an additional, systematic error associated with the frame transformation because the IBEX sensor energy channels are very wide (FWHM, ΔE/E ∼ 0.7).…”

Section: Observations From the Lines Of Sight To The V1 And Downstreamentioning

confidence: 98%

Low Energy Neutral Atoms From the Heliosheath

Fuselier

Allegrini

Bzowski

et al. 2014

ApJ

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In the heliosheath beyond the termination shock, low energy (<0.5 keV) neutral atoms are created by charge exchange with interstellar neutrals. Detecting these neutrals from Earth's orbit is difficult because their flux is reduced substantially by ionization losses as they propagate from about 100 to 1 AU and because there are a variety of other signals and backgrounds that compete with this weak signal. Observations from IBEX-Lo and -Hi from two opposing vantage points in Earth's orbit established a lower energy limit of about 0.1 keV on measurements of energetic neutral atoms (ENAs) from the heliosphere and the form of the energy spectrum from about 0.1 to 6 keV in two directions in the sky. Below 0.1 keV, the detailed ENA spectrum is not known, and IBEX provides only upper limits on the fluxes. However, using some assumptions and taking constraints on the spectrum into account, we find indications that the spectrum turns over at an energy between 0.1 and 0.2 keV.

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“…The resulting energetic neutral is not bound by the local magnetic field and will travel away from the location of the interaction. Measurements of charge exchange from magnetosheath plasma have been made in the subsolar magnetosheath Fuselier et al, 2010] as well as cusps [Taguchi et al, 2005;Petrinec et al, 2011]. These imaging techniques are complementary; however, one difference between them is the time-of-flight effect.…”

Section: Introductionmentioning

confidence: 99%

Wide field‐of‐view soft X‐ray imaging for solar wind‐magnetosphere interactions

et al. 2016

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Soft X‐ray imagers can be used to study the mesoscale and macroscale density structures that occur whenever and wherever the solar wind encounters neutral atoms at comets, the Moon, and both magnetized and unmagnetized planets. Charge exchange between high charge state solar wind ions and exospheric neutrals results in the isotropic emission of soft X‐ray photons with energies from 0.1 to 2.0 keV. At Earth, this process occurs primarily within the magnetosheath and cusps. Through providing a global view, wide field‐of‐view imaging can determine the significance of the various proposed solar wind‐magnetosphere interaction mechanisms by evaluating their global extent and occurrence patterns. A summary of wide field‐of‐view (several to tens of degrees) soft X‐ray imaging is provided including slumped micropore microchannel reflectors, simulated images, and recent flight results.

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Energetic neutral atoms from the Earth's subsolar magnetopause

Cited by 74 publications

References 24 publications

Exospheric hydrogen density distributions for equinox and summer solstice observed with TWINS1/2 during solar minimum

Exospheric hydrogen density distributions for equinox and summer solstice observed with TWINS1/2 during solar minimum

Low Energy Neutral Atoms From the Heliosheath

Wide field‐of‐view soft X‐ray imaging for solar wind‐magnetosphere interactions

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