283 research outputs found
Safety and feasibility of oral immunotherapy to multiple allergens for food allergy
BACKGROUND: Thirty percent of children with food allergy are allergic to more than one food. Previous studies on oral immunotherapy (OIT) for food allergy have focused on the administration of a single allergen at the time. This study aimed at evaluating the safety of a modified OIT protocol using multiple foods at one time. METHODS: Participants underwent double-blind placebo-controlled food challenges (DBPCFC) up to a cumulative dose of 182Â mg of food protein to peanut followed by other nuts, sesame, dairy or egg. Those meeting inclusion criteria for peanut only were started on single-allergen OIT while those with additional allergies had up to 5 foods included in their OIT mix. Reactions during dose escalations and home dosing were recorded in a symptom diary. RESULTS: Forty participants met inclusion criteria on peanut DBPCFC. Of these, 15 were mono-allergic to peanut and 25 had additional food allergies. Rates of reaction per dose did not differ significantly between the two groups (median of 3.3% and 3.7% in multi and single OIT group, respectively; pâ=â.31). In both groups, most reactions were mild but two severe reactions requiring epinephrine occurred in each group. Dose escalations progressed similarly in both groups although, per protocol design, those on multiple food took longer to reach equivalent doses per food (median +4 mo.; pâ<â.0001). CONCLUSIONS: Preliminary data show oral immunotherapy using multiple food allergens simultaneously to be feasible and relatively safe when performed in a hospital setting with trained personnel. Additional, larger, randomized studies are required to continue to test safety and efficacy of multi-OIT. TRIAL REGISTRATION: Clinicaltrial.gov NCT0149017
Interstellar Pathfinder â A Mission to the Inner Edge of the Interstellar Medium
Interstellar Pathfinder (ISP), our first step into the interstellar medium, is a scientific investigation to study the outer boundary of our heliosphere and the interstellar matter that flows into it. A wind of interstellar neutral gas penetrates to within several astronomical units (AU) of the Sun, giving us a direct sample of presentâday galactic matter. ISP is a mission to this inner edge of the interstellar medium. Using highly sensitive instrumentation, ISP will determine the composition of our local interstellar environment. It will also take the first global images of the boundary region of the heliosphere at 100 to 150 AU. These measurements will allow ISP to answer fundamental questions about the origin of the solar system and the stars, about the evolution of our galaxy and of the universe, and about the characteristics of our local galactic environment and its influence on the heliosphere. © 2003 American Institute of PhysicsPeer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/87658/2/834_1.pd
Fleeting small-scale surface magnetic fields build the quiet-Sun corona
Arch-like loop structures filled with million Kelvin hot plasma form the
building blocks of the quiet-Sun corona. Both high-resolution observations and
magnetoconvection simulations show the ubiquitous presence of magnetic fields
on the solar surface on small spatial scales of 100\,km. However, the
question of how exactly these quiet-Sun coronal loops originate from the
photosphere and how the magnetic energy from the surface is channeled to heat
the overlying atmosphere is a long-standing puzzle. Here we report
high-resolution photospheric magnetic field and coronal data acquired during
the second science perihelion of Solar Orbiter that reveal a highly dynamic
magnetic landscape underlying the observed quiet-Sun corona. We found that
coronal loops often connect to surface regions that harbor fleeting weaker,
mixed-polarity magnetic field patches structured on small spatial scales, and
that coronal disturbances could emerge from these areas. We suggest that weaker
magnetic fields with fluxes as low as \,Mx and or those that evolve on
timescales less than 5\,minutes, are crucial to understand the coronal
structuring and dynamics.Comment: Accepted for publication in The Astrophysical Journal Letter
First light observations of the solar wind in the outer corona with the Metis coronagraph
In this work, we present an investigation of the wind in the solar corona that has been initiated by observations of the resonantly scattered ultraviolet emission of the coronal plasma obtained with UVCS-SOHO, designed to measure the wind outflow speed by applying Doppler dimming diagnostics. Metis on Solar Orbiter complements the UVCS spectroscopic observations that were performed during solar activity cycle 23 by simultaneously imaging the polarized visible light and the H?» I Lyman-α corona in order to obtain high spatial and temporal resolution maps of the outward velocity of the continuously expanding solar atmosphere. The Metis observations, taken on May 15, 2020, provide the first HI Lyman-α images of the extended corona and the first instantaneous map of the speed of the coronal plasma outflows during the minimum of solar activity and allow us to identify the layer where the slow wind flow is observed. The polarized visible light (580-640 nm) and the ultraviolet HI Lyα (121.6 nm) coronal emissions, obtained with the two Metis channels, were combined in order to measure the dimming of the UV emission relative to a static corona. This effect is caused by the outward motion of the coronal plasma along the direction of incidence of the chromospheric photons on the coronal neutral hydrogen. The plasma outflow velocity was then derived as a function of the measured Doppler dimming. The static corona UV emission was simulated on the basis of the plasma electron density inferred from the polarized visible light. This study leads to the identification, in the velocity maps of the solar corona, of the high-density layer about ±10° wide, centered on the extension of a quiet equatorial streamer present at the east limb - the coronal origin of the heliospheric current sheet - where the slowest wind flows at about 160 ± 18 km s-1 from 4 Râ to 6 Râ. Beyond the boundaries of the high-density layer, the wind velocity rapidly increases, marking the transition between slow and fast wind in the corona
Plasma environment of Mars as observed by simultaneous MEX-ASPERA-3 and MEX-MARSIS observations
Magnetic fields inferred by Solar Orbiter: A comparison between SO/PHI-HRT and SDO/HMI
The High Resolution Telescope (HRT) of the Polarimetric and Helioseismic
Imager on board the Solar Orbiter spacecraft (SO/PHI) and the Helioseismic and
Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) both infer
the photospheric magnetic field from polarised light images. SO/PHI is the
first magnetograph to move out of the Sun--Earth line and will provide
unprecedented access to the Sun's poles. This provides excellent opportunities
for new research wherein the magnetic field maps from both instruments are used
simultaneously. We aim to compare the magnetic field maps from these two
instruments and discuss any possible differences between them. We used data
from both instruments obtained during Solar Orbiter's inferior conjunction on 7
March 2022. The HRT data were additionally treated for geometric distortion and
degraded to the same resolution as HMI. The HMI data were re-projected to
correct for the separation between the two observatories.
SO/PHI-HRT and HMI produce remarkably similar line-of-sight magnetograms, with
a slope coefficient of , an offset below G, and a Pearson correlation
coefficient of . However, SO/PHI-HRT infers weaker line-of-sight fields
for the strongest fields. As for the vector magnetic field, SO/PHI-HRT was
compared to both the -second and -second HMI vector magnetic field:
SO/PHI-HRT has a closer alignment with the -second HMI vector. In the weak
signal regime ( G), SO/PHI-HRT measures stronger and more horizontal
fields than HMI, very likely due to the greater noise in the SO/PHI-HRT data.
In the strong field regime ( G), HRT infers lower field strengths
but with similar inclinations (a slope of ) and azimuths (a slope of
). The slope values are from the comparison with the HMI -second
vector.Comment: 10 pages, 5 figures, accepted for publication in A&A; manuscript is a
part of Astronomy & Astrophysics special issue: Solar Orbiter First Results
(Nominal Mission Phase
Wavefront error of PHI/HRT on Solar Orbiter at various heliocentric distances
We use wavefront sensing to characterise the image quality of the the High
Resolution Telescope (HRT) of the Polarimetric and Helioseismic Imager (SO/PHI)
data products during the second remote sensing window of the Solar Orbiter (SO)
nominal mission phase. Our ultimate aims are to reconstruct the HRT data by
deconvolving with the HRT point spread function (PSF) and to correct for the
effects of optical aberrations on the data. We use a pair of focused--defocused
images to compute the wavefront error and derive the PSF of HRT by means of a
phase diversity (PD) analysis. The wavefront error of HRT depends on the
orbital distance of SO to the Sun. At distances \,au, the wavefront error
is small, and stems dominantly from the inherent optical properties of HRT. At
distances \,au, the thermo-optical effect of the Heat Rejection Entrance
Window (HREW) becomes noticeable. We develop an interpolation scheme for the
wavefront error that depends on the thermal variation of the HREW with the
distance of SO to the Sun. We also introduce a new level of image
reconstruction, termed `aberration correction', which is designed to reduce the
noise caused by image deconvolution while removing the aberrations caused by
the HREW. The computed PSF via phase diversity significantly reduces the
degradation caused by the HREW in the near-perihelion HRT data. In addition,
the aberration correction increases the noise by a factor of only
compared to the factor of increase that results from the usual PD
reconstructions
Stereoscopic disambiguation of vector magnetograms: first applications to SO/PHI-HRT data
Spectropolarimetric reconstructions of the photospheric vector magnetic field
are intrinsically limited by the 180-ambiguity in the orientation of
the transverse component. So far, the removal of such an ambiguity has required
assumptions about the properties of the photospheric field, which makes
disambiguation methods model-dependent. The basic idea is that the unambiguous
line-of-sight component of the field measured from one vantage point will
generally have a non-zero projection on the ambiguous transverse component
measured by the second telescope, thereby determining the ``true'' orientation
of the transverse field. Such an idea was developed and implemented in the
Stereoscopic Disambiguation Method (SDM), which was recently tested using
numerical simulations. In this work we present a first application of the SDM
to data obtained by the High Resolution Telescope (HRT) onboard Solar Orbiter
during the March 2022 campaign, when the angle with Earth was 27 degrees. The
method is successfully applied to remove the ambiguity in the transverse
component of the vector magnetogram solely using observations (from HRT and
from the Helioseismic and Magnetic Imager), for the first time. The SDM is
proven to provide observation-only disambiguated vector magnetograms that are
spatially homogeneous and consistent. A discussion about the sources of error
that may limit the accuracy of the method, and of the strategies to remove them
in future applications, is also presented.Comment: 32 pages, 12 figures, accepted in A&A on 09/07/202
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