647 research outputs found
On the Origin of the Slow Speed Solar Wind: Helium Abundance Variations
The First Ionization Potential (FIP) effect is the by now well known
enhancement in abundance over photospheric values of Fe and other elements with
first ionization potential below about 10 eV observed in the solar corona and
slow speed solar wind. In our model, this fractionation is achieved by means of
the ponderomotive force, arising as Alfv\'en waves propagate through or reflect
from steep density gradients in the solar chromosphere. This is also the region
where low FIP elements are ionized, and high FIP elements are largely neutral
leading to the fractionation as ions interact with the waves but neutrals do
not. Helium, the element with the highest FIP and consequently the last to
remain neutral as one moves upwards can be depleted in such models. Here, we
investigate this depletion for varying loop lengths and magnetic field
strengths.
Variations in this depletion arise as the concentration of the ponderomotive
force at the top of the chromosphere varies in response to Alfv\'en wave
frequency with respect to the resonant frequency of the overlying coronal loop,
the magnetic field, and possibly also the loop length. We find that stronger
depletions of He are obtained for weaker magnetic field, at frequencies close
to or just above the loop resonance. These results may have relevance to
observed variations of the slow wind solar He abundance with wind speed, with
slower slow speed solar wind having a stronger depletion of He.Comment: 28 pages, 12 figures, accepted to Ap
The Coronal Abundance Anomalies of M Dwarfs
We analyze Chandra X-ray spectra of the M0 V+M0 V binary GJ 338. As
quantified by X-ray surface flux, these are the most inactive M dwarfs ever
observed with X-ray grating spectroscopy. We focus on measuring coronal
abundances, in particular searching for evidence of abundance anomalies related
to First Ionization Potential (FIP). In the solar corona and wind, low FIP
elements are overabundant, which is the so-called "FIP effect." For other
stars, particularly very active ones, an "inverse FIP effect" is often
observed, with low FIP elements being underabundant. For both members of the GJ
338 binary, we find evidence for a modest inverse FIP effect, consistent with
expectations from a previously reported correlation between spectral type and
FIP bias. This amounts to strong evidence that all M dwarfs should exhibit the
inverse FIP effect phenomenon, not just the active ones. We take the first step
towards modeling the inverse FIP phenomenon in M dwarfs, building on past work
that has demonstrated that MHD waves coursing through coronal loops can lead to
a ponderomotive force that fractionates elements in a manner consistent with
the FIP effect. We demonstrate that in certain circumstances this model can
also lead to an inverse FIP effect, pointing the way to more detailed modeling
of M dwarf coronal abundances in the future.Comment: to appear in The Astrophysical Journa
A new approach to analyzing solar coronal spectra and updated collisional ionization equilibrium calculations. II. Additional ionization rate coefficients
We have reanalyzed SUMER observations of a parcel of coronal gas using new
collisional ionization equilibrium (CIE) calculations. These improved CIE
fractional abundances were calculated using state-of-the-art electron-ion
recombination data for K-shell, L-shell, Na-like, and Mg-like ions of all
elements from H through Zn and, additionally, Al- through Ar-like ions of Fe.
They also incorporate the latest recommended electron impact ionization data
for all ions of H through Zn. Improved CIE calculations based on these
recombination and ionization data are presented here. We have also developed a
new systematic method for determining the average emission measure () and
electron temperature () of an isothermal plasma. With our new CIE data and
our new approach for determining average and , we have reanalyzed
SUMER observations of the solar corona. We have compared our results with those
of previous studies and found some significant differences for the derived
and . We have also calculated the enhancement of coronal elemental
abundances compared to their photospheric abundances, using the SUMER
observations themselves to determine the abundance enhancement factor for each
of the emitting elements. Our observationally derived first ionization
potential (FIP) factors are in reasonable agreement with the theoretical model
of Laming (2008).Comment: 147 pages (102 of which are online only tables and figures).
Submitted to ApJ. Version 2 is updated addressing the referee's repor
Ion Charge States in Halo CMEs: What can we Learn about the Explosion?
We describe a new modeling approach to develop a more quantitative
understanding of the charge state distributions of the ions of various elements
detected in situ during halo Coronal Mass Ejection (CME) events by the Advanced
Composition Explorer (ACE) satellite. Using a model CME hydrodynamic evolution
based on observations of CMEs propagating in the plane of the sky and on
theoretical models, we integrate time dependent equations for the ionization
balance of various elements to compare with ACE data. We find that plasma in
the CME ``core'' typically requires further heating following filament
eruption, with thermal energy input similar to the kinetic energy input. This
extra heating is presumably the result of post eruptive reconnection. Plasma
corresponding to the CME ``cavity'' is usually not further ionized, since
whether heated or not, the low density gives freeze-in close the the Sun. The
current analysis is limited by ambiguities in the underlying model CME
evolution. Such methods are likely to reach their full potential when applied
to data to be acquired by STEREO when at optimum separation. CME evolution
observed with one spacecraft may be used to interpret CME charge states
detected by the other.Comment: 20 pages, accepted by Ap
Spatially Dependent Heating and Ionization in an ICME Observed by Both ACE and Ulysses
The 2005 January 21 interplanetary coronal mass ejection (ICME) observed by multiple spacecraft at L1 was also observed from January 21-February 4 at Ulysses (5.3ĂÂŹĂąâŹÂ AU). Previous studies of this ICME have found evidence suggesting that the flanks of a magnetic cloud like structure associated with this ICME were observed at L1 while a more central cut through the associated magnetic cloud was observed at Ulysses . This event allows us to study spatial variation across the ICME and relate it to the eruption at the Sun. In order to examine the spatial dependence of the heating in this ICME, we present an analysis and comparison of the heavy ion composition observed during the passage of the ICME at L1 and at Ulysses . Using SWICS, we compare the heavy ion composition across the two different observation cuts through the ICME and compare it with predictions for heating during the eruption based on models of the time-dependent ionization balance throughout the event.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/98582/1/0004-637X_760_2_105.pd
Demonstration of early functional compromise of bone marrow derived hematopoietic progenitor cells during bovine neonatal pancytopenia through in vitro culture of bone marrow biopsies
<p>Abstract</p> <p>Background</p> <p>Bovine neonatal pancytopenia (BNP) is a syndrome characterised by thrombocytopenia associated with marked bone marrow destruction in calves, widely reported since 2007 in several European countries and since 2011 in New Zealand. The disease is epidemiologically associated with the use of an inactivated bovine virus diarrhoea (BVD) vaccine and is currently considered to be caused by absorption of colostral antibody produced by some vaccinated cows (âBNP damsâ). Alloantibodies capable of binding to the leukocyte surface have been detected in BNP dams and antibodies recognising bovine MHC class I and ÎČ-2-microglobulin have been detected in vaccinated cattle. In this study, calves were challenged with pooled colostrum collected from BNP dams or from non-BNP dams and their bone marrow hematopoietic progenitor cells (HPC) cultured <it>in vitro</it> from sternal biopsies taken at 24 hours and 6 days post-challenge.</p> <p>Results</p> <p>Clonogenic assay demonstrated that CFU-GEMM (colony forming unit-granulocyte/erythroid/macrophage/megakaryocyte; pluripotential progenitor cell) colony development was compromised from HPCs harvested as early as 24 hour post-challenge. By 6 days post challenge, HPCs harvested from challenged calves failed to develop CFU-E (erythroid) colonies and the development of both CFU-GEMM and CFU-GM (granulocyte/macrophage) was markedly reduced.</p> <p>Conclusion</p> <p>This study suggests that the bone marrow pathology and clinical signs associated with BNP are related to an insult which compromises the pluripotential progenitor cell within the first 24 hours of life but that this does not initially include all cell types.</p
Fe XVII X-ray Line Ratios for Accurate Astrophysical Plasma Diagnostics
New laboratory measurements using an Electron Beam Ion Trap (EBIT) and an
x-ray microcalorimeter are presented for the n=3 to n=2 Fe XVII emission lines
in the 15 {\AA} to 17 {\AA} range, along with new theoretical predictions for a
variety of electron energy distributions. This work improves upon our earlier
work on these lines by providing measurements at more electron impact energies
(seven values from 846 to 1185 eV), performing an in situ determination of the
x-ray window transmission, taking steps to minimize the ion impurity
concentrations, correcting the electron energies for space charge shifts, and
estimating the residual electron energy uncertainties. The results for the
3C/3D and 3s/3C line ratios are generally in agreement with the closest theory
to within 10%, and in agreement with previous measurements from an independent
group to within 20%. Better consistency between the two experimental groups is
obtained at the lowest electron energies by using theory to interpolate, taking
into account the significantly different electron energy distributions.
Evidence for resonance collision effects in the spectra is discussed.
Renormalized values for the absolute cross sections of the 3C and 3D lines are
obtained by combining previously published results, and shown to be in
agreement with the predictions of converged R-matrix theory. This work
establishes consistency between results from independent laboratories and
improves the reliability of these lines for astrophysical diagnostics. Factors
that should be taken into account for accurate diagnostics are discussed,
including electron energy distribution, polarization, absorption/scattering,
and line blends.Comment: 29 pages, including 7 figure
A frequency weighting for the evaluation of steering wheel rotational vibration
The human perception of rotational hand-arm vibration has been investigated by means of a test rig consisting of a rigid frame, an electrodynamic shaker unit, a rigid steering wheel, a shaft assembly, bearings and an automobile seat. Fifteen subjects were tested while seated in a driving posture. Four equal sensation tests and one annoyance threshold test were performed using sinusoidal excitation at 18 frequencies in the range from 3 to 315 Hz. In order to guarantee the generality of the equal sensation data the four tests were defined to permit checks of the possible influence of three factors: reference signal amplitude, psychophysical test procedure and temporary threshold shift (TTSv) caused by the test exposure. All equal sens ation tests used a reference sinusoid of 63 Hz at either 1.0 or 1.5 m/s2 r.m.s. in amplitude. The four equal sensation curves were similar in shape and suggested a decrease in human sensitivity to hand-arm rotational vibration with increasing frequency. The slopes of the equal sensation curves changed at transition points of approximately 6.3 and 63 Hz. A frequency weighting, called Ws, was developed for the purpose of evaluating steering wheel rotational vibration. The proposed Ws has a slope of 0 dB per octave over the frequency range from 3 to 6.3 Hz, a slope of -6 dB per octave from 6.3 to 50 Hz, a slope of 0 dB per octave from 50 to 160 Hz and a slope of -10 dB per octave from 160 to 315 Hz. Ws provides a possible alternative to the existing Wh frequency weighting defined in International Standards Organisation 5349-1 (2001) and British Standards Institution 6842 (1987)
A Unified Picture of the FIP and Inverse FIP Effects
We discuss models for coronal abundance anomalies observed in the coronae of
the sun and other late-type stars following a scenario first introduced by
Schwadron, Fisk & Zurbuchen of the interaction of waves at loop footpoints with
the partially neutral gas. Instead of considering wave heating of ions in this
location, we explore the effects on the upper chromospheric plasma of the wave
ponderomotive forces. These can arise as upward propagating waves from the
chromosphere transmit or reflect upon reaching the chromosphere-corona
boundary, and are in large part determined by the properties of the coronal
loop above. Our scenario has the advantage that for realistic wave energy
densities, both positive and negative changes in the abundance of ionized
species compared to neutrals can result, allowing both FIP and Inverse FIP
effects to come out of the model. We discuss how variations in model parameters
can account for essentially all of the abundance anomalies observed in solar
spectra. Expected variations with stellar spectral type are also qualitatively
consistent with observations of the FIP effect in stellar coronae.Comment: 25 pages, 4 figures, submitted to Ap
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