1,588 research outputs found
Correspondence to Elizabeth ( Bessie ) McCaw Boggs Taylor, December 11, 1901 - February 5, 1904
Correspondence to Elizabeth ( Bessie ) McCaw Boggs Taylor, December 11, 1901 - February 5, 1904.
Box 2, folder 6.https://digitalcommons.wofford.edu/littlejohnboggs/1016/thumbnail.jp
Diffuse Galactic Soft Gamma-Ray Emission
The Galactic diffuse soft gamma-ray (30-800 keV) emission has been measured
from the Galactic Center by the HIREGS balloon-borne germanium spectrometer to
determine the spectral characteristics and origin of the emission. The
resulting Galactic diffuse continuum is found to agree well with a single
power-law (plus positronium) over the entire energy range, consistent with RXTE
and COMPTEL/CGRO observations at lower and higher energies, respectively. We
find no evidence of spectral steepening below 200 keV, as has been reported in
previous observations. The spatial distribution along the Galactic ridge is
found to be nearly flat, with upper limits set on the longitudinal gradient,
and with no evidence of an edge in the observed region. The soft gamma-ray
diffuse spectrum is well modeled by inverse Compton scattering of interstellar
radiation off of cosmic-ray electrons, minimizing the need to invoke
inefficient nonthermal bremsstrahlung emission. The resulting power requirement
is well within that provided by Galactic supernovae. We speculate that the
measured spectrum provides the first direct constraints on the cosmic-ray
electron spectrum below 300 MeV.Comment: 26 pages, 7 figure, submitted to Ap
Spectra and Symmetry in Nuclear Pairing
We apply the algebraic Bethe ansatz technique to the nuclear pairing problem
with orbit dependent coupling constants and degenerate single particle energy
levels. We find the exact energies and eigenstates. We show that for a given
shell, there are degeneracies between the states corresponding to less and more
than half full shell. We also provide a technique to solve the equations of
Bethe ansatz.Comment: 15 pages of REVTEX with 2 eps figure
Wind-tunnel study of Four Allen Center, Houston
May 1982.For Century Development Corporation.CER81-82JAP-JEC-BB-DWB66.Includes bibliographical references (pages 36-37).CSU Projects 2-27840 and 2-27940
In Vivo Detection of Residues Required for Ligand-Selective Activation of the S-Locus Receptor in Arabidopsis
SummaryThe self-incompatibility response of crucifers is a barrier to fertilization in which arrest of pollen tube development is mediated by allele-specific interactions between polymorphic receptors and ligands encoded by the S-locus haplotype. Activation of stigma-expressed S-locus receptor kinase (SRK) [1] by pollen coat-localized S-locus cysteine-rich (SCR) ligand [2–5] and the resulting rejection of pollen occurs only if receptor and ligand are encoded by the same S haplotype [4, 6–8]. To identify residues within the SRK extracellular domain (eSRK) that are required for its ligand-selective activation, we assayed chimeric receptors and receptor variants containing substitutions at polymorphic sites in Arabidopsis thaliana [9, 10]. We show that only a small number of the ∼100 polymorphic residues in eSRK are required for ligand-specific activation of self-incompatibility in vivo. These essential residues occur in two noncontiguous clusters located at equivalent positions in the two variants tested. They also correspond to sites showing elevated levels of substitutions in other SRKs, suggesting that these residues could define self-incompatibility specificity in most SRKs. The results demonstrate that the majority of eSRK residues that show signals of positive selection and previously surmised to function as specificity determinants are not essential for specificity in the SRK-SCR interaction
The Giant Flare of December 27, 2004 from SGR 1806-20
The giant flare of December 27, 2004 from SGR 1806-20 represents one of the
most extraordinary events captured in over three decades of monitoring the
gamma-ray sky. One measure of the intensity of the main peak is its effect on
X- and gamma-ray instruments. RHESSI, an instrument designed to study the
brightest solar flares, was completely saturated for ~0.5 s following the start
of the main peak. A fortuitous alignment of SGR 1806-20 near the Sun at the
time of the giant flare, however, allowed RHESSI a unique view of the giant
flare event, including the precursor, the main peak decay, and the pulsed tail.
Since RHESSI was saturated during the main peak, we augment these observations
with Wind and RHESSI particle detector data in order to reconstruct the main
peak as well. Here we present detailed spectral analysis and evolution of the
giant flare. We report the novel detection of a relatively soft fast peak just
milliseconds before the main peak, whose timescale and sizescale indicate a
magnetospheric origin. We present the novel detection of emission extending up
to 17 MeV immediately following the main peak, perhaps revealing a
highly-extended corona driven by the hyper-Eddington luminosities. The spectral
evolution and pulse evolution during the tail are presented, demonstrating
significant magnetospheric twist and evolution during this phase. Blackbody
radii are derived for every stage of the flare, which show remarkable agreement
despite the range of luminosities and temperatures covered. Finally, we place
significant upper limits on afterglow emission in the hundreds of seconds
following the giant flare.Comment: 32 pages, 14 figures, submitted to Ap
Solution of the Roth-Marques-Durian Rotational Abrasion Model
We solve the rotational abrasion model of Roth, Marques and Durian
(arXiv:1009.3492), a one-dimensional quasilinear partial differential equation
resembling the inviscid Burgers equation with the unusual feature of a step
function factor as a coefficient. The complexity of the solution is primarily
in keeping track of the cases in the piecewise function that results from
certain amputation and interpolation processes, so we also extract from it a
model of an evolving planar tree graph that tracks the evolution of the coarse
features of the contour.Comment: 5 pages, 4 figure
NuSTAR Discovery of a Cyclotron Line in the Be/X-ray Binary RX J0520.5-6932 During Outburst
We present spectral and timing analysis of NuSTAR observations of RX
J0520.56932 in the 3-79 keV band collected during its outburst in January
2014. The target was observed on two epochs and we report the detection of a
cyclotron resonant scattering feature with central energies of keV and keV during the two
observations, respectively, corresponding to a magnetic field of G. The 3-79 keV luminosity of the system during the two epochs
assuming a nominal distance of 50 kpc was and
. Both values are much higher
than the critical luminosity of
above which a radiation dominated shock front may be expected. This adds a new
object to the sparse set of three systems that have a cyclotron line observed
at luminosities in excess of . A broad
( keV) Fe emission line is observed in the spectrum at a
central energy of keV in both epochs. The pulse profile
of the pulsar was observed to be highly asymmetric with a sharply rising and
slowly falling profile of the primary peak. We also observed minor variations
in the cyclotron line energy and width as a function of the rotation phase.% As
in observations of other cyclotron absorption line sources, there is a small
() phase difference between the peak of the cyclotron
energy variation and the peak of the flux variation.Comment: 9 pages, 4 figures, 6 tables. Accepted to Ap
New Constraints on the Black Hole Low/Hard State Inner Accretion Flow with NuSTAR
We report on an observation of the Galactic black hole candidate GRS 1739-278
during its 2014 outburst, obtained with NuSTAR. The source was captured at the
peak of a rising "low/hard" state, at a flux of ~0.3 Crab. A broad, skewed iron
line and disk reflection spectrum are revealed. Fits to the sensitive NuSTAR
spectra with a number of relativistically blurred disk reflection models yield
strong geometrical constraints on the disk and hard X-ray "corona". Two models
that explicitly assume a "lamppost" corona find its base to have a vertical
height above the black hole of h = 5 (+7, -2) GM/c^2 and h = 18 +/-4 GM/c^2
(90% confidence errors); models that do not assume a "lamppost" return
emissivity profiles that are broadly consistent with coronae of this size.
Given that X-ray microlensing studies of quasars and reverberation lags in
Seyferts find similarly compact coronae, observations may now signal that
compact coronae are fundamental across the black hole mass scale. All of the
models fit to GRS 1739-278 find that the accretion disk extends very close to
the black hole - the least stringent constraint is r = 5 (+3,-4) GM/c^2. Only
two of the models deliver meaningful spin constraints, but a = 0.8 +/-0.2 is
consistent with all of the fits. Overall, the data provide especially
compelling evidence of an association between compact hard X-ray coronae and
the base of relativistic radio jets in black holes.Comment: Accepted for publication in ApJ Letter
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