608 research outputs found
Connecting physical resonant amplitudes and lattice QCD
We present a determination of the isovector, -wave scattering
phase shift obtained by extrapolating recent lattice QCD results from the
Hadron Spectrum Collaboration using MeV. The finite volume spectra
are described using extensions of L\"uscher's method to determine the infinite
volume Unitarized Chiral Perturbation Theory scattering amplitude. We exploit
the pion mass dependence of this effective theory to obtain the scattering
amplitude at MeV. The scattering phase shift is found to be in
good agreement with experiment up to center of mass energies of 1.2 GeV. The
analytic continuation of the scattering amplitude to the complex plane yields a
-resonance pole at .
The techniques presented illustrate a possible pathway towards connecting
lattice QCD observables of few-body, strongly interacting systems to
experimentally accessible quantities.Comment: 8 pages, 6 figures, equivalent to published version, added two
appendices and a figur
Two-Nucleon Systems in a Finite Volume: (II) 3S1-3D1 Coupled Channels and the Deuteron
The energy spectra of two nucleons in a cubic volume provide access to the
two phase shifts and one mixing angle that define the S-matrix in the 3S1-3D1
coupled channels containing the deuteron. With the aid of recently derived
energy quantization conditions for such systems, and the known scattering
parameters, these spectra are predicted for a range of volumes. It is found
that extractions of the infinite-volume deuteron binding energy and leading
scattering parameters, including the S-D mixing angle at the deuteron pole, are
possible from Lattice QCD calculations of two-nucleon systems with boosts of
|P| <= 2pi sqrt{3}/L in volumes with 10 fm <~ L <~ 14 fm. The viability of
extracting the asymptotic D/S ratio of the deuteron wavefunction from Lattice
QCD calculations is discussed.Comment: 31 pages, 17 figure
Scattering processes and resonances from lattice QCD
The vast majority of hadrons observed in nature are not stable under the
strong interaction, rather they are resonances whose existence is deduced from
enhancements in the energy dependence of scattering amplitudes. The study of
hadron resonances offers a window into the workings of quantum chromodynamics
(QCD) in the low-energy non-perturbative region, and in addition, many probes
of the limits of the electroweak sector of the Standard Model consider
processes which feature hadron resonances. From a theoretical standpoint, this
is a challenging field: the same dynamics that binds quarks and gluons into
hadron resonances also controls their decay into lighter hadrons, so a complete
approach to QCD is required. Presently, lattice QCD is the only available tool
that provides the required non-perturbative evaluation of hadron observables.
In this article, we review progress in the study of few-hadron reactions in
which resonances and bound-states appear using lattice QCD techniques. We
describe the leading approach which takes advantage of the periodic finite
spatial volume used in lattice QCD calculations to extract scattering
amplitudes from the discrete spectrum of QCD eigenstates in a box. We explain
how from explicit lattice QCD calculations, one can rigorously garner
information about a variety of resonance properties, including their masses,
widths, decay couplings, and form factors. The challenges which currently limit
the field are discussed along with the steps being taken to resolve them
Isoscalar scattering and the mesons from QCD
We present the first lattice QCD study of coupled isoscalar
- and -wave scattering extracted from
discrete finite-volume spectra computed on lattices which have a value of the
quark mass corresponding to MeV. In the sector we find
analogues of the experimental and states, where the
appears as a stable bound-state below threshold, and, similar
to what is seen in experiment, the manifests itself as a dip in the
cross section in the vicinity of the threshold. For
we find two states resembling the and ,
observed as narrow peaks, with the lighter state dominantly decaying to
and the heavier state to . The presence of all these
states is determined rigorously by finding the pole singularity content of
scattering amplitudes, and their couplings to decay channels are established
using the residues of the poles
Two-Baryon Systems with Twisted Boundary Conditions
We explore the use of twisted boundary conditions in extracting the nucleon
mass and the binding energy of two-baryon systems, such as the deuteron, from
Lattice QCD calculations. Averaging the results of calculations performed with
periodic and anti-periodic boundary conditions imposed upon the light-quark
fields, or other pair-wise averages, improves the volume dependence of the
deuteron binding energy from ~exp(-kappa*L)/L to ~exp(-sqrt(2)kappa*L)/L.
However, a twist angle of pi/2 in each of the spatial directions improves the
volume dependence from ~exp(-kappa*L)/L to ~exp(-2kappa*L)/L. Twist averaging
the binding energy with a random sampling of twist angles improves the volume
dependence from ~exp^(-kappa*L)/L to ~exp(-2kappa*L)/L, but with a standard
deviation of ~exp(-kappa*L)/L, introducing a signal-to-noise issue in modest
lattice volumes. Using the experimentally determined phase shifts and mixing
angles, we determine the expected energies of the deuteron states over a range
of cubic lattice volumes for a selection of twisted boundary conditions.Comment: 20 pages, 3 figure
Disks around Brown Dwarfs in the Sigma Orionis Cluster
We have performed a census of disks around brown dwarfs in the Sigma Ori
cluster using all available images from IRAC onboard the Spitzer Space
Telescope. To search for new low-mass cluster members with disks, we have
measured photometry for all sources in the Spitzer images and have identified
the ones that have red colors that are indicative of disks. We present 5
promising candidates, which may consist of 2 brown dwarfs, 2 stars with edge-on
disks, and a low-mass protostar if they are bona fide members. Spectroscopy is
needed to verify the nature of these sources. We have also used the Spitzer
data to determine which of the previously known probable members of Sigma Ori
are likely to have disks. By doing so, we measure disk fractions of ~40% and
~60% for low-mass stars and brown dwarfs, respectively. These results are
similar to previous estimates of disk fractions in IC 348 and Cha I, which have
roughly the same median ages as Sigma Ori (3 Myr). Finally, we note that our
photometric measurements and the sources that we identify as having disks
differ significantly from those of other recent studies that analyzed the same
Spitzer images. For instance, previous work has suggested that the T dwarf S
Ori 70 is redder than typical field dwarfs, which has been cited as possible
evidence of youth and cluster membership. However, we find that this object is
only slightly redder than the reddest field dwarfs in [3.6]-[4.5] (1.56+/-0.07
vs. 0.93-1.46). We measure a larger excess in [3.6]-[5.8] (1.75+/-0.21 vs.
0.87-1.19), but the flux at 5.8um may be overestimated because of the low
signal-to-noise ratio of the detection. Thus, the Spitzer data do not offer
strong evidence of youth and membership for this object, which is the faintest
and coolest candidate member of Sigma Ori that has been identified to date.Comment: Astrophysical Journal, in pres
Spitzer observations of the Orion OB1 association: disk census in the low mass stars
We present new Spitzer Space Telescope observations of two fields in the
Orion OB1 association. We report here IRAC/MIPS observations for 115 confirmed
members and 41 photometric candidates of the ~10 Myr 25 Orionis aggregate in
the OB1a subassociation, and 106 confirmed members and 65 photometric
candidates of the 5 Myr region located in the OB1b subassociation. The 25
Orionis aggregate shows a disk frequency of 6% while the field in the OB1b
subassociation shows a disk frequency of 13%. Combining IRAC, MIPS and 2MASS
photometry we place stars bearing disks in several classes: stars with
optically thick disks (class II systems), stars with an inner transitional
disks (transitional disk candidates) and stars with "evolved disks"; the last
exhibit smaller IRAC/MIPS excesses than class II systems. In all, we identify 1
transitional disk candidate in the 25 Orionis aggregate and 3 in the OB1b
field; this represents ~10% of the disk bearing stars, indicating that the
transitional disk phase can be relatively fast. We find that the frequency of
disks is a function of the stellar mass, suggesting a maximum around stars with
spectral type M0. Comparing the infrared excess in the IRAC bands among several
stellar groups we find that inner disk emission decays with stellar age,
showing a correlation with the respective disk frequencies. The disk emission
at the IRAC and MIPS bands in several stellar groups indicates that disk
dissipation takes place faster in the inner region of the disks. Comparison
with models of irradiated accretion disks, computed with several degrees of
settling, suggests that the decrease in the overall accretion rate observed in
young stellar groups is not sufficient to explain the weak disk emission
observed in the IRAC bands for disk bearing stars with ages 5 Myr or older.Comment: Accepted in the Astrophysical Journa
Photometric Accretion Signatures Near the Substellar Boundary
Multi-epoch imaging of the Orion equatorial region by the Sloan Digital Sky
Survey has revealed that significant variability in the blue continuum persists
into the late-M spectral types, indicating that magnetospheric accretion
processes occur below the substellar boundary in the Orion OB1 association. We
investigate the strength of the accretion-related continuum veiling by
comparing the reddening-invariant colors of the most highly variable stars
against those of main sequence M dwarfs and evolutionary models. A gradual
decrease in the g band veiling is seen for the cooler and less massive members,
as expected for a declining accretion rate with decreasing mass. We also see
evidence that the temperature of the accretion shock decreases in the very low
mass regime, reflecting a reduction in the energy flux carried by the accretion
columns. We find that the near-IR excess attributed to circumstellar disk
thermal emission drops rapidly for spectral types later than M4. This is likely
due to the decrease in color contrast between the disk and the cooler stellar
photosphere. Since accretion, which requires a substantial stellar magnetic
field and the presence of a circumstellar disk, is inferred for masses down to
0.05 Msol we surmise that brown dwarfs and low mass stars share a common mode
of formation.Comment: 37 pages, 14 figures, accepted by A
Spectroscopy of Brown Dwarf Candidates in the rho Ophiuchi Molecular Core
We present an analysis of low resolution infrared spectra for 20 brown dwarf
candidates in the core of the Ophiuchi molecular cloud. Fifteen of the
sources display absorption-line spectra characteristic of late-type stars. By
comparing the depths of water vapor absorption bands in our candidate objects
with a grid of M dwarf standards, we derive spectral types which are
independent of reddening. Optical spectroscopy of one brown dwarf candidate
confirms the spectral type derived from the water bands. Combining their
spectral types with published near-infrared photometry, effective temperatures
and bolometric stellar luminosities are derived enabling us to place our sample
on the Hertzsprung-Russell diagram. We compare the positions of the brown dwarf
candidates in this diagram with two sets of theoretical models in order to
estimate their masses and ages. Considering uncertainties in placing the
candidates in the H-R diagram, six objects consistently lie in the brown dwarf
regime and another five objects lie in the transition region between stellar
and substellar objects. The ages inferred for the sample are consistent with
those derived for higher mass association members. Three of the newly
identified brown dwarfs display infrared excesses at =2.2 m
suggesting that young brown dwarfs can have active accretion disks. Comparing
our mass estimates of the brown dwarf candidates with those derived from
photometric data alone suggests that spectroscopy is an essential component of
investigations of the mass functions of young clusters.Comment: Astronomical Journal, in press: 25 pages, latex, 5 tables and 6
figures (separate
Spitzer Space Telescope study of disks in the young Orionis cluster
We report new Spitzer Space Telescope observations from the IRAC and MIPS
instruments of the young (~ 3 Myr) sigma Orionis cluster. We identify 336 stars
as members of the cluster using optical and near-infrared color magnitude
diagrams. Using the spectral energy distribution (SED) slopes in the IRAC
spectral range, we place objects in several classes: non-excess stars, stars
with optically thick disks(like classical T Tauri stars), class I
(protostellar) candidates, and stars with ``evolved disks''; the last exhibit
smaller IRAC excesses than optically thick disk systems. In general, this
classification agrees with the location expected in IRAC-MIPS color-color
diagrams for these objects. We find that the evolved disk systems are mostly a
combination of objects with optically thick but non-flared disks, suggesting
grain growth and/or settling, and transition disks, systems in which the inner
disk is partially or fully cleared of small dust. In all, we identify 7
transition disk candidates and 3 possible debris disk systems. As in other
young stellar populations, the fraction of disks depends on the stellar mass,
ranging from ~10% for stars in the Herbig Ae/Be mass range (>2 msun) to ~35% in
the T Tauri mass range (1-0.1 msun). We find that the disk fraction does not
decrease significantly toward the brown dwarf candidates (<0.1 msun). The IRAC
infrared excesses found in stellar clusters and associations with and without
central high mass stars are similar, suggesting that external photoevaporation
is not very important in many clusters. Finally, we find no correlation between
the X-ray luminosity and the disk infrared excess, suggesting that the X-rays
are not strongly affected by disk accretion.Comment: 44pages, 17 figures. Sent to Ap
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