436 research outputs found
He~I Emission in the Orion Nebula and Implications for Primordial Helium Abundance
We apply a recently developed theoretical model of helium emission to
observations of both the Orion Nebula and a sample of extragalactic H II
regions. In the Orion analysis, we eliminate some weak and blended lines and
compare theory and observation for our reduced line list. With our best
theoretical model we find an average difference between theoretical and
observed intensities . We argue that
both the red and blue ends of the spectrum may have been inadequately corrected
for reddening. For the 22 highest quality lines, with , our best model predicts observations to an
average of 3.8%. We also perform an analysis of the reported observational
errors and conclude they have been underestimated. In the extragalactic
analysis, we demonstrate the likelihood of a large systematic error in the
reported data and discuss possible causes. This systematic error is at least as
large as the errors associated with nearly all attempts to calculate the
primordial helium abundance from such observations. Our Orion analysis suggests
that the problem does not lie in the theoretical models. We demonstrate a
correlation between equivalent width and apparent helium abundance of lines
from extragalactic sources that is most likely due to underlying stellar
absorption. Finally, we present fits to collisionless case-B He I emissivities
as well as the relative contributions due to collisional excitations out of the
metastable term.Comment: accepted for publication in Ap
\u3cem\u3eJ\u3c/em\u3e-Resolved He I Emission Predictions in the Low-Density Limit
Determinations of the primordial helium abundance are used in precision cosmological tests. These require highly accurate He I recombination rate coefficients. Here we reconsider the formation of He I recombination lines in the low-density limit. This is the simplest case, and it forms the basis for the more complex situation in which collisions are important. The formation of a recombination line is a two-step process, beginning with the capture of a continuum electron into a bound state and followed by radiative cascade to ground. The rate coefficient for capture from the continuum is obtained from photoionization cross sections and detailed balancing, while radiative transition probabilities determine the cascades. We have made every effort to use today\u27s best atomic data. Radiative decay rates are from Drake\u27s variational calculations, which include QED, fine structure, and singlet-triplet mixing. Certain high-L fine-structure levels do not have a singlet-triplet distinction, and the singlets and triplets are free to mix in dipole-allowed radiative decays. We use quantum-defect or hydrogenic approximations to include levels higher than those treated in the variational calculations. Photoionization cross sections come from R-matrix calculations when possible. We use Seaton\u27s method to extrapolate along sequences of transition probabilities to obtain threshold photoionization cross sections for some levels. For higher n we use scaled hydrogenic theory or an extension of quantum-defect theory. We create two independent numerical implementations to ensure that the complex bookkeeping is correct. The two codes use different (reasonable) approximations to span the gap between lower levels, having accurate data, and high levels, where scaled hydrogenic theory is appropriate. We also use different (reasonable) methods to account for recombinations above the highest levels individually considered. We compare these independent predictions to estimate the uncertainties introduced by the various approximations. Singlet-triplet mixing has little effect on the observed spectrum. While intensities of lines within multiplets change, the entire multiplet, the quantity normally observed, does not. The lack of high-precision photoionization cross sections at intermediate n and low L introduces ~0.5% uncertainties in intensities of some lines. The high-n unmodeled levels introduce ~1% uncertainties for “yrast\u27\u27 lines, defined as those having L=n-1 upper levels. This last uncertainty will not be present in actual nebulae, since such high levels are held in statistical equilibrium by collisional processes. We identify those lines that are least affected by uncertainties in the atomic physics and so should be used in precision helium abundance determinations
CTMC calculations of electron capture and ionization in collisions of multiply charged ions with elliptical Rydberg atoms
We have performed classical trajectory Monte Carlo (CTMC) studies of electron
capture and ionization in multiply charged (Q=8) ion-Rydberg atom collisions at
intermediate impact velocities. Impact parallel to the minor and to the major
axis, respectively, of the initial Kepler electron ellipse has been
investigated. The important role of the initial electron momentum distribution
found for singly charged ion impact is strongly disminished for higher
projectile charge, while the initial spatial distribution remains important for
all values of Q studied.Comment: 3 pages, 5 figure
Theoretical He I Emissivities in the Case B Approximation
We calculate the He I case B recombination cascade spectrum using improved
radiative and collisional data. We present new emissivities over a range of
electron temperatures and densities. The differences between our results and
the current standard are large enough to have a significant effect not only on
the interpretation of observed spectra of a wide variety of objects but also on
determinations of the primordial helium abundance.Comment: Accepted to ApJ
Tannins in Perennial Legume and Forb Functional Forages
Feed is the greatest input cost for cattle producers. The studies summarized here employed non-bloating, tannin-containing irrigated perennial legume pastures or hay of legumes or a hydrolysable tannin-containing forb that were grown in the Mountain West USA, with non-tannin legume, grass, or feedlot treatments for comparison. Cattle grazing legume pastures or fed legume or forb hays had greater intake, gain and nitrogen retention, and in some cases, reduced enteric methane emissions compared with grass pastures or hay, and methane emissions were not different from feedlot-fed cattle
Legumes as a Strategy for Reducing Greenhouse Gas Emissions of Forage-Livestock Systems
Incorporation of legumes into forage systems has been a widely adopted strategy to increase pasture productivity and forage nutritive value, while reducing N inputs. Considering the population growth, and the diminishing land resources for food production, the need to increase the food supply will have to be balanced with the environmental impact of these systems, particularly their carbon footprint. Enteric methane production represents the largest source of greenhouse gas emissions from livestock. Certain forage legumes have evolved plant secondary compounds, such as tannins and other polyphenols, which have been associated with reductions in enteric methane emissions. Studies were conducted at Utah State University (USU), and at the University of Florida, North Florida Research and Education Center (UF-NFREC) to assess in vivo methane emissions in grazing cattle, using the SF6 tracer technique. At USU, cattle grazing pastures of Birdsfoot trefoil (Lotus corniculatus; BFT) emitted less methane per unit of dry matter consumed when compared with cattle fed a totally mixed ration (50% barley grain, 25% alfalfa hay, and 25% corn silage) in ad libitum amounts. However, emissions in cattle grazing BFT did not differ from those grazing the legume Cicer milkvetch (Astragalus cicer), or a traditional pasture-finishing system based on Meadow brome (Bromus riparius). At UF-NFREC, three livestock-forage systems were tested during three consecutive years to determine the effects of including the legume Rhizoma peanut (Arachis glabrata Benth.; BHR) in bahiagrass pastures (Paspalum notatum Flügge) fertilized (BH) or not (BHF) with N during the warm season. No differences were observed in methane emissions (g d-1), or in methane emission intensity. From the legumes grazed in these experiments, only BFT contains significant concentrations of tannins. Thus, the potential to mitigate livestock enteric methane emissions by grazing legumes appears to be directly related to the presence of tannins
Rotational Cooling of Polar Molecules by Stark-tuned Cavity Resonance
A general scheme for rotational cooling of diatomic heteronuclear molecules
is proposed. It uses a superconducting microwave cavity to enhance the
spontaneous decay via Purcell effect. Rotational cooling can be induced by
sequentially tuning each rotational transition to cavity resonance, starting
from the highest transition level to the lowest using an electric field.
Electrostatic multipoles can be used to provide large confinement volume with
essentially homogeneous background electric field.Comment: 10 pages, 6 figure
Two-species magneto-optical trap with 40K and 87Rb
We trap and cool a gas composed of 40K and 87Rb, using a two-species
magneto-optical trap (MOT). This trap represents the first step towards cooling
the Bose-Fermi mixture to quantum degeneracy. Laser light for the MOT is
derived from laser diodes and amplified with a single high power semiconductor
amplifier chip. The four-color laser system is described, and the
single-species and two-species MOTs are characterized. Atom numbers of 1x10^7
40K and 2x10^9 87Rb are trapped in the two-species MOT. Observation of trap
loss due to collisions between species is presented and future prospects for
the experiment are discussed.Comment: 4 pages, 4 figures; accepted for publication in Physical Review
Uncertainties in Theoretical HeI Emissivities: HII Regions, Primordial Abundance, and Cosmological Recombination
A number of recent works in astronomy and cosmology have relied upon
theoretical He I emissivities, but we know of no effort to quantify the
uncertainties in the atomic data. We analyze and assign uncertainties to all
relevant atomic data, perform Monte Carlo analyses, and report standard
deviations in the line emissivities. We consider two sets of errors, which we
call "optimistic" and "pessimistic." We also consider three different
conditions, corresponding to prototypical Galactic and extragalactic H II
regions and the epoch of cosmological recombination. In the extragalactic H II
case, the errors we obtain are comparable to or larger than the errors in some
recent calculations, including those derived from CMB observations. We
demonstrate a systematic effect on primordial abundance calculations; this
effect cannot be reduced by observing a large number of objects. In the
cosmological recombination case, the errors are comparable to many of the
effects considered in recent calculations.Comment: 5 pages, 3 figures, accepted to MNRAS Letter
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