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At least 19 records
All sourcesNASA NTRSDOE OSTI
DOE OSTI2025

Crust Composition and the Shallow Heat Source in KS 1731–260

The presence of a strong shallow heat source of unknown origin in accreting neutron star crusts has been inferred by analyzing x-ray observations of their cooling in quiescence. Here, we model the cooling of KS 1731–260 using realistic crust compositions and nuclear heating and cooling sources from detailed nuclear reaction network calculations. We find that the required strength of the shallow heat source in KS 1731–260 is reduced by more than a factor of 3 compared to previous analysis, a 5⁢𝜎 difference that alleviates the need for exotic solutions. Our analysis also suggests the existence of an impure nuclear pasta layer in the inner crust of KS 1731–260, though future observations will provide more stringent constraints. In addition, we obtain constraints on the dominant surface burning modes of KS 1731–260 over its history.

neutron star cooling↗
NASA NTRS1983

The LSS 4300: A hot counterpart of Upsilon Sgr and KS Per?

A number of observations indicate that the star LSS 4300 is a high temperature analog of the hydrogen-deficient binaries upsilon Sgr and KS Per. A preliminary model-atmosphere analysis based on high-dispersion spectra obtained at Kitt Peak and Cerro Tololo yields T(eff) = 14,400 K, log(g) = 1.4, n(H)/n(He) = 0.003, and n(N)/n(C) = 20 (the corresponding values for upsilon Sgr are T(eff) = 10,000 K, log(g) = 1, n(H)/n(He) = 0.0005, and n(N)/n(C) = 20). The optical emission-line spectrum of LSS 4300 is nearly identical to that of upsilon Sgr, including strong, broad H alpha, FeII and Ca II emission. The ultraviolet spectrum of LSS 4300 was observed with IUE, and can be attributed almost entirely to the visible star. The JHKL photometry of LSS 4300 obtained at Cerro Tololo reveals an infrared excess nearly identical to that of upsilon Sgr. It is suggested that LSS 4300, like upsilon Sgr and KS Per, is a close binary system consisting of a helium supergiant of about one solar mass, and a secondary which is overluminous for its mass due to the accretion of matter from the primary, which is undergoing its second mass exchange.

Drilling, J. S.↗
NASA NTRS1984

LSS 4300 - A hot counterpart of Upsilon Sagittarii and KS Persei?

A number of recent observations indicate that the star LSS 4300 (HDE 320156) is a high-temperature analog of the hydrogen-deficient binaries Upsilon Sgr and KS Per. A preliminary model-atmosphere analysis based on high dispersion spectra obtained at Kitt Peak and Cerro Tololo yields Teff = 14,400 K, log (g) = 1.4, n(H)/n(He) = 0.003, and n(N)/n(C) = 20 for the visible component. The optical emission-line spectrum of LSS 4300 is nearly identical to that of Upsilon Sgr, including strong, broad H-alpha, Fe II, and forbidden Ca II emission; and JHKL photometry obtained at Cerr Tololo reveals an infrared excess nearly identical to that of Upsilon Sgr. It is suggested that LSS 4300, like Upsilon Sgr and KS Per, is a close binary system consisting of a helium supergiant of about 1 solar mass, which is undergoing its second mass loss, and a less luminous secondary, which is accreting matter from the primary.

Schoenberner, D.↗
NASA NTRS2003

The Ionized Gas and Nuclear Environment in NGC 3783: Variability and Modeling of the 900 ks CHANDRA Spectrum - IV

We present a detailed analysis of the 900 ks spectrum of NGC3783 obtained by Chandra in 2000-2001 (Kaspi et al. 2002). We split the data in various ways to look for time dependent and luminosity dependent spectral variations. This analysis, the measured equivalent widths of a large number of X-ray lines, and our photoionization calculations, lead us to the following conclusions: 1) NGC 3783 fluctuated in luminosity, by a factor N 1.5, during individual 170 ks observations. The fluctuations were not associated with significant spectral variations. 2) On a longer time scale, of 20-120 days, we discovered two very different spectral shapes that are noted the high state and the low state spectra. The observed changes between the two can be described as the appearance and disappearance of a soft continuum component. The spectral variations are not related, in a simple way, to the brightening or the fading of the short wavelength continuum, as observed in other objects. NGC3783 seems to be the first AGN to show this unusual behavior. 3) The appearance of the soft continuum component is consistent with beeing the only spectral variation and there is no need to invoke changes in the absorber s opacity. In particular, all absorption lines with reliable measurements show the same equivalent width, within the observational uncertainties, during high and low states. 4) Photoionization model calculations show that a combination of three ionization components, each split into two kinematic components, explain very well the intensity of almost all absorption lines and the bound-free absorption. The components span a large range of ionization and a total column of about 3 x 10(exp 22) per square centimeter Moreover, all components are thermally stable and are situated on the vertical branch of the stability curve.. This means that they are in pressure equilibrium and perhaps occupy the same volume of space. This is the first detection of such a multi-component equilibrium gas in AGN. 5) The only real discrepancy between the model and the observations is the wavelength of the iron M-shell UTA feature. This is most likely due to an underestimation of the dielectronic recombination O VI and discuss its possible origin. 6) The lower limit on the distance of the absorbing gas in NGC3783 is between 0.2 and 3.2 pc, depending of the specific ionization component. The constant pressure assumption imposes an upper limit of about 25 pc on the distance of the least ionized gas from the central sourec.

Netzer, Hagai↗
NASA NTRS2014

NuSTAR Discovery of a Cyclotron Line in KS 1947+300

We present a spectral analysis of three simultaneous Nuclear Spectroscopy Telescope Array and Swift/XRT observations of the transient Be-neutron star binary KS 1947+300 taken during its outburst in 2013/2014. These broadband observations were supported by Swift/XRTmonitoring snapshots every three days, which we use to study the evolution of the spectrum over the outburst.We find strong changes of the power-law photon index, which shows a weak trend of softening with increasing X-ray flux. The neutron star shows very strong pulsations with a period of P ≈ [almost equal to] 18.8 s. The 0.8-79 keV broadband spectrum can be described by a power law with an exponential cutoff and a blackbody component at low energies. During the second observation we detect a cyclotron resonant scattering feature at 12.5 keV, which is absent in the phase-averaged spectra of observations 1 and 3. Pulse phase-resolved spectroscopy reveals that the strength of the feature changes strongly with pulse phase and is most prominent during the broad minimum of the pulse profile. At the same phases the line also becomes visible in the first and third observation at the same energy. This discovery implies that KS 1947+300 has a magnetic field strength of B ≈ [almost equal to] 1.1 × 1012(1 + z) G, which is at the lower end of known cyclotron line sources.

radiation: dynamics↗
DOE OSTI2023

Continuous cultivation of the lithoautotrophic nitrate‐reducing Fe( II )‐oxidizing culture KS in a chemostat bioreactor

Abstract Laboratory‐based studies on microbial Fe(II) oxidation are commonly performed for 5–10 days in small volumes with high substrate concentrations, resulting in geochemical gradients and volumetric effects caused by sampling. We used a chemostat to enable uninterrupted supply of medium and investigated autotrophic nitrate‐reducing Fe(II)‐oxidizing culture KS for 24 days. We analysed Fe‐ and N‐speciation, cell‐mineral associations, and the identity of minerals. Results were compared to batch systems (50 and 700 mL—static/shaken). The Fe(II) oxidation rate was highest in the chemostat with 7.57 mM Fe(II) d −1 , while the extent of oxidation was similar to the other experimental setups (average oxidation of 92% of all Fe(II)). Short‐range ordered Fe(III) phases, presumably ferrihydrite, precipitated and later goethite was detected in the chemostat. The 1 mM solid phase Fe(II) remained in the chemostat, up to 15 μM of reactive nitrite was measured, and 42% of visualized cells were partially or completely mineral‐encrusted, likely caused by abiotic oxidation of Fe(II) by nitrite. Despite (partial) encrustation, cells were still viable. Our results show that even with similar oxidation rates as in batch cultures, cultivating Fe(II)‐oxidizing microorganisms under continuous conditions reveals the importance of reactive nitrogen intermediates on Fe(II) oxidation, mineral formation and cell–mineral interactions.

59 BASIC BIOLOGICAL SCIENCES↗
NASA NTRS1977

The method of averages applied to the KS differential equations

A new approach for the solution of artificial satellite trajectory problems is proposed. The basic idea is to apply an analytical solution method (the method of averages) to an appropriate formulation of the orbital mechanics equations of motion (the KS-element differential equations). The result is a set of transformed equations of motion that are more amenable to numerical solution.

Graf, O. F., Jr.↗
NASA NTRS1982

The hot component of KS Persei /HD 30353/

The presence of a hot companion for the single-lined spectroscopic binary KS Per (HD 30353) has been detected in a study of low-resolution IUE spectra. The system as a whole is very similar to Upsilon Sgr. The observations are consistent with a model in which the primary is a helium supergiant of about 1 solar mass and the secondary is an overluminous early-type star with a mass of 5-6 solar masses. This model predicts that the system is now undergoing its second mass exchange.

Drilling, J. S.↗
DOE OSTI2020

Materials Data on KS by Materials Project

SK1 is alpha boron-derived structured and crystallizes in the hexagonal P-62m space group. The structure is three-dimensional. there are two inequivalent K1+ sites. In the first K1+ site, K1+ is bonded in a 6-coordinate geometry to six S1- atoms. There are two shorter (3.25 Å) and four longer (3.35 Å) K–S bond lengths. In the second K1+ site, K1+ is bonded in a 6-coordinate geometry to six S1- atoms. There are four shorter (3.17 Å) and two longer (3.25 Å) K–S bond lengths. There are two inequivalent S1- sites. In the first S1- site, S1- is bonded in a 7-coordinate geometry to six K1+ and one S1- atom. The S–S bond length is 2.13 Å. In the second S1- site, S1- is bonded in a 7-coordinate geometry to six K1+ and one S1- atom. The S–S bond length is 2.14 Å.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on KS by Materials Project

SK1 is Tetraauricupride structured and crystallizes in the cubic Pm-3m space group. The structure is three-dimensional. K1+ is bonded in a body-centered cubic geometry to eight equivalent S1- atoms. All K–S bond lengths are 3.32 Å. S1- is bonded in a body-centered cubic geometry to eight equivalent K1+ atoms.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on KS by Materials Project

SK1 is Halite, Rock Salt structured and crystallizes in the cubic Fm-3m space group. The structure is three-dimensional. K1+ is bonded to six equivalent S1- atoms to form a mixture of corner and edge-sharing KS6 octahedra. The corner-sharing octahedral tilt angles are 0°. All K–S bond lengths are 3.26 Å. S1- is bonded to six equivalent K1+ atoms to form a mixture of corner and edge-sharing SK6 octahedra. The corner-sharing octahedral tilt angles are 0°.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on KS by Materials Project

SK1 is Tetraauricupride structured and crystallizes in the tetragonal P4/mmm space group. The structure is three-dimensional. K1+ is bonded in a distorted body-centered cubic geometry to eight equivalent S1- atoms. All K–S bond lengths are 3.26 Å. S1- is bonded in a distorted body-centered cubic geometry to eight equivalent K1+ atoms.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on KS by Materials Project

SK1 crystallizes in the monoclinic C2/m space group. The structure is one-dimensional and consists of two SK1 ribbons oriented in the (0, 0, 1) direction. K1+ is bonded in a linear geometry to two equivalent S1- atoms. Both K–S bond lengths are 3.02 Å. S1- is bonded in a linear geometry to two equivalent K1+ atoms.

36 MATERIALS SCIENCE↗
DOE OSTI2020

KS-TmG.1.0

As part of the Pacific Northwest National Laboratory’s (PNNL) Science Focus Area program we are investigating the impact of environmental change on microbial community function in grassland soils. To enable a comprehensive survey of the metabolic potential of complex soil microbiomes, we performed ultra-deep metagenome sequencing, collecting >1 terabase of sequence data from grassland soils representing different precipitation regimes. Intermediate precipitation regime soil (rain-fed and irrigated agriculture) was collected from Konza Prairie Biological Station (KPBS).

54 ENVIRONMENTAL SCIENCES↗
DOE OSTI2021

KS-TmG.2.0

Soil samples were collected in triplicate in the Fall of 2017 across three grassland locations having differences in historical annual precipitation. For each of the three field site soil collections, one deeply sequenced composite metagenome (> 1 terabase) was obtained and individually sequenced in replicate to provide three additional terabase metagenomes for replicate statistical comparison in addition to screening for viral soil contigs for assessing the impact of historical annual precipitation. This data package provides new knowledge of viral types, abundances, diversity, and auxiliary metabolic genes (AMGs) in grassland soils for predicting viral response to changes in their environment.

59 BASIC BIOLOGICAL SCIENCES↗
NASA NTRS1975

On redundant variables in Lagrangian mechanics, with applications to perturbation theory and KS regularization

It is shown that it is possible to make a change of variables in a Lagrangian in such a way that the number of variables is increased. The Euler-Lagrange equations in the redundant variables are obtained in the standard way (without the use of Lagrange multipliers). These equations are not independent but they are all valid and consistent. In some cases they are simpler than if the minimum number of variables are used. The redundant variables are supposed to be related to each other by several constraints (not necessarily holonomic), but these constraints are not used in the derivation of the equations of motion. The method is illustrated with the well known Kustaanheimo-Stiefel regularization. Some interesting applications to perturbation theory are also described.

Broucke, R.↗