Engineering Papers⌕ Search

SEARCH · Engineering Papers

Results for “MASS NUMBER”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.

At least 109 records · Page 6
All sourcesNASA NTRSDOE OSTI
DOE OSTI2015

Clusters in nuclear matter and Mott points

Light clusters (mass number A ≤ 4) in nuclear matter at subsaturation densities are described using a quantum statistical approach. In addition to self-energy and Pauli-blocking, effects of continuum correlations are taken into account to calculate the quasiparticle properties and abundances of light elements. Medium-modified quasiparticle properties are important ingredients to derive a nuclear matter equation of state applicable in the entire region of warm dense matter below saturation density. The influence of the nucleon—nucleon interaction on the quasiparticle shift is discussed.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗
DOE OSTI2018

Impact of Tensor Interaction on Beta-Delayed Neutron Emission from Neutron-Rich Nickel Isotopes

The Skyrme energy density functional including tensor interaction is used to describe microscopically multineutron delayed-neutron emission accompanying beta decay of even–even neutron-rich nickel isotopes of mass number in the range of A = 74−80. The respective calculations are performed in the quasiparticle random-phase approximation with allowance for the two-phonon components of the wave function for states of the daughter nucleus. The properties of the lowest quadrupole excitation of {sup 74,76,78,80}Ni are also studied. It is shown that a decrease in the strength of neutron–proton tensor interaction leads to a substantial hindrance of beta decay and to an increase in the probability for delayedneutron emission.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2017

Nuclear Data Sheets for A=138☆

Experimental nuclear structure data from various reactions and decays are compiled and evaluated for all known nuclides with mass number A=138 (Sn,Sb,Te,I,Xe,Cs,Ba,La,Ce,Pr,Nd,Pm,Sm,Eu,Gd,Tb). Detailed evaluated nuclear structure information is presented for each reaction and decay and the best values combining all available data are recommended for level energies, half-lives, γ-ray energies and intensities, decay properties (energies, intensities and placement of radiations), and other spectroscopic properties. This work supersedes the previous full evaluation of A=138 by A.A. Sonzogni (2003So13).

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2017

Special features of the structure of the beta-stability line for nuclei

The mass-number (A) dependence Z{sub β}(A) for nuclei lying on the beta-stability line (BSL) is calculated for A and Z values in the ranges of A = 2–258 and Z = 1–100, respectively. The calculated values are compared with experimental data. The deviations ΔZ = Z{sub expt} − Z{sub β} are analyzed. This analysis of ΔZ reveals that there are three regions of A values in which the A dependence of ΔZ is parabolic. The possible forms of the A dependence of ΔZ are analyzed, and it is shown that the majority of nuclei belong to several parabolas simultaneously.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2019

Ground-state and stability properties of 288-308 118 Og isotopes based on semi-microscopic calculations

In this study, we present theoretical predictions on the stability properties of the yet unknown {sup 276−293,295−308}{sub 118}Og isotopes using the Skyrme-SLy4 nucleon–nucleon interaction and the deformed Woods–Saxon single-particle potential in a semi-microscopic approach. The ground-state masses, binding energy, deformations and fission barriers are calculated from the total energy surfaces produced in a multidimensional deformation space using the dynamical differential evolution optimization method. Besides, the Q-values of the different decay modes and the nucleon separation energies for each isotope, and its α-decay (T{sub α}) and spontaneous fission half-lives are also calculated. Our study revealed the {sub 290−296}Og elements to be the most bound Oganesson isotopes, among which {sup 302,304,306}Og elements are predicted to be spherical nuclei, and {sup 299,300,301,303,305}Og elements are shown to be almost spherical. The predicted ground-state and decay properties successfully reproduced the available data of the solely known Oganesson isotope {sup 294}Og. In addition to the principle α-decay modes, we studied the rival decay modes that challenge the stability of nuclei in the superheavy regions, namely the electron capture β{sup +} decays and the spontaneous fission. An overall oscillating increasing behavior of T{sub α} with the mass number is obtained, which obviously reverses the hesitating decreasing behavior of Q{sub α} and follows increasing trend of the corresponding change in the neutron-skin thickness after α-decays. The {sub 291,294−296,299−302}Og isotopes are expected to have relatively long half-lives, T{sub α} ≈ 1–45 ms, while {sup 295}Og is found to have the longest half-life between the considered nuclei. The {sub 291−300}Og isotopes exhibited relatively high fission barriers and small branching ratios for their spontaneous fission modes.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2013

SYSTEMATICS OF DYNAMICAL MASS EJECTION, NUCLEOSYNTHESIS, AND RADIOACTIVELY POWERED ELECTROMAGNETIC SIGNALS FROM NEUTRON-STAR MERGERS

We investigate systematically the dynamical mass ejection, r-process nucleosynthesis, and properties of electromagnetic counterparts of neutron-star (NS) mergers in dependence on the uncertain properties of the nuclear equation of state (EOS) by employing 40 representative, microphysical high-density EOSs in relativistic, hydrodynamical simulations. The crucial parameter determining the ejecta mass is the radius R{sub 1.35} of a 1.35 M{sub Sun} NS. NSs with smaller R{sub 1.35} (''soft'' EOS) eject systematically higher masses. These range from {approx}10{sup -3} M{sub Sun} to {approx}10{sup -2} M{sub Sun} for 1.35-1.35 M{sub Sun} binaries and from {approx}5 Multiplication-Sign 10{sup -3} M{sub Sun} to {approx}2 Multiplication-Sign 10{sup -2} M{sub Sun} for 1.2-1.5 M{sub Sun} systems (with kinetic energies between {approx}5 Multiplication-Sign 10{sup 49} erg and 10{sup 51} erg). Correspondingly, the bolometric peak luminosities of the optical transients of symmetric (asymmetric) mergers vary between 3 Multiplication-Sign 10{sup 41} erg s{sup -1} and 14 Multiplication-Sign 10{sup 41} erg s{sup -1} (9 Multiplication-Sign 10{sup 41} erg s{sup -1} and 14.5 Multiplication-Sign 10{sup 41} erg s{sup -1}) on timescales between {approx}2 hr and {approx}12 hr. If these signals with absolute bolometric magnitudes from -15.0 to -16.7 are measured, the tight correlation of their properties with those of the merging NSs might provide valuable constraints on the high-density EOS. The r-process nucleosynthesis exhibits a remarkable robustness independent of the EOS, producing a nearly solar abundance pattern above mass number 130. By the r-process content of the Galaxy and the average production per event the Galactic merger rate is limited to 4 Multiplication-Sign 10{sup -5} yr{sup -1} (4 Multiplication-Sign 10{sup -4} yr{sup -1}) for a soft (stiff) NS EOS, if NS mergers are the main source of heavy r-nuclei. The production ratio of radioactive {sup 232}Th to {sup 238}U attains a stable value of 1.64-1.67, which does not exclude NS mergers as potential sources of heavy r-material in the most metal-poor stars.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2014

Collective and non-collective structures in nuclei of mass region A ≈ 125

Generation of angular momentum in nuclei is a key question in nuclear structure studies. In single particle model, it is due to alignment of spin of individual nucleon available in the valence space, whereas coherent motion of nucleons are assumed in the collective model. The nuclei near the closed shell at Z = 50 with mass number A ≈ 120-125 represent ideal cases to explore the interplay between these competing mechanisms and the transition from non-collective to collective behavior or vice versa. Recent spectroscopic studies of nuclei in this region reveal several non-collective maximally aligned states representing the first kind of excitation mechanism, where 8-12 particles above the {sup 114}Sn align their spins to generate these states. Deformed rotational bands feeding the non-collective states in the spin range I=20-25 and excitation energies around 10 MeV have also been observed. Structure of the collective and non-collective states are discussed in the framework of Cranked-Nilsson-Strutinsky model.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2016

Nuclear Data Sheets for A = 79

Nuclear spectroscopic information for known nuclides of mass number 79 (Ni,Cu,Zn,Ga,Ge,As,Se,Br,Kr,Rb, Sr,Y,Zr) has been evaluated and presented together with adopted energies, Jπ, and decay modes of levels in these nuclei. No data are yet available for excited states in {sup 79}Ni, {sup 79}Cu and {sup 79}Zr. The half–life of {sup 79}Se, a nuclide of importance in reactor–irradiated fuel composition has been measured by several independent groups and reported in a number of publications after 1995, and seems to be converging to a narrow margin of experimental values. These measurements were likely prompted by a recommendation made in the 1993 update of A = 79 nuclides (1993Si28), that since a 1949PaZZ report, there had been no measurement until 1993, and that based on simulation studies by 1993HeZW, the value listed in 1949PaZZ, and cited in all data tables and charts for 44 years, was quite likely in error, being too low by a factor of 10. According to conclusions in recent papers such as 2014Do20, there is still room for improvement in the measurement of this half–life, and further experiments are expected. This evaluation supersedes earlier Nuclear Data Sheets for A = 79 (2002Si13,1993Si28, 1982Si21,1975Ur03).

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2018

Nuclear Data Sheets for A=136☆

Spectroscopic data for all nuclei with mass number A=136 have been evaluated and the corresponding level schemes from radioactive decay and reaction studies are presented. No excited states are known in {sup 136}In, {sup 136}Eu, or {sup 136}Gd and {sup 136}Tb remains unidentified. Discrepancies between experiments on isomeric decays in {sup 136}Sb and {sup 136}La suggest the need for futher experimental investigation. The decay of {sup 136}Eu has only been observed in a mixed source. The energy of the 17.5 s isomer in {sup 136}Cs was determined since the last evaluation, however, the branching ratio remains unknown. This work supersedes the earlier full evaluation of A=136 by A.A. Sonzogni (2002So05), and benefited tremendously from all previous evaluations of A=136.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2016

Overall picture of the cascade gamma decay of neutron resonances within a modified practical model

The intensities of two-step cascades in 43 nuclei of mass number in the range of 28 ≤ A ≤ 200 were approximated to a high degree of precision within a modified version of the practical cascade-gammadecay model introduced earlier. In this version, the rate of the decrease in the model-dependent density of vibrational levels has the same value for any Cooper pair undergoing breakdown. The most probable values of radiative strength functions both for E1 and for M1 transitions are determined by using one or two peaks against a smooth model dependence on the gamma-transition energy. The statement that the thresholds for the breaking of Cooper pairs are higher for spherical than for deformed nuclei is a basic result of the respective analysis. The parameters of the cascade-decay process are now determined to a precision that makes it possible to observe the systematic distinctions between them for nuclei characterized by different parities of neutrons and protons.

74 ATOMIC AND MOLECULAR PHYSICS↗
DOE OSTI2015

Nuclear Data Sheets for A = 182

Nuclear spectroscopic information for known nuclides of mass number 182 (Yb,Lu,Hf,Ta,W,Re,Os,Ir,Pt,Au, Hg,Tl,Pb) with Z=70 to 82 and N=112 to 100 have been evaluated and presented together with adopted energies and Jπ of levels in these nuclei. No excited state data are yet available for {sup 182}Y and {sup 182}Lu, while only limited structure information is available for {sup 182}Pb and {sup 182}Tl. Rotational band structures are known for {sup 182}Hg and {sup 182}Au but spin–parity assignments remain largely tentative. The decays of {sup 182}Lu, {sup 182}Hg, {sup 182}Au and {sup 182}Tl are not well established. The {sup 182}Hf isotope is of geophysical and astrophysical interest. This evaluation supersedes previous full evaluations of A = 182 published by 2010Si13, 1988Fi05 and 1975Sc13, and a selected (mainly high–spin) update of A = 182 published by 1995Si04. Only the Adopted properties of levels and gamma rays are presented in NDS, consult the ENSDF database at (www.nndc.bnl.gov/ensdf/) for details of individual reaction and decay datasets.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2015

Nuclear Data Sheets for A = 86

The experimental nuclear spectroscopic data for known nuclides of mass number 86 (Ga, Ge, As, Se, Br, Kr, Rb, Sr, Y, Zr, Nb, Mo, Tc) have been evaluated and presented together with Adopted properties for levels and γ rays. New high-spin data are available for {sup 86}Se, {sup 86}Br, {sup 86}Kr, {sup 86}Sr, {sup 86}Y, {sup 86}Zr and {sup 86}Mo; and lifetime data for high-spin states in {sup 86}Y and {sup 86}Zr. No significant new data since the 2001 NDS for A=86 have been reported for {sup 86}Rb and {sup 86}Nb. No data are yet available for excited states in {sup 86}Ga and {sup 86}As. The decay scheme of radioactive {sup 86}Ge is unknown, while those for {sup 86}Ga, {sup 86}As, 47.4 min isomer of {sup 86}Y, {sup 86}Nb and {sup 86}Tc are deemed as incomplete. Isomerism in {sup 86}Nb remains unconfirmed. This work supersedes the data presented in the previous NDS evaluation of A=86 published by 2001Si43.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2016

Nuclear Data Sheets for A = 42

The experimental data are evaluated for known nuclides of mass number A = 42 (Al, Si, P, S, Cl, Ar, K, Ca, Sc, Ti, V, Cr). Detailed evaluated level properties and related information are presented, including adopted values of level and γ–ray energies, decay data (energies, intensities and placement of radiations), and other spectroscopic data. This work supersedes earlier full evaluations of A = 42 published by B. Singh, J.A. Cameron – Nucl.Data Sheets 92, 1 (2001) and P.M. Endt – Nucl. Phys. A521, 1 (1990); Errata and Addenda Nucl. Phys. A529, 763 (1991); Errata Nucl. Phys. A564, 609 (1993) (also P.M. Endt – Nucl. Phys. A633, 1 (1998) update). No excited states are known in {sup 42}Al, {sup 42}P, {sup 42}V and {sup 42}Cr, and structure information for {sup 42}Si and {sup 42}S is quite limited. There are no decay schemes available for the decay of {sup 42}Al, {sup 42}Si, {sup 42}P, {sup 42}V and {sup 42}Cr, while the decay schemes of {sup 42}Cl and {sup 42}Ti are incomplete in view of scarcity of data, and large gap between their Q–values and the highest energy levels populated in corresponding daughter nuclei. Structures of {sup 42}Ca, {sup 42}K, {sup 42}Sc and {sup 42}Ar nuclides remain the most extensively studied via many different nuclear reactions and decays.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2015

Nuclear Data Sheets for A = 224

The experimental nuclear spectroscopic data for ten experimentally known nuclides of mass number 224 (Bi, Po, At, Rn, Fr, Ra, Ac, Th, Pa, U) have been evaluated and presented together with the Adopted properties for levels and γ rays. For {sup 224}Bi, {sup 224}Po, {sup 224}At, {sup 224}Rn, {sup 224}Fr, {sup 224}Pa and {sup 224}U nuclei, only the ground–state information is known. Half–lives of ground states of 224Bi and 224Po have not yet been measured. The decay of {sup 224}Rn to {sup 224}Fr has been studied, but no decay scheme has been proposed. The decay of {sup 224}Ac to {sup 224}Ra is reported only in an abstract style conference proceedings. For a definite Jπ assignment for ground state of {sup 224}Ac, a detailed study of this decay may be helpful. In the decay of {sup 228}Pa to {sup 224}Ac, authors of 1994Ah03 state that the lowest state observed in their work may not be the ground state. Thus an extensive study of {sup 228}Pa α decay, and studies involving nuclear reactions are warranted since the level scheme of {sup 224}Ac presented in this evaluation is considered as incomplete due to the lack of confirmed information about multipolarities, mixing ratios and other spectroscopic details. Three new nuclides {sup 224}Bi, {sup 224}Po, and {sup 224}At are added in this revision, together with new in–beam γ–ray and Coulomb excitation data for {sup 224}Ra. Although, not much new experimental data have appeared since the previous evaluation (1997Ar05), extensive modifications have been made in almost all the datasets. This work supersedes the information presented in the previous NDS evaluations of A = 224: 1997Ar05, 1986Ma45 and 1976El05.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
DOE OSTI2016

Nuclear Data Sheets for A = 139

The experimental nuclear spectroscopic data for known nuclides of mass number 139 (Sn, Sb, Te, I, Xe, Cs, Ba, La, Ce, Pr, Nd, Pm, Sm, Eu, Gd, Tb, Dy) have been evaluated and presented together with adopted properties for levels and gamma rays. This evaluation represents a revision of previous one (2001Bu16) by T.W. Burrows. Since then extensive new data have become available for many A=139 nuclides although, no excited state data are yet available for {sup 139}Sn, {sup 139}Sb, {sup 139}Tb, and {sup 139}Dy. The decay schemes of {sup 139}Sn, {sup 139}Sb, {sup 139}I, {sup 139}Tb and {sup 139}Dy nuclei are not known, and those for {sup 139}Gd and {sup 139}Eu are poorly known. Particle-transfer data are available for {sup 139}Ba, {sup 139}La, {sup 139}Ce and {sup 139}Pr. Limited high-spin data are available for {sup 139}Te, {sup 139}I, {sup 139}Cs, {sup 139}Ba, {sup 139}La and {sup 139}Ce, while such data are extensive for {sup 139}Pr, {sup 139}Nd, {sup 139}Pm, {sup 139}Sm, {sup 139}Eu and {sup 139}Gd. Recent {sup 139}Pm high-spin data from two independent studies using the same reaction and similar beam energy are in conflict and could be improved using state-of-the-art large gamma-detector arrays in contrast to the smaller arrays currently used. Cases for which no new experimental information are available since the last update have undergone checking resulting in some changes in the current work, but for the most part these are taken from the previous evaluations. Thus, the present work has greatly benefited from all prior NDS evaluations (2001Bu16, 1989Bu12, 1981Pe04, 1974Gr46), but at the same time data presented herein supersede those in the earlier evaluations.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗
NASA NTRS2011

Strategic Implications of Human Exploration of Near-Earth Asteroids

The current United States Space Policy [1] as articulated by the White House and later confirmed by the Congress [2] calls for [t]he extension of the human presence from low-Earth orbit to other regions of space beyond low-Earth orbit will enable missions to the surface of the Moon and missions to deep space destinations such as near-Earth asteroids and Mars. Human exploration of the Moon and Mars has been the focus of numerous exhaustive studies and planning, but missions to Near-Earth Asteroids (NEAs) has, by comparison, garnered relatively little attention in terms of mission and systems planning. This paper examines the strategic implications of human exploration of NEAs and how they can fit into the overall exploration strategy. This paper specifically addresses how accessible NEAs are in terms of mission duration, technologies required, and overall architecture construct. Example mission architectures utilizing different propulsion technologies such as chemical, nuclear thermal, and solar electric propulsion were formulated to determine resulting figures of merit including number of NEAs accessible, time of flight, mission mass, number of departure windows, and length of the launch windows. These data, in conjunction with what we currently know about these potential exploration targets (or need to know in the future), provide key insights necessary for future mission and strategic planning.

Drake, Bret G.↗
DOE OSTI2017

Production of energetic light fragments in extensions of the CEM and LAQGSM event generators of the Monte Carlo transport code MCNP6 [Production of energetic light fragments in CEM, LAQGSM, and MCNP6]

We extend the cascade-exciton model (CEM), and the Los Alamos version of the quark-gluon string model (LAQGSM), event generators of the Monte Carlo N-particle transport code version 6 (MCNP6), to describe production of energetic light fragments (LF) heavier than 4 He from various nuclear reactions induced by particles and nuclei at energies up to about 1 TeV/nucleon. In these models, energetic LF can be produced via Fermi breakup, preequilibrium emission, and coalescence of cascade particles. Initially, we study several variations of the Fermi breakup model and choose the best option for these models. Then, we extend the modified exciton model (MEM) used by these codes to account for a possibility of multiple emission of up to 66 types of particles and LF (up to 28 Mg) at the preequilibrium stage of reactions. Then, we expand the coalescence model to allow coalescence of LF from nucleons emitted at the intranuclear cascade stage of reactions and from lighter clusters, up to fragments with mass numbers A ≤ 7, in the case of CEM, and A ≤ 12, in the case of LAQGSM. Next, we modify MCNP6 to allow calculating and outputting spectra of LF and heavier products with arbitrary mass and charge numbers. The improved version of CEM is implemented into MCNP6. Lastly, we test the improved versions of CEM, LAQGSM, and MCNP6 on a variety of measured nuclear reactions. The modified codes give an improved description of energetic LF from particle- and nucleus-induced reactions; showing a good agreement with a variety of available experimental data. They have an improved predictive power compared to the previous versions and can be used as reliable tools in simulating applications involving such types of reactions.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗