Origin of anomalous Xe-H in presolar diamonds: Indications of a "cold" r-process

We report on a concerted effort aimed at understanding the nucleosynthesis origin of Xe-H in presolar nanodiamonds. Previously explored possible explanations have included a secondary neutron-burst process occurring in the He-shell of a type II supernova (SN), as well as a rapid separation, between unstable precursor isobars of a primary r-process, and stable Xe isotopes. Here we present results from the investigation of a rapid neutron-capture scenario in core-collapse SNe with different non-standard r-process variants. Our calculations are performed in the framework of the high-entropy-wind (HEW) scenario using updated nuclear-physics input. We explore the consequences of varying the wind expansion velocity (Vexp) for selected electron fractions (Ye) with their correlated entropy ranges (S), and neutron-freezeout temperatures (T9(freeze)) and timescales (tau-r(freeze). We draw several conclusions: For Xe-H a "cold" r-process with a fast freezeout seems to be the favored scenario. Furthermore, eliminating the low-S range (i.e. the "weak" r-process component) and maintaining a pure "main" or even "strong" r-process leads to an optimum overall agreement with the measured iXe/136Xe abundance ratios. Our results can provide valuable additional insight into overall astrophysical conditions of producing the r-process part of the total SS heavy elements in explosive nucleosynthesis scenarios.Comment: 6 pages, 2 figures XII International Symposium on Nuclei in the Cosmos, August 5-12, 2012, Cairns, Australi

He and Ne ages of large presolar silicon carbide grains: Solving the recoil problem

Knowledge about the age of presolar grains provides important insights into Galactic chemical evolution and the dynamics of grain formation and destruction processes in the Galaxy. Determination from the abundance of cosmic ray interaction products is straightforward, but in the past has suffered from uncertainties in correcting for recoil losses of spallation products. The problem is less serious in a class of large (tens of micrometer) grains. We describe the correction procedure and summarise results for He and Ne ages of presolar SiC "Jumbo" grains that range from close to zero to ~850 Myr, with the majority being less than 200 Myr. We also discuss the possibility of extending our approach to the majority of smaller SiC grains and explore possible contributions from trapping of cosmic rays.Comment: Publications of the Astronomical Society of Australia, Contribution to PASA special volume "The Origin of Elements Heavier than Iron in honor of the 70th birthday of Roberto Gallino

Origin of the p-process radionuclides ⁹²Nb and ¹⁴⁶Sm in the early solar system and inferences on the birth of the Sun

The abundances of ⁹²Nb and ¹⁴⁶Sm in the early solar system are determined from meteoritic analysis, and their stellar production is attributed to the p process. We investigate if their origin from thermonuclear supernovae deriving from the explosion of white dwarfs with mass above the Chandrasekhar limit is in agreement with the abundance of ⁵³Mn, another radionuclide present in the early solar system and produced in the same events. A consistent solution for ⁹²Nb and ⁵³Mn cannot be found within the current uncertainties and requires the ⁹²Nb/⁹²Mo ratio in the early solar system to be at least 50% lower than the current nominal value, which is outside its present error bars. A different solution is to invoke another production site for ⁹²Nb, which we find in the α-rich freezeout during core-collapse supernovae from massive stars. Whichever scenario we consider, we find that a relatively long time interval of at least ∼10 My must have elapsed from when the star-forming region where the Sun was born was isolated from the interstellar medium and the birth of the Sun. This is in agreement with results obtained from radionuclides heavier than iron produced by neutron captures and lends further support to the idea that the Sun was born in a massive star-forming region together with many thousands of stellar siblings

Micro-Raman study of nanodiamonds from the Allende meteorite

We have studied the Raman spectroscopic signatures of nanodiamonds from the Allende meteorite in which some portions must be of presolar origin as indicated by the isotopic compositions of various trace elements. The spectra of the meteoritic nanodiamond show a narrow peak at 1326 cm‑1 and a broad band at 1590 cm‑1. Compared to the intensities of these peaks, the background fluorescence is relatively high. A significant frequency shift from 1332 to 1326 cm‑1, peak broadening, and appearance of a new peak at 1590 cm‑1 might be due to shock effects during formation of the diamond grains. Such changes may have several origins: an increase in bond length, a change in the electron density function or charge transfer, or a combination of these factors. However, Raman spectroscopy alone does not allow distinguishing between a shock origin of the nanodiamonds and formation by a CVD process as is favored by most workers

Ubiquitination of HIV-1 and MuLV Gag

AbstractOur previous biochemical studies of HIV-1 and MuLV virions isolated and identified mature Gag products, HIV-1 p6Gag and MuLV p12Gag, that were conjugated to a single ubiquitin. To study the importance of the monoubiquitination of Gag, a series of lysine to arginine mutants were constructed that eliminated ubiquitination at one or both of the lysines in HIV-1NL4-3 p6Gag and both lysines in Moloney MuLV p12Gag. HPLC and immunoblot analysis of the HIV-1 mutants demonstrated that either of the lysines in p6Gag, K27 or K33, could be monoubiquitinated. However, infectivity assays showed that monoubiquitination of HIV-1 p6Gag or MuLV p12Gag is not required for viral replication in vitro. Pulse-chase radiolabeling of HIV-1-producing cells revealed that monoubiquitination of p6Gag does not affect the short-term release of virus from the cell, the maturation of Pr55Gag, or the sensitivity of these processes to proteasome inhibitors. Experiments with protease-deficient HIV-1 showed that Pr55Gag can be monoubiquitinated, suggesting that p6Gag is first modified as a domain within Gag. Examination of the proteins inside an HIV-1 mutant found that free ubiquitin was incorporated into the virions in the absence of the lysines in p6Gag, showing that the ubiquitin inside the virus is not initially brought in as a p6Gag conjugate. Although our results establish that monoubiquitination of p6Gag and p12Gag is not required for viral replication in vitro, this modification may be a by-product of interactions between Gag and cellular proteins during assembly and budding

He and Ne Ages of Large Presolar Silicon Carbide Grains: Solving the Recoil Problem

Knowledge about the age of presolar grains provides important insights into Galactic chemical evolution and the dynamics of grain formation and destruction processes in the Galaxy. Determination from the abundance of cosmic ray interaction products is straightforward, but in the past has suffered from uncertainties in correcting for recoil losses of spallation products. The problem is less serious in a class of large (tens of μm) grains. We describe the correction procedure and summarise results for He and Ne ages of presolar SiC ‘Jumbo' grains that range from close to zero to ∼850 Myr, with the majority being less than 200 Myr. We also discuss the possibility of extending our approach to the majority of smaller SiC grains and explore possible contributions from trapping of cosmic ray

Long-Lived Inverse Chirp Signals from Core-Collapse in Massive Scalar-Tensor Gravity.

This Letter considers stellar core collapse in massive scalar-tensor theories of gravity. The presence of a mass term for the scalar field allows for dramatic increases in the radiated gravitational wave signal. There are several potential smoking gun signatures of a departure from general relativity associated with this process. These signatures could show up within existing LIGO-Virgo searches