Niereninfiltrationen bei malignen Lymphomen

Weiss, Andrew; Weiß, H.; Doring, A.

doi:10.1007/978-3-642-93467-4_47

Cited by 23 publications

(40 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Finally, y-ray observations during the first several years of their outburst done with the next generation of satellite observatories, could confirm the presence of decays from 7Be and 22Na (Weiss and Truran 1990;Nofar et al 1991;Jean et al, 2000, and reference therein). In the next section we report on new calculations done with the new reaction library of Iliadis et al (2000).…”

Section: Introductionmentioning

confidence: 92%

Nuclear reaction rates and the nova outburst

Starrfield¹,

Iliadis²,

Truran³

et al. 2001

Nuclear Physics A

View full text Add to dashboard Cite

Classical novae participate in the cycle of Galactic chemical evolution in which grains and metal enriched gas in their ejects, supplementing those of supernovae, AGB stars, and WR stars, are a source of heavy elements for the ISM. Once in the diffuse gas, this material is cycled through molecular clouds before being incorporated into young stars and planetary systems during star formation. Infrared observations have confirmed the presence of carbon, SiC, hydrocarbons, and oxygen-rich silicate grains in nova ejects, suggesting that some fraction of the pre-solar grains recently identified in meteoritic material may come from novae. The mean mass returned by a nova outburst to the ISM probably exceeds w 2 x 10-4 M~. Using the observed nova rate of 35+11 per year in our Galaxy, it follows that novae introduce more than N 7 x 10-3 M@ yr-l of processed matter into the ISM. It is likely, however, that novae ejects are more massive than believed, and this value is a lower limit. Novae are expected to be the major source of 15N and 170 in the Galaxy and to contribute to the abundances of other isotopes in this atomic mass range. In order to understand better their contributions to galactic chemical evolution, we have begun a series of studies with the latest nuclear reaction rate libraries. We report both on how these new rates affect the properties of the outburst and, in addition, how they change the predictions of the contributions of novae to Galactic chemical evolution.

show abstract

Section: Introductionmentioning

confidence: 92%

Nuclear reaction rates and the nova outburst

Starrfield¹,

Iliadis²,

Truran³

et al. 2001

Nuclear Physics A

View full text Add to dashboard Cite

show abstract

“…In fact, 26 Mg is found in meteorites and in presolar dust grains, implying injections of 26 Al in the solar system nebula (Hoppe et al 1994;MacPherson et al 1995;Huss et al 1997). There are three astrophysical sites for 26 Al nucleosynthesis: the first with most copious production are massive stars; the second, first discovered by Weiss & Truran (1990), are classical and recurrent novae; and the third are asymptotic giant branch stars (see discussion and additional references in Iliadis et al 2011;Bennett et al 2013). If the production of novae and asymptotic giant branch stars can be constrained, the rate of production of 26 Al can be used to derive the Galactic rate of core collapse supernovae, and with it the production rate of many other elements.…”

Section: The Detection Of Al Linesmentioning

confidence: 99%

Chemical and Physical Parameters From X-Ray High-Resolution Spectra of the Galactic Nova V959 Mon

Peretz

Orio

Behar

et al. 2016

ApJ

View full text Add to dashboard Cite

Two observations of V959 Mon, done using the Chandra X-ray gratings during the late outburst phases (2012 September and December), offer extraordinary insight into the physics and chemistry of this Galactic ONe nova. The X-ray flux was 1.7 × 10 −11 erg cm −2 s −1 and 8.6 × 10 −12 erg cm −2 s −1 , respectively at the two epochs. The first result, coupled with electron density diagnostics and compared with published optical and ultraviolet observations, indicates that most likely in 2012 September the X-rays originated from a very small fraction of the ejecta, concentrated in very dense clumps. We obtained a fairly good fit to the September spectrum with a model of plasma in collisional ionization equilibrium (CIE) with two components; one at a temperature of 0.78 keV, associated with flat-topped and asymmetrical emission lines, blueshifted by 710-930 km s −1 ; the other at a temperature of 4.5 keV, mostly contributing to the high-energy continuum. However, we cannot rule out a range of plasma temperatures between these two extremes; we also modeled the spectrum as a static cooling flow, but the available models and the data quality are not adequate yet to differentiate between the two-component fit and a smoothly varying temperature structure. In December, the central white dwarf (WD) became visible in X-rays. We estimate an effective temperature of 680,000 K, consistent with a WD mass ≥1.1 M . The WD flux is modulated with the orbital period, indicating high inclination, and two quasi-periodic modulations with hour timescales were also observed. No hot plasma component with temperature above 0.5 keV was observed in December, and the blueshifted component cooled to kT 0.45 keV. Additionally, new emission lines due to a much cooler plasma appeared, which were not observed two months earlier. We estimate abundances and yields of elements in the nova wind that cannot be measured in the optical spectra and confirm the high Ne abundance previously derived for this nova. We also find high abundance of Al, 230 times the solar value, consistently with the prediction that ONe novae contribute to at least 1/3rd of the Galactic yield of 26 Al.

show abstract

“…Networks with dozens to hundreds of species are employed in stellar evolution codes (e.g., Arnett 1977;Weaver et al 1978;Maeder & Meynet 2000;Paxton et al 2011;Bressan et al 2012;Jones et al 2015). Similar-sized or larger (up to hundreds of species) networks are also used to compute explosive nucleosynthesis in SNe Ia (e.g., Thielemann et al 1986a;Iwamoto et al 1999;Hillebrandt et al 2013;Seitenzahl et al 2013;Leung et al 2015), core-collapse supernovae (e.g., Thielemann et al 1996;Limongi & Chieffi 2003;Heger & Woosley 2010;Harris et al 2014), novae (e.g., Weiss & Truran 1990;José & Hernanz 1998;Iliadis et al 2002;Starrfield et al 2016), and X-ray bursts (e.g., Schatz et al 2001;Woosley et al 2004;Cyburt et al 2010;Parikh et al 2013).…”

Section: Introductionmentioning

confidence: 99%

SkyNet: A Modular Nuclear Reaction Network Library

Lippuner

Roberts

2017

ApJS

136

View full text Add to dashboard Cite

Almost all of the elements heavier than hydrogen that are present in our solar system were produced by nuclear burning processes either in the early universe or at some point in the life cycle of stars. In all of these environments, there are dozens to thousands of nuclear species that interact with each other to produce successively heavier elements. In this paper, we present SkyNet, a new general-purpose nuclear reaction network that evolves the abundances of nuclear species under the influence of nuclear reactions. SkyNet can be used to compute the nucleosynthesis evolution in all astrophysical scenarios where nucleosynthesis occurs. SkyNet is free and open source, and aims to be easy to use and flexible. Any list of isotopes can be evolved, and SkyNet supports different types of nuclear reactions. SkyNet is modular so that new or existing physics, like nuclear reactions or equations of state, can easily be added or modified. Here, we present in detail the physics implemented in SkyNet with a focus on a self-consistent transition to and from nuclear statistical equilibrium to non-equilibrium nuclear burning, our implementation of electron screening, and coupling of the network to an equation of state. We also present comprehensive code tests and comparisons with existing nuclear reaction networks. We find that SkyNet agrees with published results and other codes to an accuracy of a few percent. Discrepancies, where they exist, can be traced to differences in the physics implementations.

show abstract

Niereninfiltrationen bei malignen Lymphomen

Cited by 23 publications

References 1 publication

Nuclear reaction rates and the nova outburst

Nuclear reaction rates and the nova outburst

Chemical and Physical Parameters From X-Ray High-Resolution Spectra of the Galactic Nova V959 Mon

SkyNet: A Modular Nuclear Reaction Network Library

Contact Info

Product

Resources

About