Abundance Trends of Alpha and Fe
... This brief discussion of globular cluster abundances has emphasized those elements that are unaffected by the proton-capture synthesis reactions that have created large star-tostar and cluster-to-cluster light element variations. Comparisons of Ni, Cu, Ca, Ba, La, and Eu abundances in globular clust ...
... This brief discussion of globular cluster abundances has emphasized those elements that are unaffected by the proton-capture synthesis reactions that have created large star-tostar and cluster-to-cluster light element variations. Comparisons of Ni, Cu, Ca, Ba, La, and Eu abundances in globular clust ...
Millisecond Pulsars in X-Ray Binaries - CIERA
... oscillations. However, the absence of spins above 619 Hz is extremely significant, given that there is no significant loss of RXTE sensitivity out to 2 kHz. Under the simple assumption of a uniform distribution out to some maximum value, the observed distribution yields an maximum spin frequency of ...
... oscillations. However, the absence of spins above 619 Hz is extremely significant, given that there is no significant loss of RXTE sensitivity out to 2 kHz. Under the simple assumption of a uniform distribution out to some maximum value, the observed distribution yields an maximum spin frequency of ...
Gravitational Waves from 3D MHD Core
... The major task of my PhD thesis was to study the gravitational wave signature of three-dimensional magnetohydrodynamical core-collapse supenova simulations. The foundations of this work were laid in the spring term 2005, when as an undergraduate student I attended a proseminar held by Prof. Dr. B. B ...
... The major task of my PhD thesis was to study the gravitational wave signature of three-dimensional magnetohydrodynamical core-collapse supenova simulations. The foundations of this work were laid in the spring term 2005, when as an undergraduate student I attended a proseminar held by Prof. Dr. B. B ...
Dynamics of the Milky Way
... • Relaxation is expected to have occurred in some globular clusters and the densest nuclei of galaxies Dynamics of the Milky Way --- Part 1: Introduction and Fundamental Stellar Dynamics ...
... • Relaxation is expected to have occurred in some globular clusters and the densest nuclei of galaxies Dynamics of the Milky Way --- Part 1: Introduction and Fundamental Stellar Dynamics ...
Modelling the sulphur chemistry evolution in Orion KL
... of SO and SO2 abundances during Phase II are shown in Fig. 5. We observe the largest differences during the early stage (t < 5 × 104 ), where the increase of one order of magnitude in the hydrogen density of the region mainly provides differences of up to one order of magnitude in the abundances of SO ...
... of SO and SO2 abundances during Phase II are shown in Fig. 5. We observe the largest differences during the early stage (t < 5 × 104 ), where the increase of one order of magnitude in the hydrogen density of the region mainly provides differences of up to one order of magnitude in the abundances of SO ...
Large-eddy simulations of isolated disc galaxies with thermal and
... showed that the local efficiency ff,MC ' 0.1 in individual actively star-forming molecular clouds is much greater than the efficiency on galactic scales, and their depletion time-scale is considerably shorter (τdep < 100 Myr). This implies that molecular clouds convert a sizable fraction 0.1-0.4 of ...
... showed that the local efficiency ff,MC ' 0.1 in individual actively star-forming molecular clouds is much greater than the efficiency on galactic scales, and their depletion time-scale is considerably shorter (τdep < 100 Myr). This implies that molecular clouds convert a sizable fraction 0.1-0.4 of ...
Life and Death of Stars
... More mass → More gravitational energy → Higher core temperature → Faster fusion rate → Shorter time on the main sequence ...
... More mass → More gravitational energy → Higher core temperature → Faster fusion rate → Shorter time on the main sequence ...
ASTROPHYSICAL PARAMETERS OF LS 2883 AND IMPLICATIONS FOR THE Y egueruela ,
... Only a few binary systems with compact objects display TeV emission. The physical properties of the companion stars represent basic input for understanding the physical mechanisms behind the particle acceleration, emission, and absorption processes in these so-called gamma-ray binaries. Here we pres ...
... Only a few binary systems with compact objects display TeV emission. The physical properties of the companion stars represent basic input for understanding the physical mechanisms behind the particle acceleration, emission, and absorption processes in these so-called gamma-ray binaries. Here we pres ...
IR-excesses around nearby Lambda Boo stars are caused by debris
... Gaussian profile with MPFIT2DPEAK in IDL. These sources were visually identifiable as where the stellar emission was expected to be. Observations of the calibration star γ Draconis were reduced and used in conjunction with these observations to serve as a PSF reference star. The PSF reference star c ...
... Gaussian profile with MPFIT2DPEAK in IDL. These sources were visually identifiable as where the stellar emission was expected to be. Observations of the calibration star γ Draconis were reduced and used in conjunction with these observations to serve as a PSF reference star. The PSF reference star c ...
On the evolution and fate of supermassive stars
... Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60 — 1000 M⊙ . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions. Aim ...
... Context. We study the evolution and fate of solar composition super-massive stars in the mass range 60 — 1000 M⊙ . Our study is relevant for very massive objects observed in young stellar complexes as well as for super-massive stars that could potentially form through runaway stellar collisions. Aim ...
Galactic astroarchaeology: reconstructing the bulge history by
... metallicity, is reproduced well by a very fast bulge formation. As one can see, different IMFs predict different absolute [α/Fe] ratios, in the sense that the flatter the IMF, the higher the [α/Fe] ratios, since there are relatively more massive stars in a flatter IMF than in a steeper one. In additio ...
... metallicity, is reproduced well by a very fast bulge formation. As one can see, different IMFs predict different absolute [α/Fe] ratios, in the sense that the flatter the IMF, the higher the [α/Fe] ratios, since there are relatively more massive stars in a flatter IMF than in a steeper one. In additio ...
The impact of surface temperature inhomogeneities on quiescent
... appropriate for the accretion- and nuclear-powered pulsations observed in accreting systems in outburst. However, this calculation has not been performed specifically for hydrogen atmosphere models (which experience greater limb darkening) at temperatures relevant to quiescent NS low-mass X-ray bina ...
... appropriate for the accretion- and nuclear-powered pulsations observed in accreting systems in outburst. However, this calculation has not been performed specifically for hydrogen atmosphere models (which experience greater limb darkening) at temperatures relevant to quiescent NS low-mass X-ray bina ...
The Minimal CFL-Nuclear Interface
... Throughout the remainder of the paper, we will adopt the minimal hypothesis that nuclear matter composed of neutrons, protons and electrons, known to exist at densities of order n0 , and CFL matter, known to exist at asymptotically large densities, exhaust the content of a neutron star. We conclude ...
... Throughout the remainder of the paper, we will adopt the minimal hypothesis that nuclear matter composed of neutrons, protons and electrons, known to exist at densities of order n0 , and CFL matter, known to exist at asymptotically large densities, exhaust the content of a neutron star. We conclude ...
BD−21 3873: another yellow-symbiotic barium star
... insufficient to trigger the symbiotic activity. If these ideas are correct, abundance peculiarities similar to those of AG Dra are expected to be observed in other yellow symbiotic systems as well. One such yellow symbiotic system is BD−21◦ 3873. Allen (1980) assigns the spectral type G to the giant ...
... insufficient to trigger the symbiotic activity. If these ideas are correct, abundance peculiarities similar to those of AG Dra are expected to be observed in other yellow symbiotic systems as well. One such yellow symbiotic system is BD−21◦ 3873. Allen (1980) assigns the spectral type G to the giant ...
Sardinia_SA - Mullard Space Science Laboratory
... much stronger than the direct emission, in contradiction to the basic model for magnetically confined accretion • One possibility has been that the accretion flow is not smooth, known as “blobby” accretion: – gives rise to flares in light curve (c.f. VV Pup) – blobs bury themselves deep in the white ...
... much stronger than the direct emission, in contradiction to the basic model for magnetically confined accretion • One possibility has been that the accretion flow is not smooth, known as “blobby” accretion: – gives rise to flares in light curve (c.f. VV Pup) – blobs bury themselves deep in the white ...
Section IV High-Energy Astrophysics and Cosmology
... velocities (“kicks”) of the final merged black holes via anisotropic gravitational radiation up to several thousands km/s [33, 34, 35]. The basic feature of the gravitational wave (GW) recoil effect is the situation when the SMBH spends a significant fraction of time off nucleus at scales beyond tha ...
... velocities (“kicks”) of the final merged black holes via anisotropic gravitational radiation up to several thousands km/s [33, 34, 35]. The basic feature of the gravitational wave (GW) recoil effect is the situation when the SMBH spends a significant fraction of time off nucleus at scales beyond tha ...
arXiv:astro-ph/9510089 v1 17 Oct 95
... Universe, and also how they are most easily detected. The axion (Section 5) is motivated as a possible solution to the strong CP problem and is in a class by itself. The largest class is the Weakly Interacting Massive Particle (Wimp) class (Sections 4 and 6), which consists of literally hundreds of ...
... Universe, and also how they are most easily detected. The axion (Section 5) is motivated as a possible solution to the strong CP problem and is in a class by itself. The largest class is the Weakly Interacting Massive Particle (Wimp) class (Sections 4 and 6), which consists of literally hundreds of ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.