REVIEWS The formation of the first stars and galaxies Volker Bromm
... candidate for CDM is the neutralino, for which the self-annihilation cross-section is large. Neutralino dark matter is thus expected to pairannihilate in very dense regions, producing high-energy particles such as pions and electron–positron pairs and high-energy photons. These annihilation products ...
... candidate for CDM is the neutralino, for which the self-annihilation cross-section is large. Neutralino dark matter is thus expected to pairannihilate in very dense regions, producing high-energy particles such as pions and electron–positron pairs and high-energy photons. These annihilation products ...
FIRST LIGHT IN THE UNIVERSE
... • In practice, these samples are contaminated by foreground stars, z~2 galaxies etc to an extent which remains controversial. We are unlikely to resolve this definitively with spectroscopy until era of ELTs. • Comoving SF rate declines from z~3 to z~6 (and probably beyond) suggesting insufficient 6< ...
... • In practice, these samples are contaminated by foreground stars, z~2 galaxies etc to an extent which remains controversial. We are unlikely to resolve this definitively with spectroscopy until era of ELTs. • Comoving SF rate declines from z~3 to z~6 (and probably beyond) suggesting insufficient 6< ...
Slide 1 - Komitee für Hadronen
... Active visits program for students from German universities and highschools organized by ISOLDE members Magazine „Kultur und Technik“ of the „Deutsche Museum“, issue 04/2012 Report on work as a scientist at CERN Example ISOLTRAP Experiment at ISOLDE ...
... Active visits program for students from German universities and highschools organized by ISOLDE members Magazine „Kultur und Technik“ of the „Deutsche Museum“, issue 04/2012 Report on work as a scientist at CERN Example ISOLTRAP Experiment at ISOLDE ...
Disk
... outflow detection rate = 40-90% in massive YSOs (luminous IRAS sources, UC HIIs, H2O masers,…) (Osterloh et al., Beuther et al., Zhang et al., …) disks should be widespread! ...
... outflow detection rate = 40-90% in massive YSOs (luminous IRAS sources, UC HIIs, H2O masers,…) (Osterloh et al., Beuther et al., Zhang et al., …) disks should be widespread! ...
Astrophysics with the Computer: Propagation of Ionization Fronts in
... star. Where the radiation hits the gas, a layer will be ionised and hence become optically thin. Thus the stellar photons can penetrate even deeper into the gas. The boundary between neutral and ionised gas (the ionization front) will thus propagate away from the star in to the gas cloud, as long as ...
... star. Where the radiation hits the gas, a layer will be ionised and hence become optically thin. Thus the stellar photons can penetrate even deeper into the gas. The boundary between neutral and ionised gas (the ionization front) will thus propagate away from the star in to the gas cloud, as long as ...
M BH
... BHs can be found in many places and seem to have had great influence on the evolution of the universe. ...
... BHs can be found in many places and seem to have had great influence on the evolution of the universe. ...
Circumstellar medium around rotating massive stars at solar metallicity
... from the zero-age main sequence up to the end of central carbon burning and cover the main stages of stellar evolution: MS, RSG, or WR phase, if any. After carbon is exhausted in the centre of the star, the core evolution becomes so fast that the surface is insensitive to what happens in the core, a ...
... from the zero-age main sequence up to the end of central carbon burning and cover the main stages of stellar evolution: MS, RSG, or WR phase, if any. After carbon is exhausted in the centre of the star, the core evolution becomes so fast that the surface is insensitive to what happens in the core, a ...
Barium Stars: Theoretical Interpretation
... after a limited number of TPs. TDU ceases when the mass of the envelope decreases by mass loss down to ∼0.5 M . The TDU mass per pulse reaches a maximum after about ten thermal pulses and then decreases (Straniero et al. 2003). The major neutron source in AGB stars is the 13 C(α, n)16 O reaction, w ...
... after a limited number of TPs. TDU ceases when the mass of the envelope decreases by mass loss down to ∼0.5 M . The TDU mass per pulse reaches a maximum after about ten thermal pulses and then decreases (Straniero et al. 2003). The major neutron source in AGB stars is the 13 C(α, n)16 O reaction, w ...
ppt - lenac
... Title Studying the low surface brightness galaxies from the SDSS With the advent of large aperture telescopes (VLT, Magellan, GEMINI, etc.) the detailed (high S/N spectroscopy, high spatial resolution, etc.) study of low surface brightness galaxies (LSBGs) become possible. These low stellar density ...
... Title Studying the low surface brightness galaxies from the SDSS With the advent of large aperture telescopes (VLT, Magellan, GEMINI, etc.) the detailed (high S/N spectroscopy, high spatial resolution, etc.) study of low surface brightness galaxies (LSBGs) become possible. These low stellar density ...
Mass loss of massive stars near the Eddington luminosity by core
... observations may infer that some WR stars explode with much larger radii than those predicted by the current stellar evolution theory. One of the characteristics of massive stars shortly before the explosion is their huge neutrino luminosities. Neutrinos are constantly emitted from the stellar core ...
... observations may infer that some WR stars explode with much larger radii than those predicted by the current stellar evolution theory. One of the characteristics of massive stars shortly before the explosion is their huge neutrino luminosities. Neutrinos are constantly emitted from the stellar core ...
The Origin of Matter-Antimatter Asymmetry Ning Bao Prashant Saraswat
... When particle relaxes down center, angular momentum (baryonic charge) remains. ...
... When particle relaxes down center, angular momentum (baryonic charge) remains. ...
Multi-dimensional structure of accreting young stars
... implicit multi-dimensional hydrodynamics simulations. One major motivation is to analyse the validity of accretion treatment used in previous 1D stellar evolution studies. We analyse the effect of accretion on the structure of a realistic stellar model of the young Sun. Our work is inspired by the n ...
... implicit multi-dimensional hydrodynamics simulations. One major motivation is to analyse the validity of accretion treatment used in previous 1D stellar evolution studies. We analyse the effect of accretion on the structure of a realistic stellar model of the young Sun. Our work is inspired by the n ...
Available online www.jsaer.com Journal of Scientific and
... exothermic nuclear reactions liberate energies of several Mev per nucleon, or about 10 9 J per Kg, such nuclear reactions could sustain the energy loss of the sun for about 10 11 years and are the only type of reactions which supply a sufficiently large amount of energy [1]. Stars create their energ ...
... exothermic nuclear reactions liberate energies of several Mev per nucleon, or about 10 9 J per Kg, such nuclear reactions could sustain the energy loss of the sun for about 10 11 years and are the only type of reactions which supply a sufficiently large amount of energy [1]. Stars create their energ ...
Interpretation of the Helix Planetary Nebula using Hydro
... acoustical density fluctuations on scales larger than LJ (Gibson 1996). Contrary to the common misconception, pressure and temperature cannot prevent structure formation on scales larger or smaller than LJ . Density fluctuations in fluids are not barotropic as assumed by Jeans 1902 except rarely in sma ...
... acoustical density fluctuations on scales larger than LJ (Gibson 1996). Contrary to the common misconception, pressure and temperature cannot prevent structure formation on scales larger or smaller than LJ . Density fluctuations in fluids are not barotropic as assumed by Jeans 1902 except rarely in sma ...
Probing the Dark Matter Content of Local Group Dwarf Spheroidal
... of dSphs provide valuable insights into the processes of galaxy formation and evolution on the smallest scales. It is the large apparent mass-to-light ratios of dSph galaxies, and the conclusion that they contain significant amounts of dark matter, that has caused them to attract much attention in r ...
... of dSphs provide valuable insights into the processes of galaxy formation and evolution on the smallest scales. It is the large apparent mass-to-light ratios of dSph galaxies, and the conclusion that they contain significant amounts of dark matter, that has caused them to attract much attention in r ...
Formation and Evolution of Binary Millisecond Pulsars with Helium
... and the subsequent collapse leaves behind a detached (cooling) remnant in orbit with its spun-up NS companion. Since the properties of red giants are dictated primarily by their core masses, mc , and not by the mass of the stars themselves or by the mass-transfer rate, Ṁ2 , it is possible to calcul ...
... and the subsequent collapse leaves behind a detached (cooling) remnant in orbit with its spun-up NS companion. Since the properties of red giants are dictated primarily by their core masses, mc , and not by the mass of the stars themselves or by the mass-transfer rate, Ṁ2 , it is possible to calcul ...
254_1.pdf
... redistribution in the low-density, small-dimensioned fibrous targets used in viable target designs and therefore, must be carefully taken into account. Such fragile, low thermal conductivity targets must withstand irradiation with ≥ 100 kW beams for extended periods of time and therefore, care must ...
... redistribution in the low-density, small-dimensioned fibrous targets used in viable target designs and therefore, must be carefully taken into account. Such fragile, low thermal conductivity targets must withstand irradiation with ≥ 100 kW beams for extended periods of time and therefore, care must ...
No Slide Title
... neutrinos get converted to muon or tau neutrinos and these could not be detected by the early neutrino detectors! ...
... neutrinos get converted to muon or tau neutrinos and these could not be detected by the early neutrino detectors! ...
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.