Lecture 29: Ellipticals and Irregulars
... Integrated light/spectra Emission lines, particularly from neutral hydrogen and molecular gas. ...
... Integrated light/spectra Emission lines, particularly from neutral hydrogen and molecular gas. ...
Weighing Ultracompact Dwarf Galaxies in the Fornax Cluster
... Dwarf galaxies (UCDs) in the Fornax cluster of galaxies. The velocity dispersions, together with highly spatially resolved luminosity profiles from Hubble Space Telescope imaging (ACS camera), allowed us to derive the dynamical masses of the UCDs. We show that the mass-to-light ratios of UCDs in For ...
... Dwarf galaxies (UCDs) in the Fornax cluster of galaxies. The velocity dispersions, together with highly spatially resolved luminosity profiles from Hubble Space Telescope imaging (ACS camera), allowed us to derive the dynamical masses of the UCDs. We show that the mass-to-light ratios of UCDs in For ...
Fulltext PDF - Indian Academy of Sciences
... 10−2 ≤ σ ≤ 10−4 . The nuclear softness parameter is related to the rigidity of the nucleus. Thus, the SD bands are much more rigid than the ND bands. Also, as the deformation in SD nuclei increases, the SD bands become more and more rigid. This suggests a clear correlation between pairing correlatio ...
... 10−2 ≤ σ ≤ 10−4 . The nuclear softness parameter is related to the rigidity of the nucleus. Thus, the SD bands are much more rigid than the ND bands. Also, as the deformation in SD nuclei increases, the SD bands become more and more rigid. This suggests a clear correlation between pairing correlatio ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... – Helium may ignite via a “helium flash” – In red-giant phase, core helium fusion converts helium into carbon & oxygen; hydrogen fusion continues in a surrounding shell – After core no longer contains helium, star may enter “asymptotic giant branch (AGB)” phase; helium continues to burn in a shell t ...
... – Helium may ignite via a “helium flash” – In red-giant phase, core helium fusion converts helium into carbon & oxygen; hydrogen fusion continues in a surrounding shell – After core no longer contains helium, star may enter “asymptotic giant branch (AGB)” phase; helium continues to burn in a shell t ...
Bolte_LRIS_08A
... dSph-to-dSph differences in the metallicity distributions, which suggests a wide variety of star formation and chemical enrichment histories. In the dSph there is also a strong deficiency of stars with [Fe/H]<-3.0 dex compared to the Galactic halo. These finding seem to challenge the idea that dSph ...
... dSph-to-dSph differences in the metallicity distributions, which suggests a wide variety of star formation and chemical enrichment histories. In the dSph there is also a strong deficiency of stars with [Fe/H]<-3.0 dex compared to the Galactic halo. These finding seem to challenge the idea that dSph ...
Excitation of soft dipole modes in electron scattering
... the distortion of the electron wave functions, affecting mostly electron scattering on heavy nuclei. Until now, the electromagnetic response of unstable nuclei far from the stability line has been studied with Coulomb excitation of radioactive beams impinging on a heavy target [4]. This method has b ...
... the distortion of the electron wave functions, affecting mostly electron scattering on heavy nuclei. Until now, the electromagnetic response of unstable nuclei far from the stability line has been studied with Coulomb excitation of radioactive beams impinging on a heavy target [4]. This method has b ...
The Milky Way The Milky Way`s Neighbourhood
... unwind and break suddenly, and the matter and energy that had been contained rushes outward from the Sun. Solar flares can be many thousands of miles long, and they can contain far more energy than all of the energy consumption of all of human history on Earth. What Is A Supernova? A supernova is a ...
... unwind and break suddenly, and the matter and energy that had been contained rushes outward from the Sun. Solar flares can be many thousands of miles long, and they can contain far more energy than all of the energy consumption of all of human history on Earth. What Is A Supernova? A supernova is a ...
Neutron stars: compact objects with relativistic gravity
... equilibrium equations of the gravity model but also by the equation of state2 prevailing at the core of neutron stars [see refs. 36–42, for reviews]. The equation of state is not sufficiently constrained by the terrestrial experiments [43, 44] and there are large uncertainties in the microscopic cal ...
... equilibrium equations of the gravity model but also by the equation of state2 prevailing at the core of neutron stars [see refs. 36–42, for reviews]. The equation of state is not sufficiently constrained by the terrestrial experiments [43, 44] and there are large uncertainties in the microscopic cal ...
powerpoint file - QUB Astrophysics Research Centre
... We need an expression for opacity to solve the eqns of stellar structure. For stars in thermodynamic equilibrium with only a slow outward flow of energy, the opacity should have the form ...
... We need an expression for opacity to solve the eqns of stellar structure. For stars in thermodynamic equilibrium with only a slow outward flow of energy, the opacity should have the form ...
Presentation
... • Despite the complexity of the atomic model and the approximate treatments used, the observed spectral features can be reproduced. • Fine-structure dielectronic processes are important in modelling ionic recombination spectra, particularly at low temperatures (comparable to the fine-structure energ ...
... • Despite the complexity of the atomic model and the approximate treatments used, the observed spectral features can be reproduced. • Fine-structure dielectronic processes are important in modelling ionic recombination spectra, particularly at low temperatures (comparable to the fine-structure energ ...
The isotopic mixture of barium in the metal-poor
... Nucleosynthesis of heavy elements is dominated by the two neutroncapture processes known as the s- and the r-process. Some nuclides can be synthesized by only the s-process, and others by only the r-process. Both processes contribute almost all the remaining nuclides, with the exception of a few hea ...
... Nucleosynthesis of heavy elements is dominated by the two neutroncapture processes known as the s- and the r-process. Some nuclides can be synthesized by only the s-process, and others by only the r-process. Both processes contribute almost all the remaining nuclides, with the exception of a few hea ...
L7 - QUB Astrophysics Research Centre
... We need an expression for opacity to solve the eqns of stellar structure. For stars in thermodynamic equilibrium with only a slow outward flow of energy, the opacity should have the form ...
... We need an expression for opacity to solve the eqns of stellar structure. For stars in thermodynamic equilibrium with only a slow outward flow of energy, the opacity should have the form ...
L59 SOLID QUARK STARS? RX XU ABSTRACT It is
... existence of n-quark clusters in quark matter, leaving n as a free parameter, possibly from 1 to 18 or even larger. Note that n may depend on temperature and baryon density and that more than one kind of quark cluster may appear at a certain phase (i.e., quark clusters with different n’s could coexi ...
... existence of n-quark clusters in quark matter, leaving n as a free parameter, possibly from 1 to 18 or even larger. Note that n may depend on temperature and baryon density and that more than one kind of quark cluster may appear at a certain phase (i.e., quark clusters with different n’s could coexi ...
PHYS3380_110215_bw - The University of Texas at Dallas
... The Life “Clock” of a Massive Star (> 8 Msun) Let’s compress a massive star’s life into one day… H He ...
... The Life “Clock” of a Massive Star (> 8 Msun) Let’s compress a massive star’s life into one day… H He ...
Stellar Temperatures
... This is close to the τ = 2/3 photospheric temperature; for this class, we will not make a distinction. ...
... This is close to the τ = 2/3 photospheric temperature; for this class, we will not make a distinction. ...
Document
... depends on the initial mass of the star. • Although there is a continuous range of masses, there are 4 ranges of masses that capture all of the interesting features. ...
... depends on the initial mass of the star. • Although there is a continuous range of masses, there are 4 ranges of masses that capture all of the interesting features. ...
Observational Constraints on the Most Massive White Dwarf
... Here we plot the same initial-final mass relation from Slide 5, but we vary the assumed age of M35 within the current age uncertainty. The plotted error bars are the white dwarf observational uncertainties. For a younger assumed cluster age, the progenitor masses increase systematically for all of t ...
... Here we plot the same initial-final mass relation from Slide 5, but we vary the assumed age of M35 within the current age uncertainty. The plotted error bars are the white dwarf observational uncertainties. For a younger assumed cluster age, the progenitor masses increase systematically for all of t ...
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.