Galaxies on Sub-Galactic Scales
... satellite galaxies over the past seven years. It was instrumental in finding examples of the least luminous galaxies we know in the Universe, uncovering apparent inconsistencies between cold dark matter theory and dwarf galaxy properties, providing first evidence for a possible lower mass limit for ...
... satellite galaxies over the past seven years. It was instrumental in finding examples of the least luminous galaxies we know in the Universe, uncovering apparent inconsistencies between cold dark matter theory and dwarf galaxy properties, providing first evidence for a possible lower mass limit for ...
PDF hosted at the Radboud Repository of the Radboud University
... (α) is high. Assuming that the efficiency is a universal parameter, this means that the much closer HW Vir binaries should have formed from more massive sdB progenitors and thus should have lower masses (see Hu et al. 2007, Fig. 3) than EGB 5. In contrast, the masses of most sdB primaries in HW Vir sy ...
... (α) is high. Assuming that the efficiency is a universal parameter, this means that the much closer HW Vir binaries should have formed from more massive sdB progenitors and thus should have lower masses (see Hu et al. 2007, Fig. 3) than EGB 5. In contrast, the masses of most sdB primaries in HW Vir sy ...
Detecting industrial pollution in the atmospheres of earth
... • Direct exoplanet detection experiments which look for reflection or thermal emission from the planet could then be used to push constraints on industrial pollutants to terrestrial levels. At the same time, these experiments could search for less exotic biosignatures like the “red edge” of chloroph ...
... • Direct exoplanet detection experiments which look for reflection or thermal emission from the planet could then be used to push constraints on industrial pollutants to terrestrial levels. At the same time, these experiments could search for less exotic biosignatures like the “red edge” of chloroph ...
SDSS J105754. 25+ 275947.5: a period
... bright spot, accretion disc and donor star, and is described in detail by Savoury et al. (2011). The model makes a number of important assumptions: the bright spot lies on a ballistic trajectory from the donor, the donor fills its Roche lobe, the white dwarf is accurately described by a theoretical ...
... bright spot, accretion disc and donor star, and is described in detail by Savoury et al. (2011). The model makes a number of important assumptions: the bright spot lies on a ballistic trajectory from the donor, the donor fills its Roche lobe, the white dwarf is accurately described by a theoretical ...
Radio emissions from terrestrial planets around white dwarfs
... argue below that the orbital decay during each pulse is significantly lower than this estimate). The stellar radius then recontracts back towards its quiescent level and the planet remains in a contracted orbit external to the star. After one or more thermal pulses, the planet p2 is dragged into a c ...
... argue below that the orbital decay during each pulse is significantly lower than this estimate). The stellar radius then recontracts back towards its quiescent level and the planet remains in a contracted orbit external to the star. After one or more thermal pulses, the planet p2 is dragged into a c ...
Astrophysical false positives in direct imaging for exoplanets: a white
... composed of 12 acquisitions on the source with small dithering and one acquisition on the sky. Immediately after observing our science targets, we observed the standard star HIP 17280 (B5V) following an AB pattern to correct our spectra for telluric features. HD 8049 and the standard were both obser ...
... composed of 12 acquisitions on the source with small dithering and one acquisition on the sky. Immediately after observing our science targets, we observed the standard star HIP 17280 (B5V) following an AB pattern to correct our spectra for telluric features. HD 8049 and the standard were both obser ...
Document
... Stars with small masses (less than a solar mass) are much more common than massive stars (stars more than about 15 to 20 solar masses). The highest mass stars are very hot and luminous, and can alter the cloud environment. ...
... Stars with small masses (less than a solar mass) are much more common than massive stars (stars more than about 15 to 20 solar masses). The highest mass stars are very hot and luminous, and can alter the cloud environment. ...
ppt - CIERA - Northwestern
... mass segregation. Primordial mass segregation potentially amplified. IMF & survival complex relationship. ...
... mass segregation. Primordial mass segregation potentially amplified. IMF & survival complex relationship. ...
Formation of high-field magnetic white dwarfs from common envelopes
... two classes: AM Herculis (AM Her) (polars) and DQ Herculis (DQ Her) (intermediate polars). For reviews on AM Her and DQ Her systems, see refs. 9 and 10. Generally, AM Her systems are those in which both components of the binary are synchronously rotating at the orbital period. In this scenario, the ...
... two classes: AM Herculis (AM Her) (polars) and DQ Herculis (DQ Her) (intermediate polars). For reviews on AM Her and DQ Her systems, see refs. 9 and 10. Generally, AM Her systems are those in which both components of the binary are synchronously rotating at the orbital period. In this scenario, the ...
Neutron Degeneracy Pressure
... for example, of non-Hydrogen like atoms. This idea of energy state filling becomes crucial when discussing degeneracy pressure. The Pauli Exclusion Principle can also be applied to further our understanding of stars, black holes, supernovae, and many other celestial objects and phenomena studied in ...
... for example, of non-Hydrogen like atoms. This idea of energy state filling becomes crucial when discussing degeneracy pressure. The Pauli Exclusion Principle can also be applied to further our understanding of stars, black holes, supernovae, and many other celestial objects and phenomena studied in ...
The evolution of dwarf galaxy satellites with different dark matter
... Group carried out in a fully cosmological context. We use the ErisDARK cosmological simulation of a MW-sized galaxy to identify some of the most massive subhalos (Mvir > 108 M ) that fall into the main host before z = 2. Subhalos are replaced before infall with high-resolution models of dwarf galax ...
... Group carried out in a fully cosmological context. We use the ErisDARK cosmological simulation of a MW-sized galaxy to identify some of the most massive subhalos (Mvir > 108 M ) that fall into the main host before z = 2. Subhalos are replaced before infall with high-resolution models of dwarf galax ...
Detached WD/BD binaries as progenitors of CVs
... Post-CE binaries with BD secondaries • Constrain models of common envelope evolution • What is the lowest mass object that can survive a CE? • What fraction of CVs are born with a BD secondary? • Growing number of CVs with confirmed BD secondaries – Including examples thought to have formed directl ...
... Post-CE binaries with BD secondaries • Constrain models of common envelope evolution • What is the lowest mass object that can survive a CE? • What fraction of CVs are born with a BD secondary? • Growing number of CVs with confirmed BD secondaries – Including examples thought to have formed directl ...
–1– 1. Stellar Evolution For Massive Stars 1.1. The Importance of
... surface temperature then becomes non-uniform. Rotation causes g(ef f ) to decrease more at the equator and less at the poles, but the radiative flux is higher at the poles, so detailed modeling of these anisotropies is required to predict the form of the wind anisotropy. Such anisotropies have been ...
... surface temperature then becomes non-uniform. Rotation causes g(ef f ) to decrease more at the equator and less at the poles, but the radiative flux is higher at the poles, so detailed modeling of these anisotropies is required to predict the form of the wind anisotropy. Such anisotropies have been ...
Binary Star Systems
... – Sufficiently close to Earth and the stars are well enough separated that we can see the two stars individually (resolved) in a telescope and track their motion over a period of time ...
... – Sufficiently close to Earth and the stars are well enough separated that we can see the two stars individually (resolved) in a telescope and track their motion over a period of time ...
Draft paper (submitted to MNRAS)
... We explore the impact of cosmic reionization on nearby isolated dwarf galaxies using a compilation of star formation histories estimated from deep HST data and a cosmological hydrodynamical simulation of the Local Group. The nearby dwarfs show a wide diversity of star formation histories; from ancie ...
... We explore the impact of cosmic reionization on nearby isolated dwarf galaxies using a compilation of star formation histories estimated from deep HST data and a cosmological hydrodynamical simulation of the Local Group. The nearby dwarfs show a wide diversity of star formation histories; from ancie ...
The Age and Stellar Parameters of the Procyon Binary System
... one possible solution to the masses has limited the claimed accuracy. Preliminary mass determinations for each component are available from HST imaging, supported by ground-based astrometry and an excellent Hipparcos parallax; we use these for our preferred solution for the binary system. Other valu ...
... one possible solution to the masses has limited the claimed accuracy. Preliminary mass determinations for each component are available from HST imaging, supported by ground-based astrometry and an excellent Hipparcos parallax; we use these for our preferred solution for the binary system. Other valu ...
Powerpoint for today
... Old idea: they form from a single large collapsing cloud of gas, like a star but on a much larger scale. New idea: observations indicate that "sub-galactic" fragments of size several hundred parsecs were the first things to form. Hundreds might merge to form a galaxy. ...
... Old idea: they form from a single large collapsing cloud of gas, like a star but on a much larger scale. New idea: observations indicate that "sub-galactic" fragments of size several hundred parsecs were the first things to form. Hundreds might merge to form a galaxy. ...
Document
... A mean-field Lagrangian is written for the interaction between many nucleons and its parameters are obtained empirically from comparison to the binding energies of ...
... A mean-field Lagrangian is written for the interaction between many nucleons and its parameters are obtained empirically from comparison to the binding energies of ...
Stellar Mass Assembly History
... km s-1. “…these bound pairs must evolve into E/S0 members by z = 0.7…most if not all, of its earlytype members evolved from (passive) galaxy-galaxy mergers at z < 1” ...
... km s-1. “…these bound pairs must evolve into E/S0 members by z = 0.7…most if not all, of its earlytype members evolved from (passive) galaxy-galaxy mergers at z < 1” ...
Population synthesis for double white dwarfs-II. Semi
... In Fig. 1 we show the limiting mass ratio for dynamically stable mass transfer (Eq. (4)) as the upper solid line, with ζ(m) derived from Eq. (5). The initial masstransfer rates, as given by Eq. (3), can be higher than the Eddington limit of the accretor (Tutukov & Yungelson 1979). The matter that ca ...
... In Fig. 1 we show the limiting mass ratio for dynamically stable mass transfer (Eq. (4)) as the upper solid line, with ζ(m) derived from Eq. (5). The initial masstransfer rates, as given by Eq. (3), can be higher than the Eddington limit of the accretor (Tutukov & Yungelson 1979). The matter that ca ...
Downloadable Full Text
... spectroscopic binary which has a likely white dwarf companion of mass Mwd 0.3 M and an orbital period of Porb 40.11 d (Gies et al. 2008; hereafter “the inner binary system”). Regulus itself has an inferred mass of ∼ 3.4 ± 0.2 M . This very bright star has been known for many years to have at l ...
... spectroscopic binary which has a likely white dwarf companion of mass Mwd 0.3 M and an orbital period of Porb 40.11 d (Gies et al. 2008; hereafter “the inner binary system”). Regulus itself has an inferred mass of ∼ 3.4 ± 0.2 M . This very bright star has been known for many years to have at l ...
ASTR 1101-001 Spring 2008 - Louisiana State University
... Masses obtained from Fig. 17-21 and Table 19-1 ...
... Masses obtained from Fig. 17-21 and Table 19-1 ...
26.3 Life Cycles of Stars
... Small nebulas produce small, cool stars that are long-lived. A star can have a mass as low as a tenth of the sun’s mass. The gravitational force in such low-mass stars is just strong enough to create a small core where nuclear fusion takes place. This lower energy production results in red stars, th ...
... Small nebulas produce small, cool stars that are long-lived. A star can have a mass as low as a tenth of the sun’s mass. The gravitational force in such low-mass stars is just strong enough to create a small core where nuclear fusion takes place. This lower energy production results in red stars, th ...
–1– 28. HIGH-MASS STAR FORMATION: THEORY 28.1. The Effects
... s−1 considered by Keto, this restricts the accretion rate to ṁ∗ . 3 × 10−5 M¯ yr−1 , smaller than the values he considers. (One can show that when one generalizes the Bondi accretion model to approximately include the self gravity of the gas, the accretion rate is indeed about c 3 /G.) Bonnell and ...
... s−1 considered by Keto, this restricts the accretion rate to ṁ∗ . 3 × 10−5 M¯ yr−1 , smaller than the values he considers. (One can show that when one generalizes the Bondi accretion model to approximately include the self gravity of the gas, the accretion rate is indeed about c 3 /G.) Bonnell and ...