Runaway collisions in young star clusters – II. Numerical results
... with α = 2.35, M min = 0.2 M and M max = 120 M . For this stellar population, the average mass is M∗ 0.69 M . There is no initial mass segregation. To investigate the role of the initial concentration of the cluster, we consider King models with W0 = 3 or 8 (Binney & Tremaine 1987, Section 4 ...
... with α = 2.35, M min = 0.2 M and M max = 120 M . For this stellar population, the average mass is M∗ 0.69 M . There is no initial mass segregation. To investigate the role of the initial concentration of the cluster, we consider King models with W0 = 3 or 8 (Binney & Tremaine 1987, Section 4 ...
Carbon-enhanced metal-poor stars: a window on AGB
... stars catalogued in the SAGA observational database (Suda et al. 2008, 2011, last updated in January 2015) with iron abundance −2.8 ≤ [Fe/H] ≤ −1.8. Among these objects we select the stars ...
... stars catalogued in the SAGA observational database (Suda et al. 2008, 2011, last updated in January 2015) with iron abundance −2.8 ≤ [Fe/H] ≤ −1.8. Among these objects we select the stars ...
A re-examination of galactic conformity and a comparison with semi
... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
Farthest Neighbor: The Distant Milky Way Satellite Eridanus II
... et al. 2015; Koposov et al. 2015; Crnojević et al. 2016; see Table 1). Eri II is most likely located just beyond the virial radius of the Milky Way, which is typically estimated to be ∼300 kpc (Bland-Hawthorn & Gerhard 2016; Taylor et al. 2016). This places Eri II in a sharp transition region betwee ...
... et al. 2015; Koposov et al. 2015; Crnojević et al. 2016; see Table 1). Eri II is most likely located just beyond the virial radius of the Milky Way, which is typically estimated to be ∼300 kpc (Bland-Hawthorn & Gerhard 2016; Taylor et al. 2016). This places Eri II in a sharp transition region betwee ...
observations and theory of star cluster formation
... previously accepted boundaries. This result is consistent with the hierarchical clustering model. 4. Two Examples of Hierarchical Stellar Structure: Orion and W3. There are many observations of individual clusters that are part of a hierarchy on larger scales. The Orion region overall contains at le ...
... previously accepted boundaries. This result is consistent with the hierarchical clustering model. 4. Two Examples of Hierarchical Stellar Structure: Orion and W3. There are many observations of individual clusters that are part of a hierarchy on larger scales. The Orion region overall contains at le ...
Chapter 6 in the LSST Science Book
... proximity of the Galaxy. Until recently, it was held that the Clouds are captive satellites of the Galaxy and have made several passages through the Galaxy disk. The extended stream of HI, called the Magellanic Stream, which emanates from near the SMC and wraps around much of the sky, has been belie ...
... proximity of the Galaxy. Until recently, it was held that the Clouds are captive satellites of the Galaxy and have made several passages through the Galaxy disk. The extended stream of HI, called the Magellanic Stream, which emanates from near the SMC and wraps around much of the sky, has been belie ...
Abundances of the elements He to Ni in the atmosphere of Sirius A
... Aims. Among middle main sequence (A and B) stars, it is unusual to have abundance determinations for more than about a dozen of the 30 lightest chemical elements, largely because many elements do not have usefully strong spectral lines in the visible wavelength window usually used for abundance anal ...
... Aims. Among middle main sequence (A and B) stars, it is unusual to have abundance determinations for more than about a dozen of the 30 lightest chemical elements, largely because many elements do not have usefully strong spectral lines in the visible wavelength window usually used for abundance anal ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... 4.9.4. Why does Venus have a much thicker atmosphere than Earth? ...
... 4.9.4. Why does Venus have a much thicker atmosphere than Earth? ...
Transverse Beer-Can Distribution Electron Beam
... more precise instrument to explore and test the theory of QCD itself in the extent of many-body and other aspects. ...
... more precise instrument to explore and test the theory of QCD itself in the extent of many-body and other aspects. ...
YuHao_1
... Compared with storage ring accelerators, the ERL does not recirculate electron beam itself, only retrieve its energy. The electron beam does not have sufficient time to reach its equilibrium state due to synchrotron radiation and quantum excitation. Therefore, the electron beam quality mainly depend ...
... Compared with storage ring accelerators, the ERL does not recirculate electron beam itself, only retrieve its energy. The electron beam does not have sufficient time to reach its equilibrium state due to synchrotron radiation and quantum excitation. Therefore, the electron beam quality mainly depend ...
Carbon, nitrogen and oxygen abundances in
... velocity v sin i for 102 B stars. The v sin i values were found to range from 5 to 280 km s−1 ; such a large variation allowed us to analyse a relation between the helium abundances and rotational velocities. The used He I lines are strong in spectra of early and medium B stars, so their equivalent ...
... velocity v sin i for 102 B stars. The v sin i values were found to range from 5 to 280 km s−1 ; such a large variation allowed us to analyse a relation between the helium abundances and rotational velocities. The used He I lines are strong in spectra of early and medium B stars, so their equivalent ...
University of Groningen Photo-ionization studies of nebulae
... (AGB) and planetary nebulae (PNe) has gained much attention over the last decade. AGB stars lose mass fast and get obscured by their circumstellar dust. As the star leaves the AGB, its mass loss rate decreases significantly and the star may become sufficiently hot to ionize its circumstellar materia ...
... (AGB) and planetary nebulae (PNe) has gained much attention over the last decade. AGB stars lose mass fast and get obscured by their circumstellar dust. As the star leaves the AGB, its mass loss rate decreases significantly and the star may become sufficiently hot to ionize its circumstellar materia ...
SN 2006gy: DISCOVERY OF THE MOST LUMINOUS
... all (Smith & Owocki 2006), which would affect the range of initial masses that are subject to the pair instability in Population III stars. Because stars that begin their lives above 100 M are so few in number, their end fates are poorly constrained by observations (see Gal-Yam et al. 2007 for a re ...
... all (Smith & Owocki 2006), which would affect the range of initial masses that are subject to the pair instability in Population III stars. Because stars that begin their lives above 100 M are so few in number, their end fates are poorly constrained by observations (see Gal-Yam et al. 2007 for a re ...
Neutron Stars and the Determination of the Dense Matter Equation
... I have a particular thought for friends and colleagues of AstroMcGill. For more than two years now, we have shared our passion of astronomy with kids of all ages and adults alike. It was not always easy, but it was surely rewarding. Friends and colleagues, at McGill or those I met during conferences ...
... I have a particular thought for friends and colleagues of AstroMcGill. For more than two years now, we have shared our passion of astronomy with kids of all ages and adults alike. It was not always easy, but it was surely rewarding. Friends and colleagues, at McGill or those I met during conferences ...
Black Holes in Neutron Stars
... entrapment of dark matter particles. Dark matter was first postulated in 1933 and has since become a major field of research. Recent measurements of the Cosmic Microwave Background shows that dark matter may be ≥ 85% of all matter in the Universe. Given that dark matter does not interact with the el ...
... entrapment of dark matter particles. Dark matter was first postulated in 1933 and has since become a major field of research. Recent measurements of the Cosmic Microwave Background shows that dark matter may be ≥ 85% of all matter in the Universe. Given that dark matter does not interact with the el ...
Evolutionary and pulsational properties of white dwarf stars
... white dwarfs cool constitutes a fundamental issue and provides an independent cosmic clock to constrain the age and previous history of the Galactic populations including the disk (Winget et al. 1987; García-Berro et al. 1988a,b; Hernanz et al. 1994; Torres et al. 2002) and globular and open cluster ...
... white dwarfs cool constitutes a fundamental issue and provides an independent cosmic clock to constrain the age and previous history of the Galactic populations including the disk (Winget et al. 1987; García-Berro et al. 1988a,b; Hernanz et al. 1994; Torres et al. 2002) and globular and open cluster ...
A Detection Method for Small Kuiper Belt Objects: The Search for
... is estimated from 0.1 to 0.3 Earth mass (Jewitt and Luu 1995). Actually, the density of matter in the outer Solar System seems surprisingly low beyond Neptune, and the Kuiper disk could be much larger than the present observations suggest. If the Kuiper disk has a size distribution with such a const ...
... is estimated from 0.1 to 0.3 Earth mass (Jewitt and Luu 1995). Actually, the density of matter in the outer Solar System seems surprisingly low beyond Neptune, and the Kuiper disk could be much larger than the present observations suggest. If the Kuiper disk has a size distribution with such a const ...
Massive Star Formation - Max-Planck
... relatively ordered collapse via a central disk to form a single star or a small-N multiple. In this case, the pre-stellar core mass function has a similar form to the stellar initial mass function. In Competitive Accretion, the material that forms a massive star is drawn more chaotically from a wide ...
... relatively ordered collapse via a central disk to form a single star or a small-N multiple. In this case, the pre-stellar core mass function has a similar form to the stellar initial mass function. In Competitive Accretion, the material that forms a massive star is drawn more chaotically from a wide ...
EL CVn-type binaries - Discovery of 17 helium white dwarf
... do not undergo shell flashes is much longer than for those that do because their thick hydrogen envelopes can support residual p-p chain fusion for several Gyr. Maxted et al. (2013) found strong observational support for the assumption that He-WD are born with thick hydrogen envelopes. They found th ...
... do not undergo shell flashes is much longer than for those that do because their thick hydrogen envelopes can support residual p-p chain fusion for several Gyr. Maxted et al. (2013) found strong observational support for the assumption that He-WD are born with thick hydrogen envelopes. They found th ...
Using Weak Interaction to Probe Neutrons in Nuclei
... Using Weak Interaction to Probe Neutrons in Nuclei the Why and How Experimentally Robert Michaels ...
... Using Weak Interaction to Probe Neutrons in Nuclei the Why and How Experimentally Robert Michaels ...
The evolution of massive stars and their spectra
... and galaxies in the near and far Universe. They are among the most important sources of ionizing photons, energy, and some chemical species, which are ejected into the interstellar medium through powerful stellar winds and during their extraordinary deaths as supernovae (SN) and long gamma-ray burst ...
... and galaxies in the near and far Universe. They are among the most important sources of ionizing photons, energy, and some chemical species, which are ejected into the interstellar medium through powerful stellar winds and during their extraordinary deaths as supernovae (SN) and long gamma-ray burst ...
Black hole tidal problem in the Fermi normal coordinates
... where r denotes the orbital separation and µcrit is a constant ≈ 10–20 which depends on r/M , R/M , spin of the black hole, and equations of state (see Sec. V). If the condition (1) is satisfied outside a minimum orbital radius (e.g., r = 6GM/c2 for a star in a circular orbit around a Schwarzschild ...
... where r denotes the orbital separation and µcrit is a constant ≈ 10–20 which depends on r/M , R/M , spin of the black hole, and equations of state (see Sec. V). If the condition (1) is satisfied outside a minimum orbital radius (e.g., r = 6GM/c2 for a star in a circular orbit around a Schwarzschild ...
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.