INFRARED DUST BUBBLES: PROBING THE DETAILED
... 104 K. The outer thin shell of 104 K H+ gas is the region classically thought to represent the photoionized H ii region. This basic picture is supported by detailed numerical evolution models calculated for a 35 M (Freyer et al. 2006, hereafter FHY06), a 60 M ( Freyer et al. 2003), and an 85 M st ...
... 104 K. The outer thin shell of 104 K H+ gas is the region classically thought to represent the photoionized H ii region. This basic picture is supported by detailed numerical evolution models calculated for a 35 M (Freyer et al. 2006, hereafter FHY06), a 60 M ( Freyer et al. 2003), and an 85 M st ...
Munshi_washington_0250E_12611
... The primary focus of my thesis work is to study star formation using a series of high resolution cosmological N-body Simulations. Specifically, I have studied the total stellar-to-halo mass ratio as a function of halo mass for a new sample of simulated field galaxies using fully cosmological, LCDM, ...
... The primary focus of my thesis work is to study star formation using a series of high resolution cosmological N-body Simulations. Specifically, I have studied the total stellar-to-halo mass ratio as a function of halo mass for a new sample of simulated field galaxies using fully cosmological, LCDM, ...
The effect of dark matter capture on binary stars
... According to the WIMP model, stars in the galaxy travel through a background field of WIMPs that are constantly crossing the star. Some of these WIMPs collide with atomic nuclei inside stars via the weak force interaction. The ones that lose sufficient kinetic energy become bound to the star. Captur ...
... According to the WIMP model, stars in the galaxy travel through a background field of WIMPs that are constantly crossing the star. Some of these WIMPs collide with atomic nuclei inside stars via the weak force interaction. The ones that lose sufficient kinetic energy become bound to the star. Captur ...
The similarity of the stellar mass fractions of galaxy groups and
... stellar masses are measured within an aperture that is determined by the estimated total mass (e.g., r500 ), rather than within a fixed physical aperture (e.g., 1 Mpc). In the present study, we revisit the stellar mass fractions of groups and clusters but using a somewhat different approach. In part ...
... stellar masses are measured within an aperture that is determined by the estimated total mass (e.g., r500 ), rather than within a fixed physical aperture (e.g., 1 Mpc). In the present study, we revisit the stellar mass fractions of groups and clusters but using a somewhat different approach. In part ...
REVIEW Early star-forming galaxies and the reionization of the Universe
... (Figure panel a: circles with 1-s.d. error bars40,41,62,86,87; grey points indicate the contribution from Lya-emitting galaxies65). Also shown are illustrative model star formation histories for typical stellar ages of 108 yr, which are consistent with these observations (green area) and are based o ...
... (Figure panel a: circles with 1-s.d. error bars40,41,62,86,87; grey points indicate the contribution from Lya-emitting galaxies65). Also shown are illustrative model star formation histories for typical stellar ages of 108 yr, which are consistent with these observations (green area) and are based o ...
EXTREMELY EXTENDED DUST SHELLS AROUND EVOLVED
... 8.2 Basic observed parameters (distance, luminosity, pulsation period, mass loss rates and expansion velocities) for six target oxygen-rich intermediatemass stars found in literature that were used in calculations. . . . . . 177 8.3 Target evolved oxygen-rich intermediate-mass stars imaged by Infra ...
... 8.2 Basic observed parameters (distance, luminosity, pulsation period, mass loss rates and expansion velocities) for six target oxygen-rich intermediatemass stars found in literature that were used in calculations. . . . . . 177 8.3 Target evolved oxygen-rich intermediate-mass stars imaged by Infra ...
Deformations of Accreting Neutron Star Crusts and Gravitational
... an alternate scenario, Bildsten (1998a) suggested that these stars are rotating fast enough so that appreciable angular momentum is radiated away as gravitational waves (GW), allowing an equilibrium where the angular momentum added by accretion is lost to gravitational radiation. Equilibria via grav ...
... an alternate scenario, Bildsten (1998a) suggested that these stars are rotating fast enough so that appreciable angular momentum is radiated away as gravitational waves (GW), allowing an equilibrium where the angular momentum added by accretion is lost to gravitational radiation. Equilibria via grav ...
Decoding Galaxy Evolution with Gas
... principal component decomposition of relative abundances [X/Fe]—to this sample to characterize its distribution in the 12-dimensional space defined by their elemental abundances. The first principal component PC1, which describes the abundance patterns of most stars in the sample, shows a strong cont ...
... principal component decomposition of relative abundances [X/Fe]—to this sample to characterize its distribution in the 12-dimensional space defined by their elemental abundances. The first principal component PC1, which describes the abundance patterns of most stars in the sample, shows a strong cont ...
Invited Review The Beginning and Evolution of the Universe
... well as review articles. We begin with discussion of the foundations of the Big Bang Model in § 2, which summarizes research in the half century from Einstein’s foundational paper on modern cosmology until the late 1960s discovery of the CMB radiation, as well as some loose ends. Section 3 discusses ...
... well as review articles. We begin with discussion of the foundations of the Big Bang Model in § 2, which summarizes research in the half century from Einstein’s foundational paper on modern cosmology until the late 1960s discovery of the CMB radiation, as well as some loose ends. Section 3 discusses ...
Stellar activity in exoplanet hosts Enrique Herrero Casas
... stars for a targeted transit search was presented. A search within this subset would have an expected rate of findings increased in a factor of 2 o 3 with respect to a search on the initial sample (Herrero et al. 2012). The high precision photometry provided by the space missions Kepler and CoRoT has ...
... stars for a targeted transit search was presented. A search within this subset would have an expected rate of findings increased in a factor of 2 o 3 with respect to a search on the initial sample (Herrero et al. 2012). The high precision photometry provided by the space missions Kepler and CoRoT has ...
Environmental dependence of bulge
... Our team has actively explored the structural properties of earlytype galaxies at both low and high redshifts. We here summarize some of our previous empirical results relevant to this work. In Bernardi et al. (2012) we quantified the systematics in the size– luminosity relation of galaxies in the S ...
... Our team has actively explored the structural properties of earlytype galaxies at both low and high redshifts. We here summarize some of our previous empirical results relevant to this work. In Bernardi et al. (2012) we quantified the systematics in the size– luminosity relation of galaxies in the S ...
The Nuclear Equation of State and Neutron Star Masses
... nd /d n = + p. Beginning from the center, where m = r = 0, p = p c , and ε = εc , these equations are integrated to the surface, where p = p surf = 0, r = R, and m = M. For hadronic EOSs, εsurf = 0, but this is not the case for pure strange quark matter (SQM) stars, for which the energy density r ...
... nd /d n = + p. Beginning from the center, where m = r = 0, p = p c , and ε = εc , these equations are integrated to the surface, where p = p surf = 0, r = R, and m = M. For hadronic EOSs, εsurf = 0, but this is not the case for pure strange quark matter (SQM) stars, for which the energy density r ...
Population synthesis for double white dwarfs. I. Close - UvA-DARE
... a spiral-in, and that the change in orbital separation is governed by conservation of angular momentum (the equation used is given in Appendix A.2.3). We parametrise the loss of angular momentum from the binary with a factor γ. If the mass ratio is more extreme, the common envelope leads to a spiral ...
... a spiral-in, and that the change in orbital separation is governed by conservation of angular momentum (the equation used is given in Appendix A.2.3). We parametrise the loss of angular momentum from the binary with a factor γ. If the mass ratio is more extreme, the common envelope leads to a spiral ...
- UCL Discovery
... the plasma pressure within the strong field region must decrease. The high thermal conductivity of the convection zone means that any temperature difference between the strong and weak magnetic field regions is soon equalised. This, in turn, means that the reduced plasma pressure must be associated ...
... the plasma pressure within the strong field region must decrease. The high thermal conductivity of the convection zone means that any temperature difference between the strong and weak magnetic field regions is soon equalised. This, in turn, means that the reduced plasma pressure must be associated ...
Massive Star Formation - Max-Planck
... fields, and MA = 3(σ/vA ) is the Alfvén Mach number. A magnetized cloud with the same total pressure and surface density as a non-magnetic cloud will therefore have a virial parameter that is smaller by a factor φB . Clouds that are observed to have small αvir (e.g., Pillai et al., 2011; see also § ...
... fields, and MA = 3(σ/vA ) is the Alfvén Mach number. A magnetized cloud with the same total pressure and surface density as a non-magnetic cloud will therefore have a virial parameter that is smaller by a factor φB . Clouds that are observed to have small αvir (e.g., Pillai et al., 2011; see also § ...
edmund c. stoner and the discovery of the maximum mass of white
... density approximation, by substituting for the internal energy density Fowler’s nonrelativistic equation of state for a degenerate electron gas.12 In particular, he found that the density increases with the square of the mass of the star.13 In such a gas the mean momentum of an electron is proportio ...
... density approximation, by substituting for the internal energy density Fowler’s nonrelativistic equation of state for a degenerate electron gas.12 In particular, he found that the density increases with the square of the mass of the star.13 In such a gas the mean momentum of an electron is proportio ...