Zinc and chromium abundances in a third
... The finding that the only two abundance measurements available at z < 1 are both well below solar – and quite typical of the sample at z > 1.5 – has caused concerns as to whether DLAs are really unbiased tracers of the chemical evolution history of the universe. Here we report measurements of the ab ...
... The finding that the only two abundance measurements available at z < 1 are both well below solar – and quite typical of the sample at z > 1.5 – has caused concerns as to whether DLAs are really unbiased tracers of the chemical evolution history of the universe. Here we report measurements of the ab ...
The 8190-A sodium doublet in cataclysmic variables
... the differences between them are easily discernible. Unfortunately, it is not possible for us to determine the exact binary phase of our observations because the high inaccuracies of the ephemeris found by Howell et al. (1988) are likely to yield incorrect eclipse times if extrapolated to 1991 (cf. ...
... the differences between them are easily discernible. Unfortunately, it is not possible for us to determine the exact binary phase of our observations because the high inaccuracies of the ephemeris found by Howell et al. (1988) are likely to yield incorrect eclipse times if extrapolated to 1991 (cf. ...
Magnetic collapse of a neutron gas: Can magnetars
... approach. These authors present several physical mechanisms for its origin in both extremely low and very high density systems, which may include astrophysical compact objects. In the case of highly dense systems, it was pointed out that “exotic” phase transitions could occur during gravitational co ...
... approach. These authors present several physical mechanisms for its origin in both extremely low and very high density systems, which may include astrophysical compact objects. In the case of highly dense systems, it was pointed out that “exotic” phase transitions could occur during gravitational co ...
JET FORMATION FROM MASSIVE YOUNG STARS
... 2.4. The Stellar and Disk Luminosity The massive young star produces a substantial luminosity, which is supposed to dynamically change the outflow structure. The dependence of the radiation force on stellar luminosity is parameterized by the Eddington ratio Γe , defined as the ratio of radiation for ...
... 2.4. The Stellar and Disk Luminosity The massive young star produces a substantial luminosity, which is supposed to dynamically change the outflow structure. The dependence of the radiation force on stellar luminosity is parameterized by the Eddington ratio Γe , defined as the ratio of radiation for ...
PS1-10jh: The Disruption of a Main-Sequence Star of Near
... less than 10−1 times as dense as the current peak density are derefined, but maximum refinement is maintained within 4rp at all times. For the q = 106 simulation, each refinement level is assigned to a single decade in ρ, using the star’s original central density ρc as a baseline, with the exception ...
... less than 10−1 times as dense as the current peak density are derefined, but maximum refinement is maintained within 4rp at all times. For the q = 106 simulation, each refinement level is assigned to a single decade in ρ, using the star’s original central density ρc as a baseline, with the exception ...
PDF
... above the threshold 关47兴. The layers change their topology and fold into a square lattice of parabolic focal conic domains 共PFCDs兲. The layers are in the form of Dupin cyclides for which the focal surfaces degenerate into 1D singularities, in this case a pair of parabolae that pass through each othe ...
... above the threshold 关47兴. The layers change their topology and fold into a square lattice of parabolic focal conic domains 共PFCDs兲. The layers are in the form of Dupin cyclides for which the focal surfaces degenerate into 1D singularities, in this case a pair of parabolae that pass through each othe ...
Global structure and kinematics of stellar haloes in cosmological
... spectrum). The value of σ8 is approximately 2-sigma higher than has been inferred from the most recent CMB data (Komatsu et al. 2009), which will affect the abundance of Milky Way-mass systems somewhat, but should not significantly affect their individual properties. The simulations were evolved fro ...
... spectrum). The value of σ8 is approximately 2-sigma higher than has been inferred from the most recent CMB data (Komatsu et al. 2009), which will affect the abundance of Milky Way-mass systems somewhat, but should not significantly affect their individual properties. The simulations were evolved fro ...
SN 2011dh and the progenitors of Type IIb supernovae Mattias Ergon
... 2011dh would later occur are obtained. Examining the position of the SN reveals an anonymous yellow star, seemingly similar to millions of other stars in this galaxy. However, beneath the surface, in the interior of the star, the situation is quite different, and a furious struggle between gravity a ...
... 2011dh would later occur are obtained. Examining the position of the SN reveals an anonymous yellow star, seemingly similar to millions of other stars in this galaxy. However, beneath the surface, in the interior of the star, the situation is quite different, and a furious struggle between gravity a ...
The importance of episodic accretion for low
... protostar. The disc becomes gravitationally unstable (first and second column) but fragmentation is damped by heating due to an accretion burst (third column); however, after this burst the disc cools sufficiently to undergo gravitational fragmentation; 2 low-mass stars form in the disc. ...
... protostar. The disc becomes gravitationally unstable (first and second column) but fragmentation is damped by heating due to an accretion burst (third column); however, after this burst the disc cools sufficiently to undergo gravitational fragmentation; 2 low-mass stars form in the disc. ...
Post Common Envelope Binaries from SDSS. I: 101 white dwarf
... variations. To answer this question, we first consider wide WDMS that did not undergo a CE phase, i.e. binaries with orbital periods of & years. For these systems, sub-spectra obtained over the course of several days will show no significant radial velocity variation, and combining them into a singl ...
... variations. To answer this question, we first consider wide WDMS that did not undergo a CE phase, i.e. binaries with orbital periods of & years. For these systems, sub-spectra obtained over the course of several days will show no significant radial velocity variation, and combining them into a singl ...
Dan Hooper - Indirect Searches For Particle Dark
... •The nature of this new physics is highly constrained by precision measurements of LEP Suggestive of an additional symmetry (R-parity, T-parity, KK-parity, etc.), naturally (or at least plausibly) leading to a stable new particle ...
... •The nature of this new physics is highly constrained by precision measurements of LEP Suggestive of an additional symmetry (R-parity, T-parity, KK-parity, etc.), naturally (or at least plausibly) leading to a stable new particle ...
AN ULTRA-DEEP NEAR-INFRARED SPECTRUM OF
... Several recent studies have shown that about half of the massive galaxies at z ∼ 2 are in a quiescent phase. Moreover, these galaxies are commonly found to be ultra-compact with half-light radii of ∼ 1 kpc. We have obtained a ∼ 29 hr spectrum of a typical quiescent, ultra-dense galaxy at z = 2.1865 ...
... Several recent studies have shown that about half of the massive galaxies at z ∼ 2 are in a quiescent phase. Moreover, these galaxies are commonly found to be ultra-compact with half-light radii of ∼ 1 kpc. We have obtained a ∼ 29 hr spectrum of a typical quiescent, ultra-dense galaxy at z = 2.1865 ...
The dual nature of the Milky Way stellar halo
... surrounded by a DM halo containing the major portion of the total galaxy mass and extending very far beyond the visible matter. Some indirect means suggest that the DM halo may extend as far as 170 kpc/h from the center of the galaxy. According to Carollo et al. (2007), the inner-halo component of t ...
... surrounded by a DM halo containing the major portion of the total galaxy mass and extending very far beyond the visible matter. Some indirect means suggest that the DM halo may extend as far as 170 kpc/h from the center of the galaxy. According to Carollo et al. (2007), the inner-halo component of t ...
Imaging and spectroscopy of ejected common envelopes
... shows that the nebular morphology exhibits an 'H' shape with the addition of fainter material forming a continuous loop. Suitable scaling shows that the central bar is split and resembles an ellipse. If we assume that this is in fact a circular structure inclined to our line ofsight and that it has ...
... shows that the nebular morphology exhibits an 'H' shape with the addition of fainter material forming a continuous loop. Suitable scaling shows that the central bar is split and resembles an ellipse. If we assume that this is in fact a circular structure inclined to our line ofsight and that it has ...
pdf-file - Max-Planck-Institut für Astronomie
... opacities also show some dependence on metallicity as well. In a regime where dust begins to sublimate and molecules start to form, there is a sharp decrease in the opacity. In this regime, the dependence of opacity on density is strong, unlike the opacity due to dust, and in general it is very diff ...
... opacities also show some dependence on metallicity as well. In a regime where dust begins to sublimate and molecules start to form, there is a sharp decrease in the opacity. In this regime, the dependence of opacity on density is strong, unlike the opacity due to dust, and in general it is very diff ...
The physics of star formation
... directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central importance in astrophysics to understand how stars form and what determines their properties. The ...
... directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central importance in astrophysics to understand how stars form and what determines their properties. The ...
The physics of star formation - Yale Astronomy
... directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central importance in astrophysics to understand how stars form and what determines their properties. The ...
... directly or indirectly, for most of what we see when we observe it. They also serve as our primary tracers of the structure and evolution of the universe and its contents. Consequently, it is of central importance in astrophysics to understand how stars form and what determines their properties. The ...
IGR J18483-0311: a new intermediate supergiant fast X
... X-ray transients (SFXTs, Negueruela et al. 2006). IGR J18483−0311 was discovered during observations performed with INTEGRAL in 2003 April 23-28 (Chernyakova et al. 2003), and it was found to have average fluxes of about 10 mCrab and 5 mCrab in the 15−40 keV and 40−100 keV bands, respectively. Molko ...
... X-ray transients (SFXTs, Negueruela et al. 2006). IGR J18483−0311 was discovered during observations performed with INTEGRAL in 2003 April 23-28 (Chernyakova et al. 2003), and it was found to have average fluxes of about 10 mCrab and 5 mCrab in the 15−40 keV and 40−100 keV bands, respectively. Molko ...
Microscopic vortex velocity in the inner crust and outer core of
... The physical state of the inner crust with its neutron rich nuclei and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is found to be somewhat larger than the outside dripped superfl ...
... The physical state of the inner crust with its neutron rich nuclei and dripped neutron superfluid interspersed with them is well established since the pioneering work of Negele & Vautherin (1973). The superfluid density inside a nucleus is found to be somewhat larger than the outside dripped superfl ...
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.