Astronomy Astrophysics Astrophysical parameters and orbital solution of the peculiar X-ray
... In SGXBs the optical companion is an OB supergiant. Supergiant stars are known to suffer great mass loss in the form of a radiation-driven stellar wind (Kudritzki & Puls 2000). The compact star interacts with this wind, producing the persistent X-rays observed in SGXBs (with typically LX ∼ 1036 erg s ...
... In SGXBs the optical companion is an OB supergiant. Supergiant stars are known to suffer great mass loss in the form of a radiation-driven stellar wind (Kudritzki & Puls 2000). The compact star interacts with this wind, producing the persistent X-rays observed in SGXBs (with typically LX ∼ 1036 erg s ...
0004-637X 778 2 119
... upper limit to the strength of the dipole field. If the neutron star is evolving with an active fallback disk, the dipole field strength that can produce the properties of this source could be in the (1–2) × 1012 G range on the surface of the neutron star (Alpar et al. 2011). These results clearly s ...
... upper limit to the strength of the dipole field. If the neutron star is evolving with an active fallback disk, the dipole field strength that can produce the properties of this source could be in the (1–2) × 1012 G range on the surface of the neutron star (Alpar et al. 2011). These results clearly s ...
Stellar Population Effects on the Inferred Photon Density at
... reliably estimated. However difficulties arise when any of these properties are unknown. A young starburst will contain a larger proportion of hot, massive stars than an older one and so emit more ionizing photons for a given 1500Å continuum measurement. By contrast, a stellar population that has for ...
... reliably estimated. However difficulties arise when any of these properties are unknown. A young starburst will contain a larger proportion of hot, massive stars than an older one and so emit more ionizing photons for a given 1500Å continuum measurement. By contrast, a stellar population that has for ...
Radioactive decay data: powerful aids in medical
... transition/emission probabilities and transition type (also EC/β + ratios when appropriate); γ -ray energies, emission probabilities and internal conversion coefficients (also internal-pair formation coefficients for β + β − when appropriate); Auger- and conversion-electron energies and emission pro ...
... transition/emission probabilities and transition type (also EC/β + ratios when appropriate); γ -ray energies, emission probabilities and internal conversion coefficients (also internal-pair formation coefficients for β + β − when appropriate); Auger- and conversion-electron energies and emission pro ...
Orbital period decay of compact black hole X
... greater than 0.00035, the mass transfer becomes dynamically unstable. If we take δ = 0.000345, the calculated evolution of the BHXB is in agreement with the observations. For the other result δ ≤ 0.00034, the efficiency of circumbinary disk the extracting angular momentum is relatively low and the fin ...
... greater than 0.00035, the mass transfer becomes dynamically unstable. If we take δ = 0.000345, the calculated evolution of the BHXB is in agreement with the observations. For the other result δ ≤ 0.00034, the efficiency of circumbinary disk the extracting angular momentum is relatively low and the fin ...
Metallicity, Age, and Mass of Star Forming Galaxies at z~3
... HDF images as red sources. There are no such galaxies. But we do see z>4 LBGs. Where are they at Z~3? Recurrent SF? Just bad luck in The HDF? ...
... HDF images as red sources. There are no such galaxies. But we do see z>4 LBGs. Where are they at Z~3? Recurrent SF? Just bad luck in The HDF? ...
Gamma-Ray Bursts and Puzzles of Core
... results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) by Fernández et al. (1999). Circles denote the GRB host galaxies with the BTA photometry, asterisks are results by other authors (HST, VLT). For the galaxy GRB 991208 first measurement of z = 0.706 and R ...
... results of the photometric measurement of z applied to galaxies from the Hubble Deep Field (HDF) by Fernández et al. (1999). Circles denote the GRB host galaxies with the BTA photometry, asterisks are results by other authors (HST, VLT). For the galaxy GRB 991208 first measurement of z = 0.706 and R ...
Giant molecular clouds: star factories
... lead to much higher know how these clouds are whole galaxy, however, other star formation dispersed, or destroyed. The simulations do not explicitly rates gas in GMCs could all be turned model the dark matter halo and into stars, but this would lead to stars. Rather, these are assumed to much higher ...
... lead to much higher know how these clouds are whole galaxy, however, other star formation dispersed, or destroyed. The simulations do not explicitly rates gas in GMCs could all be turned model the dark matter halo and into stars, but this would lead to stars. Rather, these are assumed to much higher ...
A New Measurement of the Fusion Reaction 14N(p,γ)
... Stars create the light we observe from energy liberated by nuclear fusion reactions. For most of their lives, stars exist as main-sequence objects quiescently burning hydrogen. At temperatures present in stars slightly larger than the Sun, the CN cycle dominates hydrogen burning and thus a star’s ma ...
... Stars create the light we observe from energy liberated by nuclear fusion reactions. For most of their lives, stars exist as main-sequence objects quiescently burning hydrogen. At temperatures present in stars slightly larger than the Sun, the CN cycle dominates hydrogen burning and thus a star’s ma ...
The white dwarf population within 40 pc of the Sun
... evolution of white dwarfs is determined by a simple gravothermal process. However, although the basic picture of white dwarf evolution has remained unchanged for some time, we now have very reliable and accurate evolutionary tracks, which take into account all the relevant physical processes involve ...
... evolution of white dwarfs is determined by a simple gravothermal process. However, although the basic picture of white dwarf evolution has remained unchanged for some time, we now have very reliable and accurate evolutionary tracks, which take into account all the relevant physical processes involve ...
The white dwarf population within 40 pc of the Sun
... decades now that the evolution of white dwarfs is determined by a simple gravothermal process. However, although the basic picture of white dwarf evolution has remained unchanged for some time, we now have very reliable and accurate evolutionary tracks, which take into account all the relevant physi ...
... decades now that the evolution of white dwarfs is determined by a simple gravothermal process. However, although the basic picture of white dwarf evolution has remained unchanged for some time, we now have very reliable and accurate evolutionary tracks, which take into account all the relevant physi ...
The white dwarf population within 40 pc of the Sun
... the number of synthetic white dwarfs increases smoothly for increasing magnitudes up to Mbol ≈ 15.0, and that for magnitudes larger than this value there is a dramatic drop in the white dwarf number counts. Furthermore, for distances of ∼ 40 pc the observational magnitude cut will eliminate all whit ...
... the number of synthetic white dwarfs increases smoothly for increasing magnitudes up to Mbol ≈ 15.0, and that for magnitudes larger than this value there is a dramatic drop in the white dwarf number counts. Furthermore, for distances of ∼ 40 pc the observational magnitude cut will eliminate all whit ...
An evolutionary channel towards the accreting millisecond pulsar
... Table 1 summarizes the calculated results when the magnetic braking cut-off is included. In the case that initial orbital period is Porb,i = 2.2 d, a low mass-transfer rate (less than Ṁcr ) due to the sudden stop of magnetic braking would result in an accretion-disc instability. The subsequent evap ...
... Table 1 summarizes the calculated results when the magnetic braking cut-off is included. In the case that initial orbital period is Porb,i = 2.2 d, a low mass-transfer rate (less than Ṁcr ) due to the sudden stop of magnetic braking would result in an accretion-disc instability. The subsequent evap ...
... triple system found among PNe). The two mainsequence companions have masses of 0.85 and 0.1M⊙ (Adam & Mugrauer 2014). The central star is evolving erratically, possibly due to the recovery from a symbiotic outburst 20 years ago. Hajduk et al. (2014a) searched for PN central stars binaries in the SMC ...
What powers luminous infrared galaxies?
... The line ratio in most sources including the two ULIRGs is reasonably well fit by effective temperatures near 42,000 K. The Galactic center (here we used ne 3000 and log(U)=-1) lies at the cool end of the distribution, a fact that is very likely explained by the ageing effects of its most recent s ...
... The line ratio in most sources including the two ULIRGs is reasonably well fit by effective temperatures near 42,000 K. The Galactic center (here we used ne 3000 and log(U)=-1) lies at the cool end of the distribution, a fact that is very likely explained by the ageing effects of its most recent s ...
Chapter 5 - Leiden Observatory
... Tutukov, 1984]. In the SD scenario, a CO WD explodes as an SNIa if its mass approaches Mch through accretion from a non-degenerate companion. In the DD scenario, two CO WDs can produce an SN Ia while merging if their combined mass is larger than Mch . However, observationally as well as theoreticall ...
... Tutukov, 1984]. In the SD scenario, a CO WD explodes as an SNIa if its mass approaches Mch through accretion from a non-degenerate companion. In the DD scenario, two CO WDs can produce an SN Ia while merging if their combined mass is larger than Mch . However, observationally as well as theoreticall ...
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.