Synthesis, Characterization, and pH-Dependent
... excess of protons whose spins are aligned with the magnetic field provides the measurable net magnetization seen in an MRI sample. Once the spins have reached this equilibrium state, a radiofrequency (RF) pulse, at the Larmor frequency, is applied. For example, one can imagine an RF pulse strong en ...
... excess of protons whose spins are aligned with the magnetic field provides the measurable net magnetization seen in an MRI sample. Once the spins have reached this equilibrium state, a radiofrequency (RF) pulse, at the Larmor frequency, is applied. For example, one can imagine an RF pulse strong en ...
Particle Accelerators and Detectors for medical
... the Bragg dose distribution produced by accelerated ions. Since then, a remarkable scientific and technological development transformed Wilson’s vision into reality and hadrontherapy can be considered nowadays an established clinical practice and a challenging field of research in full evolution [22 ...
... the Bragg dose distribution produced by accelerated ions. Since then, a remarkable scientific and technological development transformed Wilson’s vision into reality and hadrontherapy can be considered nowadays an established clinical practice and a challenging field of research in full evolution [22 ...
Yellow supergiants as supernova progenitors: an indication of
... the most popular mass-loss prescriptions for the RSG phase is given by de Jager et al. (1988), and has been confirmed observationally (Crowther 2001; Mauron & Josselin 2011). On the other hand, some authors claim that the mass-loss rates during the RSG phase could have been underestimated (van Loon ...
... the most popular mass-loss prescriptions for the RSG phase is given by de Jager et al. (1988), and has been confirmed observationally (Crowther 2001; Mauron & Josselin 2011). On the other hand, some authors claim that the mass-loss rates during the RSG phase could have been underestimated (van Loon ...
Radiative Precession of an Isolated Neutron Star
... Note that the combined elasto-hydromagnetic deformation is triaxial in general. Biaxiality (ǫ′ = 0) is a good approximation only when one has ǫcr ≪ ǫmag (or else ǫcr ≫ ǫmag ) and the internal magnetic field (or crust) is symmetric about a unique axis. Equations (11), (13) and (14) reveal that, as a ...
... Note that the combined elasto-hydromagnetic deformation is triaxial in general. Biaxiality (ǫ′ = 0) is a good approximation only when one has ǫcr ≪ ǫmag (or else ǫcr ≫ ǫmag ) and the internal magnetic field (or crust) is symmetric about a unique axis. Equations (11), (13) and (14) reveal that, as a ...
On the onset of runaway stellar collisions in dense star clusters I
... They also found that collisions occur every few ten thousand years, which is roughly the time required for a collision product to reach the main-sequence. Stellar collisions also play an important role in the formation of stellar exotica in young star clusters, such as blue stragglers. If cluster pr ...
... They also found that collisions occur every few ten thousand years, which is roughly the time required for a collision product to reach the main-sequence. Stellar collisions also play an important role in the formation of stellar exotica in young star clusters, such as blue stragglers. If cluster pr ...
NEUTRINOS AND DARK MATTER IN NUCLEAR PHYSICS (NDM15)
... physics and it is of utmost importance to allow people working at the intersections of these fields to meet every now and then to exchange ideas and results. The NDM Symposium series is practically the only large venue dedicated to the discussion of connections of nuclear-structure physics to fundam ...
... physics and it is of utmost importance to allow people working at the intersections of these fields to meet every now and then to exchange ideas and results. The NDM Symposium series is practically the only large venue dedicated to the discussion of connections of nuclear-structure physics to fundam ...
Presentazione di PowerPoint
... Indeed, normal hydrogen burning stars, in the stellar core or in a shell typically behave as canonical stellar evolution models predict. And we have CMDs which are a clear evidence that globular clusters are typically populated by stars with homogeneous composition and born at the same time. ...
... Indeed, normal hydrogen burning stars, in the stellar core or in a shell typically behave as canonical stellar evolution models predict. And we have CMDs which are a clear evidence that globular clusters are typically populated by stars with homogeneous composition and born at the same time. ...
The Age and Stellar Parameters of the Procyon Binary System
... themselves out of this “iron box”. Atmospheres with realistic trace adundances, obtained from fitting the spectrum and the 1,800–10,000Å spectral energy distribution were employed to obtain Teff = 7,740±50 K. They now estimated the radius to be 0.01234±0.00032 R⊙ , consistent with a carbon-oxygen i ...
... themselves out of this “iron box”. Atmospheres with realistic trace adundances, obtained from fitting the spectrum and the 1,800–10,000Å spectral energy distribution were employed to obtain Teff = 7,740±50 K. They now estimated the radius to be 0.01234±0.00032 R⊙ , consistent with a carbon-oxygen i ...
Pulsations in White Dwarfs
... of post-AGB objects; He-C-O in roughly comparable proportions) Low-degree (1,2), low- to mid-order g-mode pulsators Opacity-driven (classical kappa-mechanism) due to opaque high ions of C and O in the envelope ...
... of post-AGB objects; He-C-O in roughly comparable proportions) Low-degree (1,2), low- to mid-order g-mode pulsators Opacity-driven (classical kappa-mechanism) due to opaque high ions of C and O in the envelope ...
Self-similarity in the chemical evolution of galaxies and the delay
... lifetimes etc. All of these are described in detail in Y13. The only parameter that we treat as a variable in the present contribution is the delay time distribution (DTD) of SNeIa. The DTD describes the probability for a SN Ia to explode as a function of the time elapsed since a star formation even ...
... lifetimes etc. All of these are described in detail in Y13. The only parameter that we treat as a variable in the present contribution is the delay time distribution (DTD) of SNeIa. The DTD describes the probability for a SN Ia to explode as a function of the time elapsed since a star formation even ...
The AG Carinae nebula: abundant evidence for a red supergiant
... abundances are derived for five regions across the nebula from high spatial resolution spectroscopy obtained at the Anglo-Australian Telescope (AAT). We derive an average Te of 6350 ± 400 K, an ne of 820 ± 170 cm-3, and find that nitrogen (N) is enhanced by a factor of 4.5 ± 1.3 and that oxygen (0) ...
... abundances are derived for five regions across the nebula from high spatial resolution spectroscopy obtained at the Anglo-Australian Telescope (AAT). We derive an average Te of 6350 ± 400 K, an ne of 820 ± 170 cm-3, and find that nitrogen (N) is enhanced by a factor of 4.5 ± 1.3 and that oxygen (0) ...
Document
... degrees (solid line), 82 degrees (dotted line) and 90 degrees (dash-dotted line). In the last case the contribution of both hemispheres was taken into account, in the first two cases it wasn’t necessary. ...
... degrees (solid line), 82 degrees (dotted line) and 90 degrees (dash-dotted line). In the last case the contribution of both hemispheres was taken into account, in the first two cases it wasn’t necessary. ...
Can Planets survive Stellar Evolution?
... maximum planet mass that can be evaporated inside an AGB envelope can be obtained by equating the location of the evaporation region (where the local sound speed in the stellar envelope matches the escape velocity from the planet’s surface) to the energy required to expel the envelope (Soker 1996, 1 ...
... maximum planet mass that can be evaporated inside an AGB envelope can be obtained by equating the location of the evaporation region (where the local sound speed in the stellar envelope matches the escape velocity from the planet’s surface) to the energy required to expel the envelope (Soker 1996, 1 ...
MAX-PLANCK-INSTITUT FÜR GRAVITATIONSPHYSIK
... Gravitational waves were first predicted by Einstein in 1916 as a consequence of his general theory of relativity, but have not yet been directly detected. Einstein@Home was developed as part of the World Year of Physics 2005 activities of the American Physical Society. For the past five years, Eins ...
... Gravitational waves were first predicted by Einstein in 1916 as a consequence of his general theory of relativity, but have not yet been directly detected. Einstein@Home was developed as part of the World Year of Physics 2005 activities of the American Physical Society. For the past five years, Eins ...
Surface temperature distribution and absorption features in Isolated
... According to magnetic-dipole braking model [5], neutron stars rotate in vacuum at angular velocity Ω and possesses a magnetic dipole moment m forming an angle α with the rotation axis. The rotation is assumed to be sufficiently slow that non-spherical distortions can be ignored to lowest order. Inde ...
... According to magnetic-dipole braking model [5], neutron stars rotate in vacuum at angular velocity Ω and possesses a magnetic dipole moment m forming an angle α with the rotation axis. The rotation is assumed to be sufficiently slow that non-spherical distortions can be ignored to lowest order. Inde ...
Massive quiescent galaxies at cosmic noon Robert Feldmann UC Berkeley
... Massive at Cosmic Noon and dynamica galaxies over the past 10 Gyr. The uncerta rown in size by a factor of ALMA: 870μm + CO Extreme Star-bursts (SMGs) was determined from simulations~1.4that i rs (10 Gyr). A key test of Gyr and template mismatch. However, w ellarHighest kinematics of• one form of st ...
... Massive at Cosmic Noon and dynamica galaxies over the past 10 Gyr. The uncerta rown in size by a factor of ALMA: 870μm + CO Extreme Star-bursts (SMGs) was determined from simulations~1.4that i rs (10 Gyr). A key test of Gyr and template mismatch. However, w ellarHighest kinematics of• one form of st ...
Confronting predictions of the galaxy stellar mass function with
... increasing by 0.6 dex from z = 10 to 5. It is also interesting to note from Fig. 2 that it appears the intrinsic UV luminosity of galaxies with L1500 > 1028 erg s−1 h−1 can alone be used to estimate the stellar mass with an accuracy of ≈50 per cent. This contrasts sharply with the low-redshift Unive ...
... increasing by 0.6 dex from z = 10 to 5. It is also interesting to note from Fig. 2 that it appears the intrinsic UV luminosity of galaxies with L1500 > 1028 erg s−1 h−1 can alone be used to estimate the stellar mass with an accuracy of ≈50 per cent. This contrasts sharply with the low-redshift Unive ...
Star Formation in Disks: Spiral Arms, Turbulence, and Triggering
... energy is much denser, several hundred eV cm−3 . Of the first four, only supersonic turbulence has been associated with star formation triggering because such turbulence can compress the gas a lot. Thermal instabilities compress the gas too, but usually in small regions where self-gravity is not impo ...
... energy is much denser, several hundred eV cm−3 . Of the first four, only supersonic turbulence has been associated with star formation triggering because such turbulence can compress the gas a lot. Thermal instabilities compress the gas too, but usually in small regions where self-gravity is not impo ...
Chapter 2 Simulation Methodology 2.1 The generation of cosmological initial conditions
... resources, particularly when the grids are further refined with adaptive mesh only in the most highly refined subvolume. See Figure 2.1 for an example. An example of the overall cost savings can be shown very simply. Let us assume that the situation is as described for the simulation discussed above ...
... resources, particularly when the grids are further refined with adaptive mesh only in the most highly refined subvolume. See Figure 2.1 for an example. An example of the overall cost savings can be shown very simply. Let us assume that the situation is as described for the simulation discussed above ...
Spectroscopic Variability of Supergiant Star HD14134, B3Ia
... 1 and 2). In these same spectra, all the other lines typical for hot supergiants such as HD14134, apart from Hα, are observed, including Hβ. In order to investigate the short term variability in the Hα profile, all individual spectra obtained on December 29-30, 2013, and on February 13, 15, 2016 were ...
... 1 and 2). In these same spectra, all the other lines typical for hot supergiants such as HD14134, apart from Hα, are observed, including Hβ. In order to investigate the short term variability in the Hα profile, all individual spectra obtained on December 29-30, 2013, and on February 13, 15, 2016 were ...
asteroseismological study of massive zz ceti stars with
... mass right before the first thermal pulse. Althaus et al. (2010a) demonstrated that, depending on the stellar mass of the white dwarf, the central oxygen abundances can be underestimated up to a ∼15% if the white dwarf mass is taken as the mass of the hydrogen-free core at the first thermal pulse. L ...
... mass right before the first thermal pulse. Althaus et al. (2010a) demonstrated that, depending on the stellar mass of the white dwarf, the central oxygen abundances can be underestimated up to a ∼15% if the white dwarf mass is taken as the mass of the hydrogen-free core at the first thermal pulse. L ...
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.