Chemical evolution models for the dwarf spheroidal galaxies Leo 1
... but in different fractions. Leo 2 formed the majority of its stars ∼7–14 Gyr ago, whereas the major episode of star formation in Leo 1 occurred between 1–7 Gyr ago with a minor fraction of stars being formed before ∼10 Gyr ago. In this work we adopt detailed chemical evolution models with the aim to ...
... but in different fractions. Leo 2 formed the majority of its stars ∼7–14 Gyr ago, whereas the major episode of star formation in Leo 1 occurred between 1–7 Gyr ago with a minor fraction of stars being formed before ∼10 Gyr ago. In this work we adopt detailed chemical evolution models with the aim to ...
wing galaxies: a formation mechanism of the clumpy irregular galaxy
... We made two kinds of numerical simulations for Mrk 297. ...
... We made two kinds of numerical simulations for Mrk 297. ...
Barium Stars: Theoretical Interpretation
... (TDU) episodes, mixing with the envelope C-rich and s-process-rich material synthesised in the He intershell (the zone between H shell and He shell). The most likely interpretation of barium stars is that they acquired the senrichment by mass transfer in a binary system through stellar winds from an ...
... (TDU) episodes, mixing with the envelope C-rich and s-process-rich material synthesised in the He intershell (the zone between H shell and He shell). The most likely interpretation of barium stars is that they acquired the senrichment by mass transfer in a binary system through stellar winds from an ...
Neutron stars as probes of extreme energy density matter
... In old and cold neutron stars, matter is in weak-interaction equilibrium and charge neutral. It suffices to choose two independent chemical potentials μn and μe to characterize the prevalent conditions (neutrinos with their long mean free paths leave the star; when trapped, their chemical potentials ...
... In old and cold neutron stars, matter is in weak-interaction equilibrium and charge neutral. It suffices to choose two independent chemical potentials μn and μe to characterize the prevalent conditions (neutrinos with their long mean free paths leave the star; when trapped, their chemical potentials ...
Non-radiative inelastic processes in lithium-helium ion
... excitation/de-excitation processes are based on non-adiabatic transitions within the 1 Σ+ and 3 Σ+ systems. Finally, it should be emphasized that the LZ model might provide less accurate transition probabilities for non-adiabatic regions with large adiabatic splittings or for cases when other quantu ...
... excitation/de-excitation processes are based on non-adiabatic transitions within the 1 Σ+ and 3 Σ+ systems. Finally, it should be emphasized that the LZ model might provide less accurate transition probabilities for non-adiabatic regions with large adiabatic splittings or for cases when other quantu ...
Chapter 5 - Leiden Observatory
... Zwart & Yungelson, 1998]. Following mass transfer in a binary, the donor may turn into a helium-burning star without hydrogen envelope. When the mass transfer leads to a merger between the binary stars, we estimate the resulting stellar product and follow the evolution further. Note that we do not s ...
... Zwart & Yungelson, 1998]. Following mass transfer in a binary, the donor may turn into a helium-burning star without hydrogen envelope. When the mass transfer leads to a merger between the binary stars, we estimate the resulting stellar product and follow the evolution further. Note that we do not s ...
Neutron Stars – Cooling and Transport
... where F is the heat flux density, H is the heating power per unit volume, cv is specific heat (Sects. 2.5, 3.2, and 4.2), Qν is neutrino emissivity (Sects. 2.6, 3.3, 4.3), κ̂ is the thermal conductivity tensor (Sects. 2.7, 3.4, and 4.4), and ∇ = (e−Λ (r) ∂ /∂ r, r−1 ∂ /∂ θ , (r sin θ )−1 ∂ /∂ ϕ ) in ...
... where F is the heat flux density, H is the heating power per unit volume, cv is specific heat (Sects. 2.5, 3.2, and 4.2), Qν is neutrino emissivity (Sects. 2.6, 3.3, 4.3), κ̂ is the thermal conductivity tensor (Sects. 2.7, 3.4, and 4.4), and ∇ = (e−Λ (r) ∂ /∂ r, r−1 ∂ /∂ θ , (r sin θ )−1 ∂ /∂ ϕ ) in ...
Geosystems, 7e (Christopherson) Chapter 2 Solar Energy to Earth
... D) The wavelength generated is directly proportional to the temperature of the emitter; i.e., as temperature of the emitting object increases, the wavelength also increases. E) The hotter an object, the more energy it emits at all wavelengths. Answer: D Diff: 3 ...
... D) The wavelength generated is directly proportional to the temperature of the emitter; i.e., as temperature of the emitting object increases, the wavelength also increases. E) The hotter an object, the more energy it emits at all wavelengths. Answer: D Diff: 3 ...
YEAR - University of Maryland Astronomy
... X-Rays and Gamma Rays on the Sun The Problem with Mars Fasten Your Seatbelts! The Bumpy Ride to Star Formation Looking at Other Wavelengths: A Survey of Astronomy Observatories from Radio to Gamma Rays Gravity, From Here to Eternity Have you seen the Milky Way? Building the Universe at the National ...
... X-Rays and Gamma Rays on the Sun The Problem with Mars Fasten Your Seatbelts! The Bumpy Ride to Star Formation Looking at Other Wavelengths: A Survey of Astronomy Observatories from Radio to Gamma Rays Gravity, From Here to Eternity Have you seen the Milky Way? Building the Universe at the National ...
in chiral mean
... Non strange partners revisited N(1710) is not seen anymore in most recent N scattering PWA [Arndt et al. 03] If Q is extremely narrow N* should be also narrow 10-20 MeV. Narrow resonance easy to miss in PWA. There is a possiblity for narrow N*(1/2+) at 1680 and/or 1730 MeV [Arndt et al. 03] In the ...
... Non strange partners revisited N(1710) is not seen anymore in most recent N scattering PWA [Arndt et al. 03] If Q is extremely narrow N* should be also narrow 10-20 MeV. Narrow resonance easy to miss in PWA. There is a possiblity for narrow N*(1/2+) at 1680 and/or 1730 MeV [Arndt et al. 03] In the ...
Solar Radiation - Energy
... In the convective zone, which follows the radiative zone (from 0.7 solar radii to the full solar radius), the solar plasma has a much lower density (about ) and also a lower temperature (about 2,000,000 K) than in the radiative zone. The energy transport occurs through convection. The visible surfac ...
... In the convective zone, which follows the radiative zone (from 0.7 solar radii to the full solar radius), the solar plasma has a much lower density (about ) and also a lower temperature (about 2,000,000 K) than in the radiative zone. The energy transport occurs through convection. The visible surfac ...
Synthetic Light Curves of Shocked Dense Circumstellar Shells
... Initial conditions of our numerical calculations are constructed based on SM07 at first. We do not follow shock propagation in shells to make the initial conditions the same as those of SM07. The initial conditions are supposed to result from the shock passage in the dense circumstellar shell. Since ...
... Initial conditions of our numerical calculations are constructed based on SM07 at first. We do not follow shock propagation in shells to make the initial conditions the same as those of SM07. The initial conditions are supposed to result from the shock passage in the dense circumstellar shell. Since ...
Determination of the position angle of stellar spin axes
... There is currently a lack of observational methods for determining stellar spin orientation for slowly rotating stars. We investigate the potential of spectro-astrometry to measure the position angle of these stars, with focus on late-type giants. We aim here to define the optimal conditions, instru ...
... There is currently a lack of observational methods for determining stellar spin orientation for slowly rotating stars. We investigate the potential of spectro-astrometry to measure the position angle of these stars, with focus on late-type giants. We aim here to define the optimal conditions, instru ...
ertan et al 11cesme
... AXP/SGRs. For the sources with weaker magnetic dipole fields, rin comes out of the light cylinder earlier than it does for the sources with stronger dipole fields. After this point, P remains almost constant because of decreasing efficiency of the disk torque [2]. As seen in Fig. 1, the model source ...
... AXP/SGRs. For the sources with weaker magnetic dipole fields, rin comes out of the light cylinder earlier than it does for the sources with stronger dipole fields. After this point, P remains almost constant because of decreasing efficiency of the disk torque [2]. As seen in Fig. 1, the model source ...
The Milky Way galaxy Contents Summary
... Galaxies vary enormously in size from objects that contain only 100 000 stars, to ones with hundreds of billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Uni ...
... Galaxies vary enormously in size from objects that contain only 100 000 stars, to ones with hundreds of billions of stars. The smaller galaxies are much more numerous than the larger ones, but not by a sufficient factor to compensate for their lower luminosities. So most of the luminosity in the Uni ...
A SIGNIFICANTLY LOW CO ABUNDANCE TOWARD THE TW Hya
... (Aikawa et al. 1996; Dartois et al. 2003). Under normal conditions CO freezes-out at low temperatures present in the midplane, T 20 K, where HD does not strongly emit, and therefore the reduced measured χ (CO) in the gas-phase is unlikely to be the result of freeze-out. In fact a number of studies ...
... (Aikawa et al. 1996; Dartois et al. 2003). Under normal conditions CO freezes-out at low temperatures present in the midplane, T 20 K, where HD does not strongly emit, and therefore the reduced measured χ (CO) in the gas-phase is unlikely to be the result of freeze-out. In fact a number of studies ...
