The Rare Isotope Accelerator Program at MSU
... be the world-leading facility for research in nuclear structure and nuclear astrophysics. • The exciting new scientific opportunities offered by research with rare isotopes are compelling. RIA is required to exploit these opportunities and to ensure world leadership in these areas of nuclear science ...
... be the world-leading facility for research in nuclear structure and nuclear astrophysics. • The exciting new scientific opportunities offered by research with rare isotopes are compelling. RIA is required to exploit these opportunities and to ensure world leadership in these areas of nuclear science ...
Star formation rates and efficiencies in the Galactic Centre
... a difficult quantity to determine, as inferences of the threedimensional structure have to be made in order to convert two-dimensional line-of-sight column density measurements. The measured column density of hydrogen in the CMZ appears to be at least an order of magnitude higher than clouds within ...
... a difficult quantity to determine, as inferences of the threedimensional structure have to be made in order to convert two-dimensional line-of-sight column density measurements. The measured column density of hydrogen in the CMZ appears to be at least an order of magnitude higher than clouds within ...
observations of white dwarfs in the solar neighborhood
... and June 22. We used the SITE 2048 2048 CCD and the 600 line mm1 grating to obtain a spectral range of 4210– 7560 Å with substantial vignetting toward the ends of this range. The 100 slit gave 3.2 Å spectral resolution (FWHM). The main observing program was focused on accurate radial velocitie ...
... and June 22. We used the SITE 2048 2048 CCD and the 600 line mm1 grating to obtain a spectral range of 4210– 7560 Å with substantial vignetting toward the ends of this range. The 100 slit gave 3.2 Å spectral resolution (FWHM). The main observing program was focused on accurate radial velocitie ...
A Study of Herbig Ae Be Star HD 163296: Variability in
... fields across the star. This dipole is thought to be responsible for several different mechanisms surrounding the star, including outflows and accretion. The strength and consistency of the dipole is dependent on both the age and mass of the star. We will discuss each of these variables in the next ...
... fields across the star. This dipole is thought to be responsible for several different mechanisms surrounding the star, including outflows and accretion. The strength and consistency of the dipole is dependent on both the age and mass of the star. We will discuss each of these variables in the next ...
Polaris B, an optical companion of the Polaris (αUMi) system
... Polaris B (BD+88◦ 7; SAO 305) is the nearest optical companion to the Cepheid binary Polaris Ab (α UMi) system. Its visual magnitude of 8.60 mag, angular distance of 18 arcsec from Polaris, and spectral type of F3 V suggest that it is a physical main-sequence companion of α UMi (Fernie 1966; Turner ...
... Polaris B (BD+88◦ 7; SAO 305) is the nearest optical companion to the Cepheid binary Polaris Ab (α UMi) system. Its visual magnitude of 8.60 mag, angular distance of 18 arcsec from Polaris, and spectral type of F3 V suggest that it is a physical main-sequence companion of α UMi (Fernie 1966; Turner ...
The nature of the ultraluminous X-ray sources inside galaxies and
... nearby Seyfert galaxies with XMM-Newton has shown that Send offprint requests to: G. Burbidge, e-mail: [email protected] ...
... nearby Seyfert galaxies with XMM-Newton has shown that Send offprint requests to: G. Burbidge, e-mail: [email protected] ...
Asymptotic Giant Branch stars viewed up-close and far-off
... the luminosity slowly increases until it reaches a maximum just before the next shell flash. During this ‘quiet’ phase, the base of the convective envelope reaches into the intershell region now enriched with new elements created in the ISCZ due to various processes, e.g. the s-process (see below), ...
... the luminosity slowly increases until it reaches a maximum just before the next shell flash. During this ‘quiet’ phase, the base of the convective envelope reaches into the intershell region now enriched with new elements created in the ISCZ due to various processes, e.g. the s-process (see below), ...
Polaris B, an optical companion of Polaris (alpha UMi) system
... (HJD 2453904.879) using 6 m telescope BTA of the Special Astrophysical Observatory of the Russian Academy of Sciences with the high resolution echelle spectrograph NES (Panchuk et al. 2002). In combination both with CCD 2048 x 2048 pixels and with an image slicer (Panchuk et al. 2003), NES provides ...
... (HJD 2453904.879) using 6 m telescope BTA of the Special Astrophysical Observatory of the Russian Academy of Sciences with the high resolution echelle spectrograph NES (Panchuk et al. 2002). In combination both with CCD 2048 x 2048 pixels and with an image slicer (Panchuk et al. 2003), NES provides ...
Master Thesis - Sterrenkunde RU Nijmegen
... iron and nickel. Fusing iron and nickel does not produce any energy, and thus the pressure drops. This causes the star to implode, which release enormous amounts of potential energy, which heats up the outer parts of the star. The star explodes as a supernova and the core either end up as a neutron ...
... iron and nickel. Fusing iron and nickel does not produce any energy, and thus the pressure drops. This causes the star to implode, which release enormous amounts of potential energy, which heats up the outer parts of the star. The star explodes as a supernova and the core either end up as a neutron ...
PDF hosted at the Radboud Repository of the Radboud University
... Single carbon-oxygen white dwarfs are not formed at masses larger than 1.2M , and the majority are born at masses considerably lower than that, typically around ∼ 0.6M (Homeier et al. 1998). However, type Ia supernovae likely originate from carbon-oxygen white dwarfs at or close to the Chandrasekh ...
... Single carbon-oxygen white dwarfs are not formed at masses larger than 1.2M , and the majority are born at masses considerably lower than that, typically around ∼ 0.6M (Homeier et al. 1998). However, type Ia supernovae likely originate from carbon-oxygen white dwarfs at or close to the Chandrasekh ...
Seminar 2
... show significant changes with redshift, the overall space density of galaxies is constant up to z = 1, indicating that the number of galaxies seem to be constant in this redshift range. The nature of the large fraction of peculiar galaxies at higher redshifts remains a mystery, but it seems conceiva ...
... show significant changes with redshift, the overall space density of galaxies is constant up to z = 1, indicating that the number of galaxies seem to be constant in this redshift range. The nature of the large fraction of peculiar galaxies at higher redshifts remains a mystery, but it seems conceiva ...
Large scale kinematics and dynamical modelling of the Milky Way
... the Galactic centre, but only 15 of their targets are within 8 pc from the Galactic centre, and therefore likely cluster members. McGinn et al. (1989) obtained integrated light spectra of selected fields with a 2000 (0.78 pc) aperture at 2.3 µm out to ∼4 pc (1.70 ) distance along the Galactic plane ...
... the Galactic centre, but only 15 of their targets are within 8 pc from the Galactic centre, and therefore likely cluster members. McGinn et al. (1989) obtained integrated light spectra of selected fields with a 2000 (0.78 pc) aperture at 2.3 µm out to ∼4 pc (1.70 ) distance along the Galactic plane ...
The Milky Way-Pulsars and Isolated Neutron Stars
... be so faint in X-rays that further observations at that energy range would be hopeless. On the other hand, results from high-energy cosmic ray experiments suggested that there exist celestial objects (e.g. supernova remnants) which produce high-energy cosmic rays in processes which, in turn, may als ...
... be so faint in X-rays that further observations at that energy range would be hopeless. On the other hand, results from high-energy cosmic ray experiments suggested that there exist celestial objects (e.g. supernova remnants) which produce high-energy cosmic rays in processes which, in turn, may als ...
Electron Scattering from an Almost Free Neutron in
... obtaining the ratio F2 / F2 at high Bjorken x. The F2 structure function is difficult to obtain due to nature’s lack of a free neutron target. Previous experiments have measured n inclusive scattering from atomic nuclei, but extracting F2 from these data requires knowledge of inclusive scattering fr ...
... obtaining the ratio F2 / F2 at high Bjorken x. The F2 structure function is difficult to obtain due to nature’s lack of a free neutron target. Previous experiments have measured n inclusive scattering from atomic nuclei, but extracting F2 from these data requires knowledge of inclusive scattering fr ...
SKA and VLBI synergies
... VLBI observations have remarkably strong impact in the Stellar physics studies. We can mention the study of Gamma Ray Bursts (GRBs), Radio Supernovae (RSNe) and Supernova Remnants (SNRs), Microquasars or Pulsars, among others. Moreover, VLBI astrometry is a unique tool providing stellar parallax mea ...
... VLBI observations have remarkably strong impact in the Stellar physics studies. We can mention the study of Gamma Ray Bursts (GRBs), Radio Supernovae (RSNe) and Supernova Remnants (SNRs), Microquasars or Pulsars, among others. Moreover, VLBI astrometry is a unique tool providing stellar parallax mea ...
Doppler imaging of AB Doradus using the Li I 6708 line
... The Li abundance is measured in the following way. A model image is generated from a fit obtained using Ca I and Fe I lines. Model profiles are then produced using this image and different lookup value is tables with increasing values of Li abundances. The measured for each of these sets of model pr ...
... The Li abundance is measured in the following way. A model image is generated from a fit obtained using Ca I and Fe I lines. Model profiles are then produced using this image and different lookup value is tables with increasing values of Li abundances. The measured for each of these sets of model pr ...
Massive Star Formation in the Galactic Center
... cluster. The following sections describe the stellar content in the clusters and the resultant implications for star formation in the region. They closely follow recent reviews (Figer et al. 1999a; Figer 2003, 2004), with updates, as summarized in Table 1. The three clusters are similar in many resp ...
... cluster. The following sections describe the stellar content in the clusters and the resultant implications for star formation in the region. They closely follow recent reviews (Figer et al. 1999a; Figer 2003, 2004), with updates, as summarized in Table 1. The three clusters are similar in many resp ...
Astrophysical Quark Matter
... QM in pulsar-like compact stars It is still a challenge for astrophysicists to reproduce a successful core-collapse supernova! ...
... QM in pulsar-like compact stars It is still a challenge for astrophysicists to reproduce a successful core-collapse supernova! ...
radioactive 26a1 in the galaxy: observations versus theory
... Enter rudioactivity. Stellar nucleosynthesis produces not only stable, but also unstable nuclei with lifetimes ranging from seconds to billions of years. Their radioactive transitions may give rise to y-ray photons which, under certain conditions, may be detected by sufficiently sensitive instrument ...
... Enter rudioactivity. Stellar nucleosynthesis produces not only stable, but also unstable nuclei with lifetimes ranging from seconds to billions of years. Their radioactive transitions may give rise to y-ray photons which, under certain conditions, may be detected by sufficiently sensitive instrument ...
![The P Cygni supergiant [OMN2000] LS1](http://s1.studyres.com/store/data/014882705_1-5f78b60dc5267f0c5ad35fc8d810ae0e-300x300.png)
galaxy formation with cold gas accretion and evolving stellar initial
... evolves with time, the correction does depend on galaxy mass and redshift (Marchesini et al. 2009), and determining these dependences is beyond the scope of this paper. For our comparison of galaxy SMFs, we continue to use the C03 IMF and focus on the effects of cold accretion and tidal stripping on ...
... evolves with time, the correction does depend on galaxy mass and redshift (Marchesini et al. 2009), and determining these dependences is beyond the scope of this paper. For our comparison of galaxy SMFs, we continue to use the C03 IMF and focus on the effects of cold accretion and tidal stripping on ...
Here
... I hereby declare that my thesis entitled The Evolution and Nucleosynthesis of Thermally Pulsing Asymptotic Giant Branch Stars is not substantially the same as any that I have submitted for a degree or diploma or other qualification at any other University. I further state that no part of my thesis h ...
... I hereby declare that my thesis entitled The Evolution and Nucleosynthesis of Thermally Pulsing Asymptotic Giant Branch Stars is not substantially the same as any that I have submitted for a degree or diploma or other qualification at any other University. I further state that no part of my thesis h ...
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.