FIRST LIGHT IN THE UNIVERSE
... • Contribution of lower luminosity systems less clear (lensing: Lecture 7) • Spitzer’s IRAC can detect large numbers of z~5-6 galaxies and it seems many have high masses (one spectacularly so!) and signatures of mature stellar populations - implies earlier activity • Reconciling mature galaxies at z ...
... • Contribution of lower luminosity systems less clear (lensing: Lecture 7) • Spitzer’s IRAC can detect large numbers of z~5-6 galaxies and it seems many have high masses (one spectacularly so!) and signatures of mature stellar populations - implies earlier activity • Reconciling mature galaxies at z ...
Can Planets survive Stellar Evolution?
... Single white dwarf progenitors are expected to have main sequence masses in the range from 1 to about 8 M⊙ mass (the upper mass limit is not well established). As these stars leave the main sequence they evolve into the RGB, Horizontal Branch, AGB, and PN phases in the Hertzsprung-Russell (HR) diagr ...
... Single white dwarf progenitors are expected to have main sequence masses in the range from 1 to about 8 M⊙ mass (the upper mass limit is not well established). As these stars leave the main sequence they evolve into the RGB, Horizontal Branch, AGB, and PN phases in the Hertzsprung-Russell (HR) diagr ...
1. INTRODUCTION 2. MASS AND LIGHT
... 2. The argument of ° 2 fails because the intervening structures happen to be contained within 5¡ of the LMC center (although they must extend over at least the inner D3¡ to account for the observed events). This possibility could only apply to a self-gravitating structure and not to an intrinsically ...
... 2. The argument of ° 2 fails because the intervening structures happen to be contained within 5¡ of the LMC center (although they must extend over at least the inner D3¡ to account for the observed events). This possibility could only apply to a self-gravitating structure and not to an intrinsically ...
Neutron Stars - Lick Observatory
... rotating with relatively small period derivatives. In a (P, P! ) diagram they cluster around P ! 1 s and P! ! 10!15. A few young pulsars, e.g. those such as the CRAB and VELA PULSARS, have short periods and large period derivatives. The nearest known neutron star, RXJ185635-3754, located in the sout ...
... rotating with relatively small period derivatives. In a (P, P! ) diagram they cluster around P ! 1 s and P! ! 10!15. A few young pulsars, e.g. those such as the CRAB and VELA PULSARS, have short periods and large period derivatives. The nearest known neutron star, RXJ185635-3754, located in the sout ...
The chemical case for no winds in dwarf irregular galaxies
... In this work, we focus our attention on the evolution of isolated gas-rich dwarf galaxies, not affected by external environmental processes. One of the agents that may regulate the star formation history of these objects is the presence of strong galactic winds. If they have a low mass and a high st ...
... In this work, we focus our attention on the evolution of isolated gas-rich dwarf galaxies, not affected by external environmental processes. One of the agents that may regulate the star formation history of these objects is the presence of strong galactic winds. If they have a low mass and a high st ...
Neutron stars: compact objects with relativistic gravity
... was clearly established that the energy is expelled from the system at the rate gravitational waves would take away as predicted within general relativity [30–34]. Given that the strong surface gravity of neutron stars is at a regime not probed by the solar system tests and binary pulsars, one may h ...
... was clearly established that the energy is expelled from the system at the rate gravitational waves would take away as predicted within general relativity [30–34]. Given that the strong surface gravity of neutron stars is at a regime not probed by the solar system tests and binary pulsars, one may h ...
Magnetic fields in Local Group dwarf irregulars⋆
... and dwarf irregular galaxies with the 100-m Effelsberg telescope at 2.64 GHz. Three galaxies were detected. A higher frequency (4.85 GHz) was used to search for polarized emission in five dwarfs that are the most luminous ones in the infrared domain, of which three were detected. Results. Magnetic fi ...
... and dwarf irregular galaxies with the 100-m Effelsberg telescope at 2.64 GHz. Three galaxies were detected. A higher frequency (4.85 GHz) was used to search for polarized emission in five dwarfs that are the most luminous ones in the infrared domain, of which three were detected. Results. Magnetic fi ...
Expanding the Catalog: Considering the Importance
... For the higher mass models (the left-hand column of Figure 1) we see evidence of the Kelvin-Helmholtz mechanism (KH “jag”), wherein a star nearing the end of its MS lifetime begins to cool and compress due to decreased internal pressure from the end of core hydrogen burning. This compression reheats ...
... For the higher mass models (the left-hand column of Figure 1) we see evidence of the Kelvin-Helmholtz mechanism (KH “jag”), wherein a star nearing the end of its MS lifetime begins to cool and compress due to decreased internal pressure from the end of core hydrogen burning. This compression reheats ...
The accretion properties of the intermediate mass Herbig Ae/Be stars
... correlate with accretion luminosity. Can be used as accretion diagnostic Lacc determination much easier than using UV excess Extended the number of calibrated lines to entire XShooter spectral range Fairlamb+ 2016, subm. Mendigutia+2011, Garcia-Lopez+ 2005, Muzerolle+2004, Donehew & Brittain 2011 ...
... correlate with accretion luminosity. Can be used as accretion diagnostic Lacc determination much easier than using UV excess Extended the number of calibrated lines to entire XShooter spectral range Fairlamb+ 2016, subm. Mendigutia+2011, Garcia-Lopez+ 2005, Muzerolle+2004, Donehew & Brittain 2011 ...
Chapter 5 - Leiden Observatory
... onto different stars can be found in Appendix 5.A.2. The accretion procedure previously used in SeBa is complemented with a procedure for accretion from a hydrogen-poor star. We assume that for ordinary stars, helium-rich matter is accreted directly to the core of the star. The mass accretion process ...
... onto different stars can be found in Appendix 5.A.2. The accretion procedure previously used in SeBa is complemented with a procedure for accretion from a hydrogen-poor star. We assume that for ordinary stars, helium-rich matter is accreted directly to the core of the star. The mass accretion process ...
Mass segregation in star clusters is not energy equipartition
... not moving more slowly, nor are the brown dwarfs moving faster than the average stars in the cluster. We note that Zapatero Osorio et al. (2014) find evidence that the proper motions of objects in the Plaiedes cluster increase with decreasing mass. We suggest that this result is probably due to the ...
... not moving more slowly, nor are the brown dwarfs moving faster than the average stars in the cluster. We note that Zapatero Osorio et al. (2014) find evidence that the proper motions of objects in the Plaiedes cluster increase with decreasing mass. We suggest that this result is probably due to the ...
Abundance Anomalies In Tidal Disruption Events
... find that extreme hydrogen to helium line ratios are achievable at Solar metallicity using broad line widths and radiation transfer models better suited to high optical depths than CLOUDY. All these calculations have assumed that the debris has Solar composition. This may be true at birth on the zer ...
... find that extreme hydrogen to helium line ratios are achievable at Solar metallicity using broad line widths and radiation transfer models better suited to high optical depths than CLOUDY. All these calculations have assumed that the debris has Solar composition. This may be true at birth on the zer ...
Testing the Initial-Final Mass Relationship of White Dwarfs Silvia Catal´ an Ruiz
... have focused in studying white dwarfs in open clusters (Ferrario et al. 2005, Dobbie et al. 2006), whose ages can be determined from model fits to the turn-off location in a color-magnitude diagram. One of the aims of this work is to increase the number of observational data points by studying white ...
... have focused in studying white dwarfs in open clusters (Ferrario et al. 2005, Dobbie et al. 2006), whose ages can be determined from model fits to the turn-off location in a color-magnitude diagram. One of the aims of this work is to increase the number of observational data points by studying white ...
The white dwarf luminosity function
... stars in the local neighborhood which, in turn, provides an important constraint on pre-white dwarf stellar evolutionary sequences. However, in order to use the white dwarf luminosity function to study these interesting astrophysical problems, it is necessary to have good observational data, accurat ...
... stars in the local neighborhood which, in turn, provides an important constraint on pre-white dwarf stellar evolutionary sequences. However, in order to use the white dwarf luminosity function to study these interesting astrophysical problems, it is necessary to have good observational data, accurat ...
Ultra faint dwarfs: probing early cosmic star formation
... UFs are the oldest and most dark matter (M/L > 100) dominated dSphs in the MW system with a total mass M = 107−8 M⊙ and L = 103−5 L⊙ ; they are found to be left-overs of H2 -cooling minihaloes formed at z > 8.5, i.e. before reionization. Their MDF is broader (because of their more prolonged SF) and ...
... UFs are the oldest and most dark matter (M/L > 100) dominated dSphs in the MW system with a total mass M = 107−8 M⊙ and L = 103−5 L⊙ ; they are found to be left-overs of H2 -cooling minihaloes formed at z > 8.5, i.e. before reionization. Their MDF is broader (because of their more prolonged SF) and ...
Gaseous Planets, Protostars And Young Brown Dwarfs
... Physikalisches Institut, University of Bern We review recent theoretical progress aimed at understanding the formation and the early stages of evolution of giant planets, low-mass stars and brown dwarfs. Calculations coupling giant planet formation, within a modern version of the core accretion mode ...
... Physikalisches Institut, University of Bern We review recent theoretical progress aimed at understanding the formation and the early stages of evolution of giant planets, low-mass stars and brown dwarfs. Calculations coupling giant planet formation, within a modern version of the core accretion mode ...
Finding Hot-Jupiters by Gaia photometry using the Directed Follow
... “Hipparcos Catalog does not represent a likely place to detect planets in the absence (Jenkins et al. 2002) orbital period (≈ 3.5 days), the transit dura- of 2. other Hipparcosinformation” photometric measurements ...
... “Hipparcos Catalog does not represent a likely place to detect planets in the absence (Jenkins et al. 2002) orbital period (≈ 3.5 days), the transit dura- of 2. other Hipparcosinformation” photometric measurements ...
Long-term photometry of the eclipsing dwarf nova V893 Scorpii
... Cataclysmic variables (CVs) are well known to be short period interacting binary systems where a Roche-lobe filling star, the secondary, transfers matter via an accretion disk to a white dwarf primary. The structure of CVs can best be studied in systems where the secondary, which is faint and contri ...
... Cataclysmic variables (CVs) are well known to be short period interacting binary systems where a Roche-lobe filling star, the secondary, transfers matter via an accretion disk to a white dwarf primary. The structure of CVs can best be studied in systems where the secondary, which is faint and contri ...
Pre-supernova evolution of massive stars
... in our schematic picture (Chapter 7, shown as a dotted arrow), but some deviation to higher ρ and lower T occurs due to neutrino losses. Non-monotonic (non-homologous) behaviour is seen whenever nuclear fuels are ignited and a convective core is formed. (Figure adapted from Woosley, Heger & Weaver 2 ...
... in our schematic picture (Chapter 7, shown as a dotted arrow), but some deviation to higher ρ and lower T occurs due to neutrino losses. Non-monotonic (non-homologous) behaviour is seen whenever nuclear fuels are ignited and a convective core is formed. (Figure adapted from Woosley, Heger & Weaver 2 ...
PDF only
... the age, , and magnetic field of a pulsar from the measured values of and ; for example, (lines of constant and are shown in Figure 1b). Although model dependent, observations yield the ranges and , with some of the youngest objects having the largest magnetic fields (magnetars) and the oldest ones ...
... the age, , and magnetic field of a pulsar from the measured values of and ; for example, (lines of constant and are shown in Figure 1b). Although model dependent, observations yield the ranges and , with some of the youngest objects having the largest magnetic fields (magnetars) and the oldest ones ...
Dark Matter Spiral Structure Basic Galaxy Morphology Disk Galaxy Rotation Curves:
... It cannot be concentrated in the disk, as it would make the velocity dispersion of stars too high. ...
... It cannot be concentrated in the disk, as it would make the velocity dispersion of stars too high. ...
Constraining the Bulk Properties of Dense Matter by Measuring
... The most massive observed neutron star also sets a quantitative upper limit to its central density, which then cannot be exceeded in any neutron star. As successively more massive neutron stars are observed, the limiting central density gets smaller. Approximately, the limit is ρmax ≤ 36ρs (M /Mmax ...
... The most massive observed neutron star also sets a quantitative upper limit to its central density, which then cannot be exceeded in any neutron star. As successively more massive neutron stars are observed, the limiting central density gets smaller. Approximately, the limit is ρmax ≤ 36ρs (M /Mmax ...
Interpretation of the Helix Planetary Nebula using Hydro
... acoustical density fluctuations on scales larger than LJ (Gibson 1996). Contrary to the common misconception, pressure and temperature cannot prevent structure formation on scales larger or smaller than LJ . Density fluctuations in fluids are not barotropic as assumed by Jeans 1902 except rarely in sma ...
... acoustical density fluctuations on scales larger than LJ (Gibson 1996). Contrary to the common misconception, pressure and temperature cannot prevent structure formation on scales larger or smaller than LJ . Density fluctuations in fluids are not barotropic as assumed by Jeans 1902 except rarely in sma ...
1. Basic Properties of Stars
... G, K and M. Note that the spectra classes are also divisions of temperature such that O stars are hot, M stars are cool. Between the classes there were 10 subdivisions numbered 0 to 9. For example, our Sun is a G2 star. Sirius, a hot blue star, is type B3. Why do some stars have strong lines of hydr ...
... G, K and M. Note that the spectra classes are also divisions of temperature such that O stars are hot, M stars are cool. Between the classes there were 10 subdivisions numbered 0 to 9. For example, our Sun is a G2 star. Sirius, a hot blue star, is type B3. Why do some stars have strong lines of hydr ...
Stellar Populations For many modern applications, one is not
... The above analytic solutions are only useful for guidance. To compare with observations, predictions must be made in specific bandpasses, or for specific absorption lines. This requires numerical calculations which include 1) sets of stellar isochrones, detailing the precise number of stars at any p ...
... The above analytic solutions are only useful for guidance. To compare with observations, predictions must be made in specific bandpasses, or for specific absorption lines. This requires numerical calculations which include 1) sets of stellar isochrones, detailing the precise number of stars at any p ...