Implications for dwarf spheroidal mass content from interloper removal
... to identify in gas, but not from the discrete distribution of stars (McConnachie et al. 2009). The same is true for clusters of galaxies when the mass is inferred from the measured temperature and density of the X-ray emitting plasma. Alternatively, cluster masses can be measured with gravitational ...
... to identify in gas, but not from the discrete distribution of stars (McConnachie et al. 2009). The same is true for clusters of galaxies when the mass is inferred from the measured temperature and density of the X-ray emitting plasma. Alternatively, cluster masses can be measured with gravitational ...
The spin-up of contracting red supergiants
... of angular momentum in the helium core is much smaller than that in the hydrogen-rich envelope ( ∼ < 2 % in the 12 M model discussed below), so that even if all of that would be transported out into the envelope it would not alter its angular momentum balance much. As a star evolves into a red supe ...
... of angular momentum in the helium core is much smaller than that in the hydrogen-rich envelope ( ∼ < 2 % in the 12 M model discussed below), so that even if all of that would be transported out into the envelope it would not alter its angular momentum balance much. As a star evolves into a red supe ...
Core-Halo Age Gradients and Star Formation in the Orion Nebula
... scales, the formation of rich stellar clusters dominated by OB stars is quite uncertain. Debate has waged for decades over the relative importance of rapid ‘top-down’ fragmentation or a slower ‘bottom-up’ process involving merging of subcomponents (Clarke et al. 2000). In the former model, cluster f ...
... scales, the formation of rich stellar clusters dominated by OB stars is quite uncertain. Debate has waged for decades over the relative importance of rapid ‘top-down’ fragmentation or a slower ‘bottom-up’ process involving merging of subcomponents (Clarke et al. 2000). In the former model, cluster f ...
STIS/HST Observations of Large Magellanic Cloud Planetary
... J. C. Blades (STScI), & B. Balick (UoW) The STIS/HST Survey of LMC PNs Planetary Nebulae (PNs) have for many years been used as probes of the late stages of stellar evolution. While in many ways such studies have been very successful, and have inspired elaborate theoretical work on stellar evolution ...
... J. C. Blades (STScI), & B. Balick (UoW) The STIS/HST Survey of LMC PNs Planetary Nebulae (PNs) have for many years been used as probes of the late stages of stellar evolution. While in many ways such studies have been very successful, and have inspired elaborate theoretical work on stellar evolution ...
On the role of the WNH phase in the evolution of very massive stars
... We propose the new designation “WNH” for luminous Wolf-Rayet (WR) stars of the nitrogen sequence with hydrogen in their spectra. These have been commonly referred to as WNL stars (WN7h, for example), but this new shorthand avoids confusion because there are late-type WN stars without hydrogen and ea ...
... We propose the new designation “WNH” for luminous Wolf-Rayet (WR) stars of the nitrogen sequence with hydrogen in their spectra. These have been commonly referred to as WNL stars (WN7h, for example), but this new shorthand avoids confusion because there are late-type WN stars without hydrogen and ea ...
The eccentricities of the barium stars
... have an index of either ,1, 1 or 2. The sample of spectroscopically normal giant binaries have MK spectral classifications indicating giant luminosity and G or K spectral type as the barium stars. The average eccentricities are 0.17 for the barium stars and 0.23 for the normal giants, while a Kolmog ...
... have an index of either ,1, 1 or 2. The sample of spectroscopically normal giant binaries have MK spectral classifications indicating giant luminosity and G or K spectral type as the barium stars. The average eccentricities are 0.17 for the barium stars and 0.23 for the normal giants, while a Kolmog ...
THE ORIGIN AND EVOLUTION OF PLANETARY NEBULAE
... He therefore argued that the emission-line spectrum of PN is the result of the nebula absorbing the continuous radiation from the central star. In order to explain the strength of the Hβ line, Menzel (1926) suggested that all the stellar output beyond the Lyman limit (912 Å) must be utilized to ion ...
... He therefore argued that the emission-line spectrum of PN is the result of the nebula absorbing the continuous radiation from the central star. In order to explain the strength of the Hβ line, Menzel (1926) suggested that all the stellar output beyond the Lyman limit (912 Å) must be utilized to ion ...
ppt - Serbian Virtual Observatory
... the end of 1963, with which Konkoly Observatory for about more than a 30-year period took part in the international campaign initiated by F. Zwicky. •Konkoly Flare Star Digital Archive – of representative plates obtained with the Schmidt telescopes of Konkoly observatory during the observation campa ...
... the end of 1963, with which Konkoly Observatory for about more than a 30-year period took part in the international campaign initiated by F. Zwicky. •Konkoly Flare Star Digital Archive – of representative plates obtained with the Schmidt telescopes of Konkoly observatory during the observation campa ...
A Study of Herbig Ae Be Star HD 163296: Variability in
... plasma to areas much cooler than the ones close to the core, where fusion is taking place. These parcels rise up slightly and are much warmer than the surrounding material, causing them to have a lower density. Now, the parcels continues to rise up due to its newfound buoyancy. This causes other par ...
... plasma to areas much cooler than the ones close to the core, where fusion is taking place. These parcels rise up slightly and are much warmer than the surrounding material, causing them to have a lower density. Now, the parcels continues to rise up due to its newfound buoyancy. This causes other par ...
Theoretical and observational framework Spectroscopic approach
... • The presence of fast HB rotators is confirmed and extended to other clusters. • The abundance of fast HB rotators can apparently change from cluster to cluster. • The change in rotational velocity seems to be associated to the onset of diffusive processes in the stellar atmosphere. • Radiative lev ...
... • The presence of fast HB rotators is confirmed and extended to other clusters. • The abundance of fast HB rotators can apparently change from cluster to cluster. • The change in rotational velocity seems to be associated to the onset of diffusive processes in the stellar atmosphere. • Radiative lev ...
The Milky Way and Andromeda galaxies in a constrained
... to produce similar results using different codes, despite their individual successes. Efforts to overcome these problems are indeed ongoing, both in terms of direct comparison between codes (Kim et al. 2014) and of the development of more physicallymotivated routines to treat star formation and feedba ...
... to produce similar results using different codes, despite their individual successes. Efforts to overcome these problems are indeed ongoing, both in terms of direct comparison between codes (Kim et al. 2014) and of the development of more physicallymotivated routines to treat star formation and feedba ...
IR-excesses around nearby Lambda Boo stars are caused by debris
... found around stars of ∼1 Gyr in age, subgiants, and even white dwarfs (Bonsor et al. 2014a; Matthews et al. 2014b). If the mechanism were internal, A stars would need to have a very specific criteria for initiating and ceasing a Lambda Boo-like phase, independent of age and stellar evolution. In ord ...
... found around stars of ∼1 Gyr in age, subgiants, and even white dwarfs (Bonsor et al. 2014a; Matthews et al. 2014b). If the mechanism were internal, A stars would need to have a very specific criteria for initiating and ceasing a Lambda Boo-like phase, independent of age and stellar evolution. In ord ...
The Milky Way galaxy Contents Summary
... them to drift inwards. The outward thrust from the bar and the frictional inward drift balance just outside rcr , and gas accumulates here. This accumulation of gas near rcr is conspicuous in the lower panel of Figure 8 as a band of emission that slopes from upper left to lower right at |l| < 25◦ . ...
... them to drift inwards. The outward thrust from the bar and the frictional inward drift balance just outside rcr , and gas accumulates here. This accumulation of gas near rcr is conspicuous in the lower panel of Figure 8 as a band of emission that slopes from upper left to lower right at |l| < 25◦ . ...
ASTROPHYSICAL PARAMETERS OF LS 2883 AND IMPLICATIONS FOR THE Y egueruela ,
... PSR B1259–63, showing it to rotate faster and be significantly earlier and more luminous than previously thought. Analysis of the interstellar lines suggests that the system is located at the same distance as (and thus is likely a member of) Cen OB1. Taking the distance to the association, d = 2.3 k ...
... PSR B1259–63, showing it to rotate faster and be significantly earlier and more luminous than previously thought. Analysis of the interstellar lines suggests that the system is located at the same distance as (and thus is likely a member of) Cen OB1. Taking the distance to the association, d = 2.3 k ...
Massive Stars in the Arches Cluster 12
... to be vcluster, ≈ +95 km s−1 . Taken together, these results suggest that the Arches cluster was formed in a short, but massive, burst of star formation about 2.5±0.5 Myr ago, from a molecular cloud which is no longer present. The cluster happens to be approaching and ionizing the surface of a back ...
... to be vcluster, ≈ +95 km s−1 . Taken together, these results suggest that the Arches cluster was formed in a short, but massive, burst of star formation about 2.5±0.5 Myr ago, from a molecular cloud which is no longer present. The cluster happens to be approaching and ionizing the surface of a back ...
The impact of rotation on the line profiles of Wolf
... Potsdam Wolf-Rayet (PoWR) model atmosphere code potentially imply the existence of rapidly rotating WR stars. Hamann et al. (2006) performed a flux-convolution with a rotation profile (e.g. Unsöld 1955) in order to reproduce the broad and round emission lines of the Galactic WN2 star WR 2. Hainich e ...
... Potsdam Wolf-Rayet (PoWR) model atmosphere code potentially imply the existence of rapidly rotating WR stars. Hamann et al. (2006) performed a flux-convolution with a rotation profile (e.g. Unsöld 1955) in order to reproduce the broad and round emission lines of the Galactic WN2 star WR 2. Hainich e ...
A PCA approach to stellar effective temperatures⋆
... Key words. stars: fundamental parameters – catalogs – techniques: spectroscopic – stars: solar-type ...
... Key words. stars: fundamental parameters – catalogs – techniques: spectroscopic – stars: solar-type ...
Astronomy Astrophysics - Utrecht University Repository
... is the observed minimum brightness of the EROS II light curve over the 5 years of observations. The size of the symbols corresponds to the RE -band amplitude of variability during the period of EROS II observations. The figure shows that the stars are distributed on an increasingly wider range of ∆R ...
... is the observed minimum brightness of the EROS II light curve over the 5 years of observations. The size of the symbols corresponds to the RE -band amplitude of variability during the period of EROS II observations. The figure shows that the stars are distributed on an increasingly wider range of ∆R ...
Tracing the evolution of NGC 6397 through the chemical
... scenario are the initial mass function (IMF) of the polluting stars, the initial total mass of the cluster, and the amount of mixing between processed gas in the slow stellar ejecta and pristine cluster gas. We discuss these issues in Sect. 4. HST photometry of NGC 6397 produces a remarkably clean H ...
... scenario are the initial mass function (IMF) of the polluting stars, the initial total mass of the cluster, and the amount of mixing between processed gas in the slow stellar ejecta and pristine cluster gas. We discuss these issues in Sect. 4. HST photometry of NGC 6397 produces a remarkably clean H ...
Galactic chemical evolution of heavy elements: from Barium to
... from detailed nucleosynthesis calculations based on TP-AGB models for different masses and metallicities, with updated reaction networks and neutron capture cross sections. In addition, as anticipated by Truran (1981), at low metallicities the r-process contribution to the various elements becomes d ...
... from detailed nucleosynthesis calculations based on TP-AGB models for different masses and metallicities, with updated reaction networks and neutron capture cross sections. In addition, as anticipated by Truran (1981), at low metallicities the r-process contribution to the various elements becomes d ...
Two distinct sequences of blue straggler stars in the globular cluster
... Creek ACT 2611, Australia Stars in globular clusters are generally believed to have all formed at the same time, early in the Galaxy's history1. 'Blue stragglers' are stars sufficiently massive2 that they should have evolved into white dwarfs long ago. Two possible mechanisms have been proposed for ...
... Creek ACT 2611, Australia Stars in globular clusters are generally believed to have all formed at the same time, early in the Galaxy's history1. 'Blue stragglers' are stars sufficiently massive2 that they should have evolved into white dwarfs long ago. Two possible mechanisms have been proposed for ...
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 ...
Tidal interaction of a rotating 1 vec {M_sun} star with a - UvA-DARE
... perturbations are complex-valued which expresses the induced phase-lags with respect to the companion. Although the energy equation is not separable, we have nevertheless simply replaced the n(n + 1) factor in the energy equation for a non-rotating star by λn (Eq. (15)) to approximately take the hor ...
... perturbations are complex-valued which expresses the induced phase-lags with respect to the companion. Although the energy equation is not separable, we have nevertheless simply replaced the n(n + 1) factor in the energy equation for a non-rotating star by λn (Eq. (15)) to approximately take the hor ...
Three-dimensional simulations of the upper
... and of the motions in the atmosphere, the determination of abundances and other physical conditions can also be affected (Dravins & Nordlund 1990a,b; Asplund et al. 2000; Steffen & Holweger 2002). This paper describes physically realistic convection in the Sun and at two points along its future evol ...
... and of the motions in the atmosphere, the determination of abundances and other physical conditions can also be affected (Dravins & Nordlund 1990a,b; Asplund et al. 2000; Steffen & Holweger 2002). This paper describes physically realistic convection in the Sun and at two points along its future evol ...