Stellar evolution models for Z = 0.0001 to 0.03
... Indeed, convection is by far the most efficient means of energy transfer in a star, except very close to the photosphere. Stars with effective temperatures Teff # 6500 K develop deep outer convection zones, and the model parameters Teff and radius depend strongly on the representation of this convec ...
... Indeed, convection is by far the most efficient means of energy transfer in a star, except very close to the photosphere. Stars with effective temperatures Teff # 6500 K develop deep outer convection zones, and the model parameters Teff and radius depend strongly on the representation of this convec ...
Stellar evolution models for Z = 0.0001 to 0.03
... Indeed, convection is by far the most efficient means of energy transfer in a star, except very close to the photosphere. Stars with effective temperatures Teff # 6500 K develop deep outer convection zones, and the model parameters Teff and radius depend strongly on the representation of this convec ...
... Indeed, convection is by far the most efficient means of energy transfer in a star, except very close to the photosphere. Stars with effective temperatures Teff # 6500 K develop deep outer convection zones, and the model parameters Teff and radius depend strongly on the representation of this convec ...
Oscillation Modes of Strange Quark Stars with a Strangelet Crust
... form a mixed phase. This model has the advantage that it reduces the density gradient near the crust and produces negligible electric field energy at the stars surface. However, there will be short-range (screened) electric fields inside the mixed phase, which can be tolerated if the Gibbs free ener ...
... form a mixed phase. This model has the advantage that it reduces the density gradient near the crust and produces negligible electric field energy at the stars surface. However, there will be short-range (screened) electric fields inside the mixed phase, which can be tolerated if the Gibbs free ener ...
THE FINAL FATE OF STARS THAT IGNITE NEON AND OXYGEN
... models of 8–12 M stars which suggest that there could be an evolutionary channel producing EC-SNe in addition to superAGB stars. These stars would be the most massive progenitors of EC-SNe and would ignite neon and oxygen burning offcenter where the maximum temperature has moved outward as neutrino ...
... models of 8–12 M stars which suggest that there could be an evolutionary channel producing EC-SNe in addition to superAGB stars. These stars would be the most massive progenitors of EC-SNe and would ignite neon and oxygen burning offcenter where the maximum temperature has moved outward as neutrino ...
Metallicity, Age, and Mass of Star Forming Galaxies at z~3
... Yet, with some exceptions (see next viewgraph) Lyα from possible proto galaxies is rarely detected in deep narrow band searches (Thompson etal 1995; Stern & Spinrad, 1999, PASP, 111, 1475) This implies that the galaxies are obscured by dust. ...
... Yet, with some exceptions (see next viewgraph) Lyα from possible proto galaxies is rarely detected in deep narrow band searches (Thompson etal 1995; Stern & Spinrad, 1999, PASP, 111, 1475) This implies that the galaxies are obscured by dust. ...
Star counts in the Galaxy-Simulating from very deep to very shallow
... composition, etc.) as a function of initial mass Mi , stellar age τ, and metallicity Z; 2. tables of bolometric corrections BCλi for the several filter pass-bands λi , as a function of T eff , log g, and [M/H], as well as the relative absorption in the several passbands with respect to V, Aλi /AV ; 3 ...
... composition, etc.) as a function of initial mass Mi , stellar age τ, and metallicity Z; 2. tables of bolometric corrections BCλi for the several filter pass-bands λi , as a function of T eff , log g, and [M/H], as well as the relative absorption in the several passbands with respect to V, Aλi /AV ; 3 ...
Potassium abundances in nearby metal-poor stars
... Aims. The potassium abundances for 58 metal-poor stars are determined using high-resolution spectroscopy. The abundance trends in stars of different population are discussed. Methods. All abundance results have been derived from NLTE statistical equilibrium calculations and spectrum synthesis methods ...
... Aims. The potassium abundances for 58 metal-poor stars are determined using high-resolution spectroscopy. The abundance trends in stars of different population are discussed. Methods. All abundance results have been derived from NLTE statistical equilibrium calculations and spectrum synthesis methods ...
THE KEPLER CLUSTER STUDY: STELLAR ROTATION IN NGC 6811
... for its application to determine stellar ages from measurements of colors and rotation periods (gyrochronology; Barnes 2003, 2007; Mamajek & Hillenbrand 2008; Soderblom 2010). The thinner the surface the more precisely a gyrochronology age of a star can be determined. Knowing stellar ages is fundame ...
... for its application to determine stellar ages from measurements of colors and rotation periods (gyrochronology; Barnes 2003, 2007; Mamajek & Hillenbrand 2008; Soderblom 2010). The thinner the surface the more precisely a gyrochronology age of a star can be determined. Knowing stellar ages is fundame ...
Quantitative evidence of an intrinsic luminosity spread in the Orion
... we list the ACS filters, their ground-based telescope equivalents, and the duration of individual exposures. The complete ACS/WFC catalog for the ONC includes ∼3200 sources (Robberto, in prep.) that have been classified as either a single star, binary star, photo-evaporated disk, dark silhouette, or ...
... we list the ACS filters, their ground-based telescope equivalents, and the duration of individual exposures. The complete ACS/WFC catalog for the ONC includes ∼3200 sources (Robberto, in prep.) that have been classified as either a single star, binary star, photo-evaporated disk, dark silhouette, or ...
Three-dimensional simulations of the atmosphere of an AGB star
... Department of Astronomy and Space Physics, Uppsala University, Sweden ...
... Department of Astronomy and Space Physics, Uppsala University, Sweden ...
THE MYSTERIOUS SICKLE OBJECT IN THE CARINA NEBULA: A
... this data set) clearly reveals a compact clump located close to the tip of the Sickle. The position of the peak of the sub-mm emission is 10h 44m 04.06s , −59◦ 33′ 35.5′′ , i.e. 10 arcseconds (or 0.1 pc) north-west of the star MJ 218 and about 3 arcseconds north-west of the apex point of the Sickle ...
... this data set) clearly reveals a compact clump located close to the tip of the Sickle. The position of the peak of the sub-mm emission is 10h 44m 04.06s , −59◦ 33′ 35.5′′ , i.e. 10 arcseconds (or 0.1 pc) north-west of the star MJ 218 and about 3 arcseconds north-west of the apex point of the Sickle ...
The fundamental parameters of the roAp star γ Equulei
... opposite profile since their abundance is more than 6 dex higher in the upper layers than in the deeper atmospheric ones. Such abundance inhomogeneities clearly lead to a patchy surface, a redistribution of the stellar flux, and a complex atmospheric structure, resulting in biased photometric and sp ...
... opposite profile since their abundance is more than 6 dex higher in the upper layers than in the deeper atmospheric ones. Such abundance inhomogeneities clearly lead to a patchy surface, a redistribution of the stellar flux, and a complex atmospheric structure, resulting in biased photometric and sp ...
Winds of Main-Sequence Stars - Harvard
... Solar X-rays & magnetic flux • Empirically, does solar mass loss really scale with FX ~ Φ ? It depends on which field lines are considered! ...
... Solar X-rays & magnetic flux • Empirically, does solar mass loss really scale with FX ~ Φ ? It depends on which field lines are considered! ...
16.1 A Little History
... is actually converted into the kinetic energy of the envelope—that is the actual mechanics of the explosion of a massive star—turns out to be a very difficult problem that has been the subject of intense theoretical activity in the modern computational era. ...
... is actually converted into the kinetic energy of the envelope—that is the actual mechanics of the explosion of a massive star—turns out to be a very difficult problem that has been the subject of intense theoretical activity in the modern computational era. ...
Study of an unbiased sample of B stars observed with Hipparcos
... show α Cyg-type variability with respect to pulsators of which we know the cause of the pulsations. The Hipparcos sample of B-type variable stars offers the possibility to do this. A caveat to place the supergiants in the HR diagram is that their temperature and luminosity are difficult to determine ...
... show α Cyg-type variability with respect to pulsators of which we know the cause of the pulsations. The Hipparcos sample of B-type variable stars offers the possibility to do this. A caveat to place the supergiants in the HR diagram is that their temperature and luminosity are difficult to determine ...
Period Changes of Delta Scuti Stars and Stellar Evolution
... we constructed envelope models using global stellar parameters (mass, effective temperature and luminosity) along the evolutionary tracks computed by D’Antona & Mazzitelli (1994), and then computed radial oscillations of these models. The envelopes were integrated from the surface to a layer with tem ...
... we constructed envelope models using global stellar parameters (mass, effective temperature and luminosity) along the evolutionary tracks computed by D’Antona & Mazzitelli (1994), and then computed radial oscillations of these models. The envelopes were integrated from the surface to a layer with tem ...
Neutron stars: compact objects with relativistic gravity
... 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 hope to provide even more stringent tests of general relativity by measuring mass and radius of neutron stars. This is hampered by the fact that the mass and radius ...
... 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 hope to provide even more stringent tests of general relativity by measuring mass and radius of neutron stars. This is hampered by the fact that the mass and radius ...
Stars in the Sky Stars in the Sky
... This is called the Doppler effect. It works with both sound and light. As a light source moves away quickly, its light looks redder. This particular Doppler effect is called red shift. The farther apart two galaxies are moving, the faster the galaxies are moving apart. From the perspective of each g ...
... This is called the Doppler effect. It works with both sound and light. As a light source moves away quickly, its light looks redder. This particular Doppler effect is called red shift. The farther apart two galaxies are moving, the faster the galaxies are moving apart. From the perspective of each g ...
Formation of Massive Stars
... • Massive stars are expected to modify their environment soon after a stellar core has formed since their Kelvin-Helmholtz time scale (< 104 yrs for an O star) is short ( tKH = E/L ~ GM2/LR) (Shu et al. 1987 AARA 25 23) ...
... • Massive stars are expected to modify their environment soon after a stellar core has formed since their Kelvin-Helmholtz time scale (< 104 yrs for an O star) is short ( tKH = E/L ~ GM2/LR) (Shu et al. 1987 AARA 25 23) ...
Notes on Stars
... of the Balmer line strengths along the Harvard sequence? As the excitation occurs from the n = 2 state, the temperature has to be high enough to populate this level. This is the case for most of the stars. The n = 2 level will become more and more populated if we pass from K stars to A stars, as wit ...
... of the Balmer line strengths along the Harvard sequence? As the excitation occurs from the n = 2 state, the temperature has to be high enough to populate this level. This is the case for most of the stars. The n = 2 level will become more and more populated if we pass from K stars to A stars, as wit ...
Oxygen isotopes in circumstellar Al_2O_3 grains from meteorites
... OXYGEN ISOTOPES IN CIRCUMSTELLAR Al 2 0 3 GRAINS FROM METEORITES ...
... OXYGEN ISOTOPES IN CIRCUMSTELLAR Al 2 0 3 GRAINS FROM METEORITES ...
Toward $ ab\, initio $ extremely metal poor stars
... formation enriched by a single, low-energy Pop III supernova. We present an ab initio cosmological hydrodynamical simulation involving a single Pop III supernova with a low explosion energy of 1051 erg, proceeding until a metal-enriched pre-stellar core has formed in the cosmological box and the con ...
... formation enriched by a single, low-energy Pop III supernova. We present an ab initio cosmological hydrodynamical simulation involving a single Pop III supernova with a low explosion energy of 1051 erg, proceeding until a metal-enriched pre-stellar core has formed in the cosmological box and the con ...
Chemical tagging of three distinct populations of red giants in the
... Na-O anticorrelation, is quite clear when Al abundances are considered. These results tell us that in NGC 6752 the interplay between star formation and dilution with pristine material acted so that two groups of stars with rather homogeneous chemical composition stand out. Thus, any mechanism result ...
... Na-O anticorrelation, is quite clear when Al abundances are considered. These results tell us that in NGC 6752 the interplay between star formation and dilution with pristine material acted so that two groups of stars with rather homogeneous chemical composition stand out. Thus, any mechanism result ...
laboratory analysis of presolar silicate stardust from a
... Refractory dust grains with highly anomalous isotopic compositions are found in small quantities in primitive meteorites, interplanetary dust particles, and cometary matter (e.g., Zinner 2007; Hoppe 2008). These “presolar” grains have formed in the winds of evolved stars or in the ejecta of stellar ...
... Refractory dust grains with highly anomalous isotopic compositions are found in small quantities in primitive meteorites, interplanetary dust particles, and cometary matter (e.g., Zinner 2007; Hoppe 2008). These “presolar” grains have formed in the winds of evolved stars or in the ejecta of stellar ...
Article PDF - IOPscience
... the simulations were run with the binary parameters turned off. Since for this study we required detailed information regarding the companion stars and their orbital properties, these were added after the fact as follows. From the TRILEGAL output, we constructed a distance-limited sample with maximu ...
... the simulations were run with the binary parameters turned off. Since for this study we required detailed information regarding the companion stars and their orbital properties, these were added after the fact as follows. From the TRILEGAL output, we constructed a distance-limited sample with maximu ...