Dust formation in the winds of AGBs: the contribution at low
... At lower stellar masses (<8 M ) grain condensation occurs during the AGB and super-AGB phases and the resulting dust mass depends on the progenitor stellar mass and metallicity through complex processes which affect the chemical composition and physical conditions in the stellar atmospheres. Previo ...
... At lower stellar masses (<8 M ) grain condensation occurs during the AGB and super-AGB phases and the resulting dust mass depends on the progenitor stellar mass and metallicity through complex processes which affect the chemical composition and physical conditions in the stellar atmospheres. Previo ...
The spectroscopic Hertzsprung-Russell diagram
... Results. Observed stars can be as conveniently compared to stellar evolution calculations in the sHR diagram as in the HertzsprungRussell diagram. However, at the same time, our ordinate is proportional to the stellar mass-to-luminosity ratio, which can thus be directly determined. For intermediate ...
... Results. Observed stars can be as conveniently compared to stellar evolution calculations in the sHR diagram as in the HertzsprungRussell diagram. However, at the same time, our ordinate is proportional to the stellar mass-to-luminosity ratio, which can thus be directly determined. For intermediate ...
Helium - Boreal Science
... in the universe. Only Hydrogen is more abundant! These two elements were copiously formed during the creation of the universe. In the early stages of the universe, helium and hydrogen nuclei were actually formed. No atoms were formed until about 300,000 years after the Big Bang took place, when the ...
... in the universe. Only Hydrogen is more abundant! These two elements were copiously formed during the creation of the universe. In the early stages of the universe, helium and hydrogen nuclei were actually formed. No atoms were formed until about 300,000 years after the Big Bang took place, when the ...
SPIRou Science Case
... for studying Earth-mass rocky planets, in particular those located within the habitable zones (HZs) of their host stars, i.e., in the orbital range where liquid water can be stable at the planetary surfaces. Identifying habitable Earth-like planets and searching for biomarkers in their atmospheres i ...
... for studying Earth-mass rocky planets, in particular those located within the habitable zones (HZs) of their host stars, i.e., in the orbital range where liquid water can be stable at the planetary surfaces. Identifying habitable Earth-like planets and searching for biomarkers in their atmospheres i ...
PowerPoint Presentation - Isolated Neutron Stars, solid crust
... Osservatorio Astronomico di Roma, 9-11 Dicembre 2003 ...
... Osservatorio Astronomico di Roma, 9-11 Dicembre 2003 ...
Teaching Tips Table of Contents - Hubble Deep Field
... 5. How was the area covered by the Hubble Deep Fields selected? ............................. 37 6. How long did it take the Hubble Space Telescope to obtain the HDF-N image? ....... 38 7. What is a galaxy? ............................................................................................. ...
... 5. How was the area covered by the Hubble Deep Fields selected? ............................. 37 6. How long did it take the Hubble Space Telescope to obtain the HDF-N image? ....... 38 7. What is a galaxy? ............................................................................................. ...
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 ...
Distance determination for RAVE stars using stellar models
... mass in nebulae. By this definition dark matter does not interact with normal matter through the electro-magnetic force, but does interact through the gravitational force. This popular and successful cosmological picture is referred to as ΛCDM cosmology and predicts a hierarchical formation of struc ...
... mass in nebulae. By this definition dark matter does not interact with normal matter through the electro-magnetic force, but does interact through the gravitational force. This popular and successful cosmological picture is referred to as ΛCDM cosmology and predicts a hierarchical formation of struc ...
1. INTRODUCTION - Institut für Theoretische Astrophysik
... of hydrogen are also important (see, e.g., Kneer 1980 ; Carlsson & Stein 1992, 1995) but have not been included either. Interestingly, both approximations are expected to change the thermal structure of the atmospheres in opposite directions : ignoring the ionization energy of hydrogen in the energy ...
... of hydrogen are also important (see, e.g., Kneer 1980 ; Carlsson & Stein 1992, 1995) but have not been included either. Interestingly, both approximations are expected to change the thermal structure of the atmospheres in opposite directions : ignoring the ionization energy of hydrogen in the energy ...
Clusters as laboratories for the study of galaxy evolution
... Velocity dispersions and optical photometry for 21 “early-type” galaxies in the Groth strip. “The difference in the degree of evolution between our field sample and published cluster galaxies suggests a more recent formation epoch, around z=1.5 for field galaxies compared to z>2.0 for cluster galaxi ...
... Velocity dispersions and optical photometry for 21 “early-type” galaxies in the Groth strip. “The difference in the degree of evolution between our field sample and published cluster galaxies suggests a more recent formation epoch, around z=1.5 for field galaxies compared to z>2.0 for cluster galaxi ...
Test 3 Review Clicker Questions
... layers above the core. They gradually shift in spectrum to visible and infrared light at the ...
... layers above the core. They gradually shift in spectrum to visible and infrared light at the ...
Direct Imaging Searches Around White Dwarfs - X
... • Original orbit ~2AU (max extent of AGB envelope) • WD progenitor 3.5Msun/B9V ...
... • Original orbit ~2AU (max extent of AGB envelope) • WD progenitor 3.5Msun/B9V ...
Camelopardalis-Better-Know-A-Constellation
... deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnitudes 4.0 and 7.4. • The second brightest is CS Camelopardalis, which h ...
... deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnitudes 4.0 and 7.4. • The second brightest is CS Camelopardalis, which h ...
The Gould Belt
... galaxy by 30ўX. The Local stellar system has no effect on the motion of stars at distances greater than 300 pc from the sun. The idea of the Supercluster was developed by Eggen [52,53], who combines several fairly young clusters into the Pleiades group (age 100–150 million years) based on the closen ...
... galaxy by 30ўX. The Local stellar system has no effect on the motion of stars at distances greater than 300 pc from the sun. The idea of the Supercluster was developed by Eggen [52,53], who combines several fairly young clusters into the Pleiades group (age 100–150 million years) based on the closen ...
Theoretical Predictions for Mass Loss Rates: Rotation & Pulsation
... What sets the Sun’s mass loss? • Coronal heating must be ultimately responsible. ...
... What sets the Sun’s mass loss? • Coronal heating must be ultimately responsible. ...
PDF - Department of Statistics
... the arithmetic mean and standard deviation in order to guard against occultations and aberrant outliers. Let Yksh denote the resulting test statistic for hold h of star s on telescope k. We now describe a test based on measurements at multiple telescopes which flags a star-hold if Yksh is sufficient ...
... the arithmetic mean and standard deviation in order to guard against occultations and aberrant outliers. Let Yksh denote the resulting test statistic for hold h of star s on telescope k. We now describe a test based on measurements at multiple telescopes which flags a star-hold if Yksh is sufficient ...
Stars Evolution of High Mass Stars Nucleosynthesis Supernovae
... • A star’s mass determines its entire life story because it determines its core temperature. • High-mass stars have short lives, eventually becoming hot enough to make iron, and end in ...
... • A star’s mass determines its entire life story because it determines its core temperature. • High-mass stars have short lives, eventually becoming hot enough to make iron, and end in ...
High precision effective temperatures for 181 F-
... of metallicity. As to the effect of rotation, we should note that all objects in our sample are old Main Sequence stars with slow to negligible rotation (vsini<15 km s−1 ), which is comparable to the instrumental broadening. Thus, we initially selected about 600 pairs of 256 unblended SiI, TiI, VI, ...
... of metallicity. As to the effect of rotation, we should note that all objects in our sample are old Main Sequence stars with slow to negligible rotation (vsini<15 km s−1 ), which is comparable to the instrumental broadening. Thus, we initially selected about 600 pairs of 256 unblended SiI, TiI, VI, ...
Element Segregation in Low Metallicity Stars and the Primordial
... star. This result leads to the idea that the observed lithium abundances may be related to this maximum value. When VC95 computed the effect of mass loss on the lithium abundances in Pop II stars, they found the following characteristic behavior : for very small mass loss rates, the surface lithium ...
... star. This result leads to the idea that the observed lithium abundances may be related to this maximum value. When VC95 computed the effect of mass loss on the lithium abundances in Pop II stars, they found the following characteristic behavior : for very small mass loss rates, the surface lithium ...
THE MORPHOLOGICAL DEMOGRAPHICS OF GALAXIES IN THE
... The archeological nature of galaxy evolution studies prevents us from following individual galaxies over time. In consequence we are only left with snapshots at different lookback times from where we attempt, as excavators, to piece together their evolutionary histories from the motion of different ...
... The archeological nature of galaxy evolution studies prevents us from following individual galaxies over time. In consequence we are only left with snapshots at different lookback times from where we attempt, as excavators, to piece together their evolutionary histories from the motion of different ...
Program and Abstract Book - European Southern Observatory
... Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass both accretes from the core onto a protostar, likely through an accretion disk, and is ejected in the form of jets and outflows. It is during this protostellar phase that the initial masses of ...
... Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass both accretes from the core onto a protostar, likely through an accretion disk, and is ejected in the form of jets and outflows. It is during this protostellar phase that the initial masses of ...