The effect of stellar limb darkening values on the accuracy of the
... the previous section, we can easily conclude that the uncertainties in the relative radius ratio of the planet and the star varies between 1% and 10%, but it can be around 8% at the high temperature. Below 5000 K, where the curves of different theories are very divergent, we have uncertainties of up ...
... the previous section, we can easily conclude that the uncertainties in the relative radius ratio of the planet and the star varies between 1% and 10%, but it can be around 8% at the high temperature. Below 5000 K, where the curves of different theories are very divergent, we have uncertainties of up ...
Thesis (complete) - Research Explorer
... mass star with M ∼ 0.8 M⋆ to higher mass stars with M ≥ 2 M⋆ . For stars with masses about that of the Sun, the proton-proton (pp) chain dominates the energy production on the main sequence. For stars more massive than about 2 M⊙ , the CNO-cycle is responsible for most of the energy produced. The pr ...
... mass star with M ∼ 0.8 M⋆ to higher mass stars with M ≥ 2 M⋆ . For stars with masses about that of the Sun, the proton-proton (pp) chain dominates the energy production on the main sequence. For stars more massive than about 2 M⊙ , the CNO-cycle is responsible for most of the energy produced. The pr ...
Galaxies in the Universe: An Introduction, Second Edition
... We have tried to place material which is relatively more difficult or more intricate at the end of each subsection. Students who find some portions heavy going at a first reading are advised to move to the following subsection and return later to the troublesome passage. Some problems have been include ...
... We have tried to place material which is relatively more difficult or more intricate at the end of each subsection. Students who find some portions heavy going at a first reading are advised to move to the following subsection and return later to the troublesome passage. Some problems have been include ...
submillimeter observations of giant molecular clouds in the large
... emission is sensitive to and is well correlated with the local H flux. We infer that differences of clump properties represent an evolutionary sequence of GMCs in terms of density increase leading to star formation. Type I and II GMCs (starless GMCs and GMCs with H ii regions only, respectively) ar ...
... emission is sensitive to and is well correlated with the local H flux. We infer that differences of clump properties represent an evolutionary sequence of GMCs in terms of density increase leading to star formation. Type I and II GMCs (starless GMCs and GMCs with H ii regions only, respectively) ar ...
X-ray binaries in the Milky Way and other galaxies
... 4.1. Comparison of the differential Log(N)–Log(S) relation for Galactic XRBs from ASM and ASCA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.2. Comparison of the number-flux relation observed in the ASCA GRS and the predicted Log(N)–Log(S) from ASM luminosity functions. . . . . . . . . ...
... 4.1. Comparison of the differential Log(N)–Log(S) relation for Galactic XRBs from ASM and ASCA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4.2. Comparison of the number-flux relation observed in the ASCA GRS and the predicted Log(N)–Log(S) from ASM luminosity functions. . . . . . . . . ...
The white dwarf luminosity function
... mechanisms operating in the envelopes of white dwarfs, such as gravitational settling, thermal diffusion, radiative levitation, convection at the H-He and He-core interfaces, proton burning, stellar winds and mass accretion from the interstellar medium. These interesting topics are, however, out of ...
... mechanisms operating in the envelopes of white dwarfs, such as gravitational settling, thermal diffusion, radiative levitation, convection at the H-He and He-core interfaces, proton burning, stellar winds and mass accretion from the interstellar medium. These interesting topics are, however, out of ...
The effect of dark matter capture on binary stars
... This work has led to a number of interesting conclusions: (1) Binary stars, due to their orbital motion, can produce more collisions that result in initially bound orbits. However, the gravitational interaction with two masses quickly scatters nearly all WIMPs out of the system. The few that survive ...
... This work has led to a number of interesting conclusions: (1) Binary stars, due to their orbital motion, can produce more collisions that result in initially bound orbits. However, the gravitational interaction with two masses quickly scatters nearly all WIMPs out of the system. The few that survive ...
Full Text - Digital Access to Scholarship at Harvard
... has a broad range of energy levels and can interact with light over much of a star’s spectrum, whereas atomic hydrogen gas, for instance, can interact with light primarily only within a few lines for all wavelengths longward of ionizing hydrogen. Because of this, about 30% of the light leaving the G ...
... has a broad range of energy levels and can interact with light over much of a star’s spectrum, whereas atomic hydrogen gas, for instance, can interact with light primarily only within a few lines for all wavelengths longward of ionizing hydrogen. Because of this, about 30% of the light leaving the G ...
Full Text - University of Toronto Astronomy
... literature and to study limb-darkening for stars with low gravity. It is determined that stellar limb-darkening can be used to constrain fundamental properties of stars. When this is coupled with interferometric or microlensing observations, stellar limb-darkening can predict the masses of isolated ...
... literature and to study limb-darkening for stars with low gravity. It is determined that stellar limb-darkening can be used to constrain fundamental properties of stars. When this is coupled with interferometric or microlensing observations, stellar limb-darkening can predict the masses of isolated ...
Link - Max-Planck-Institut für Astronomie
... the star formation community. It is now viewed as a common, though still poorly understood, phenomenon in low-mass star formation. The FU Orionis objects (FUors) are long-studied examples of this phenomenon. FUors are believed to undergo accretion outbursts during which the accretion rate rapidly in ...
... the star formation community. It is now viewed as a common, though still poorly understood, phenomenon in low-mass star formation. The FU Orionis objects (FUors) are long-studied examples of this phenomenon. FUors are believed to undergo accretion outbursts during which the accretion rate rapidly in ...
arXiv:1410.8731v2 [astro
... 2014). By now the object is expected to have passed through its peribothron and tidal disruption as well as intense accretion events have been predicted. Eckart et al. (2013) show a possible spectral decomposition of this source using the M-band measurement by Gillessen et al. (2012). Depending on t ...
... 2014). By now the object is expected to have passed through its peribothron and tidal disruption as well as intense accretion events have been predicted. Eckart et al. (2013) show a possible spectral decomposition of this source using the M-band measurement by Gillessen et al. (2012). Depending on t ...
The 3-D shaping of NGC 6741: a massive, fast
... valid for the reduction and investigation methods: so far long-slit echellograms have been used to obtain, either the kinematics in a few ions (in general, [O III], H I and [N II]), or the “average” nebular properties (physical conditions, ionic and chemical abundances) integrated over the whole sli ...
... valid for the reduction and investigation methods: so far long-slit echellograms have been used to obtain, either the kinematics in a few ions (in general, [O III], H I and [N II]), or the “average” nebular properties (physical conditions, ionic and chemical abundances) integrated over the whole sli ...
Full Text
... N.1 Inleiding . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . N.1.1 Sterpopulaties . . . . . . . . . . . . . . . . . . . . . . . . . . . N.1.2 AGB sterren . . . . . . . . . . . . . . . . . . . . . . . . . . . N.1.2.1 Pre-AGB evolutie . . . . . . . . . . . . . . . . . . . N.1.2.2 ...
... N.1 Inleiding . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . N.1.1 Sterpopulaties . . . . . . . . . . . . . . . . . . . . . . . . . . . N.1.2 AGB sterren . . . . . . . . . . . . . . . . . . . . . . . . . . . N.1.2.1 Pre-AGB evolutie . . . . . . . . . . . . . . . . . . . N.1.2.2 ...
Cepheids
... HIPPARCOS catalogue and the distance to the LMC” (A&A V.356, P.849, 2000) • A.Sandage et al. “The Hubble constant: a summary of the HST program for the luminosity calibration of type Ia SuperNovae by means of Cepheids” (ApJ V.653, P.843, 2006) • F.van Leeuwen et al. “Cepheid parallaxes and the Hubbl ...
... HIPPARCOS catalogue and the distance to the LMC” (A&A V.356, P.849, 2000) • A.Sandage et al. “The Hubble constant: a summary of the HST program for the luminosity calibration of type Ia SuperNovae by means of Cepheids” (ApJ V.653, P.843, 2006) • F.van Leeuwen et al. “Cepheid parallaxes and the Hubbl ...
Population effects on the red giant clump absolute magnitude, and
... however, depends on the possible presence of systematic magnitude differences DM RC I between the local clump revealed by the Hipparcos colour±magnitude diagram (CMD), and the clump stars observed in distant galaxies. In this paper, we re-address the problem of these systematic `population' effec ...
... however, depends on the possible presence of systematic magnitude differences DM RC I between the local clump revealed by the Hipparcos colour±magnitude diagram (CMD), and the clump stars observed in distant galaxies. In this paper, we re-address the problem of these systematic `population' effec ...
Cool Subdwarf Investigations (CSI) I: New Thoughts for the Spectral
... Figure 3 shows TiO5 plotted against CaH1 and CaH2+CaH3 for various samples of stars. Our subdwarfs are shown with solid circles. For comparison, small dots indicate main sequence stars from Hawley et al. (1996), while open triangles and squares represent subdwarfs and “extreme” subdwarfs from Gizis ...
... Figure 3 shows TiO5 plotted against CaH1 and CaH2+CaH3 for various samples of stars. Our subdwarfs are shown with solid circles. For comparison, small dots indicate main sequence stars from Hawley et al. (1996), while open triangles and squares represent subdwarfs and “extreme” subdwarfs from Gizis ...
The 3-D shaping of NGC 6741: A massive, fast
... Abstract. We infer the gas kinematics, diagnostics and ionic radial profiles, distance and central star parameters, nebular photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position an ...
... Abstract. We infer the gas kinematics, diagnostics and ionic radial profiles, distance and central star parameters, nebular photo-ionization model, spatial structure and evolutionary phase of the Planetary Nebula NGC 6741 by means of long-slit ESO NTT+EMMI high-resolution spectra at nine position an ...
Oxygen, magnesium and chromium isotopic ratios of
... (LL3.0), Bishunpur (LL3.1) and Krymka (LL3.1), prepared using methods similar to those for the Murray residue. These grains ranged in size from 0.3 to 2 m and were identified as presolar by automated O isotopic analysis of all three O isotopes in the Carnegie ims-6f ion microprobe (Nittler and Alex ...
... (LL3.0), Bishunpur (LL3.1) and Krymka (LL3.1), prepared using methods similar to those for the Murray residue. These grains ranged in size from 0.3 to 2 m and were identified as presolar by automated O isotopic analysis of all three O isotopes in the Carnegie ims-6f ion microprobe (Nittler and Alex ...
Giant Molecular Clouds in Local Group Galaxies
... and beyond. An exhaustive list of their efforts is beyond the scope of the present article. The situation has changed in the last five years as a result of the construction of the NANTEN telescope in the Southern Hemisphere and the completion of the 10-element BIMA Array. The former made it possible ...
... and beyond. An exhaustive list of their efforts is beyond the scope of the present article. The situation has changed in the last five years as a result of the construction of the NANTEN telescope in the Southern Hemisphere and the completion of the 10-element BIMA Array. The former made it possible ...
Stars and dust in the Galactic Center
... Binwise median and maximum three-dimensional velocity . . . . Binwise maximum of the minimum binding mass . . . . . . . . . Distance constraints from stars that are close to escaping . . . . Velocity histograms of our dynamics sample . . . . . . . . . . . Fits of the dispersion in the inner 25′′ by ...
... Binwise median and maximum three-dimensional velocity . . . . Binwise maximum of the minimum binding mass . . . . . . . . . Distance constraints from stars that are close to escaping . . . . Velocity histograms of our dynamics sample . . . . . . . . . . . Fits of the dispersion in the inner 25′′ by ...
VLA OBSERVATIONS OF AMMONIA IN HIGH
... three sub-classes in the sample: filaments, hot cores, and NH3 dispersed sources. The ubiquitous gas filaments found on 1 pc scales have a typical width of ∼0.1 pc and often contain regularly spaced fragments along the major axis. The spacing of the fragments and the column densities are consistent ...
... three sub-classes in the sample: filaments, hot cores, and NH3 dispersed sources. The ubiquitous gas filaments found on 1 pc scales have a typical width of ∼0.1 pc and often contain regularly spaced fragments along the major axis. The spacing of the fragments and the column densities are consistent ...
Radiation-driven wind models of massive stars
... dynamical role, as they are responsible for a large amount of momentum and energy input into the ISM due to stellar winds and supernova explosions. See Abbott (1982b) and Leitherer et al. (1992) for an overview. Moreover, as massive stars are hot, with effective temperatures in the range of about 10 ...
... dynamical role, as they are responsible for a large amount of momentum and energy input into the ISM due to stellar winds and supernova explosions. See Abbott (1982b) and Leitherer et al. (1992) for an overview. Moreover, as massive stars are hot, with effective temperatures in the range of about 10 ...
Testing the Initial-Final Mass Relationship of White Dwarfs Silvia Catal´ an Ruiz
... total age or metallicity, are available. Most of the works carried out up to now 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 t ...
... total age or metallicity, are available. Most of the works carried out up to now 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 t ...
Decoding Galaxy Evolution with Gas
... long-lived asymptotic giant branch stars that is absent from the bulge PC2 because of rapid bulge formation. Detailed interpretations of stellar abundance patterns require chemical evolution modeling, but these models are sensitive to the treatment of star formation efficiency (SFE), outflow, stellar y ...
... long-lived asymptotic giant branch stars that is absent from the bulge PC2 because of rapid bulge formation. Detailed interpretations of stellar abundance patterns require chemical evolution modeling, but these models are sensitive to the treatment of star formation efficiency (SFE), outflow, stellar y ...
Models for circumstellar nebulae around red and blue supergiants
... Stars spend most of their life in the Main Sequence (MS). In this stage of their evolution the source of energy production is the fusion of hydrogen into helium in their core. This energy escapes from the star in the form of radiation and, to a minor fraction, in the form of stellar wind. Depending ...
... Stars spend most of their life in the Main Sequence (MS). In this stage of their evolution the source of energy production is the fusion of hydrogen into helium in their core. This energy escapes from the star in the form of radiation and, to a minor fraction, in the form of stellar wind. Depending ...