The importance of radiative feedback for the stellar initial mass
... Whereas star formation in the barotropic simulations continued unabated until the simulations stopped, we find that radiative feedback, even from low-mass stars, were essentially terminates the production of new objects within low-mass dense molecular cloud cores after roughly one local dynamical ti ...
... Whereas star formation in the barotropic simulations continued unabated until the simulations stopped, we find that radiative feedback, even from low-mass stars, were essentially terminates the production of new objects within low-mass dense molecular cloud cores after roughly one local dynamical ti ...
Evolution of the barium abundance in the early Galaxy from a NLTE
... result of the experimental fitting of the barium lines in solar spectrum. Collisions with atomic hydrogen for the forbidden transitions were not taken into account, but we checked that the resulting uncertainty about the equivalent width of the lines, computed by the method of Takeda (1991), does no ...
... result of the experimental fitting of the barium lines in solar spectrum. Collisions with atomic hydrogen for the forbidden transitions were not taken into account, but we checked that the resulting uncertainty about the equivalent width of the lines, computed by the method of Takeda (1991), does no ...
A Detailed Spectroscopic and Photometric Analysis of DQ White
... As discussed in the Introduction, the presence of carbon not only produces the strong atomic and molecular absorption features shown in Figure 2, but it also contributes to increase the number of free electrons, and thus the He− free-free opacity. The resulting effect of carbon on the atmospheric st ...
... As discussed in the Introduction, the presence of carbon not only produces the strong atomic and molecular absorption features shown in Figure 2, but it also contributes to increase the number of free electrons, and thus the He− free-free opacity. The resulting effect of carbon on the atmospheric st ...
The rebirth of Supernova 1987A a study of the ejecta-ring collision
... Supernovae are some of the most energetic phenomena in the Universe and they have throughout history fascinated people as they appeared as new stars in the sky. Supernova (SN) 1987A exploded in the nearby satellite galaxy, the Large Magellanic Cloud (LMC), at a distance of only 168 000 light years. ...
... Supernovae are some of the most energetic phenomena in the Universe and they have throughout history fascinated people as they appeared as new stars in the sky. Supernova (SN) 1987A exploded in the nearby satellite galaxy, the Large Magellanic Cloud (LMC), at a distance of only 168 000 light years. ...
Lithium abundances for 185 main-sequence stars
... resolution spectra of 130 stars and a reanalysis of data for 55 stars from Lambert et al. (1991). The survey takes advantage of improved photometric and spectroscopic determinations of effective temperature and metallicity as well as mass and age derived from Hipparcos absolute magnitudes, offering ...
... resolution spectra of 130 stars and a reanalysis of data for 55 stars from Lambert et al. (1991). The survey takes advantage of improved photometric and spectroscopic determinations of effective temperature and metallicity as well as mass and age derived from Hipparcos absolute magnitudes, offering ...
mass transfer in close, rapidly accreting protobinaries
... et al. 2006). Harries et al. (2003) and Hilditch et al. (2005) report a sample of 50 OB star eclipsing binaries with periods of 5 days or less taken from the Optical Gravitational Lens Experiment survey (OGLE; Udalski et al. 1998) of the SMC. This period limit corresponds to a semimajor axis of 0:26 ...
... et al. 2006). Harries et al. (2003) and Hilditch et al. (2005) report a sample of 50 OB star eclipsing binaries with periods of 5 days or less taken from the Optical Gravitational Lens Experiment survey (OGLE; Udalski et al. 1998) of the SMC. This period limit corresponds to a semimajor axis of 0:26 ...
IR-excesses around nearby Lambda Boo stars are caused by debris
... 2013). In those cases, polarimetry has been shown to aid in the identification of bow waves through the determination of the polarization angle relative to the emission, which helps differentiate the origin of the IR excess emission as bow waves. However, AO assisted spectroscopy from large ground-b ...
... 2013). In those cases, polarimetry has been shown to aid in the identification of bow waves through the determination of the polarization angle relative to the emission, which helps differentiate the origin of the IR excess emission as bow waves. However, AO assisted spectroscopy from large ground-b ...
Gas giants in hot water: inhibiting giant planet
... a function of radius, affecting their structure and their potential to form planets via gravitational instability or core accretion. In fact, I show that in the interior of massive embedded star clusters, the temperature approaches and exceeds the condensation temperature of water ice, TIce 150–17 ...
... a function of radius, affecting their structure and their potential to form planets via gravitational instability or core accretion. In fact, I show that in the interior of massive embedded star clusters, the temperature approaches and exceeds the condensation temperature of water ice, TIce 150–17 ...
Spectroscopic observation of helium-ion- and hydrogen
... a “cloud” obeyed a three-dimensional wave equation. This model was later modified by Born who proposed a point electron existing everywhere at once weighed statistically so that only an expectation value as a single-valued observable is obtained with measurement that “collapses” the infinity of simu ...
... a “cloud” obeyed a three-dimensional wave equation. This model was later modified by Born who proposed a point electron existing everywhere at once weighed statistically so that only an expectation value as a single-valued observable is obtained with measurement that “collapses” the infinity of simu ...
this article
... “presolar”. The majority (~ 99%) of the “presolar” dust grains emanated from AGB stars based on their isotopic compositions and the nuclear processes expected to occur in those stars. Presolar grains demonstrate that the AGB dust grains become part of the next generation of stars and planets (Clayto ...
... “presolar”. The majority (~ 99%) of the “presolar” dust grains emanated from AGB stars based on their isotopic compositions and the nuclear processes expected to occur in those stars. Presolar grains demonstrate that the AGB dust grains become part of the next generation of stars and planets (Clayto ...
Elliptical galaxies
... The effective radius Re is strongly correlated with the absolute magnitude MB ...
... The effective radius Re is strongly correlated with the absolute magnitude MB ...
Properties of rapidly rotating PNS with antikaon condensates at
... have been observed in our galaxy[12], many of them can have a period of as low as a millisecond, or a frequency that is greater than 500 Hz. The fastest known pulsar, PSR J1748-2446ad, that has been observed to date was discovered [13] in 2004. It has a rotation period of 1.397 ms and frequency of 7 ...
... have been observed in our galaxy[12], many of them can have a period of as low as a millisecond, or a frequency that is greater than 500 Hz. The fastest known pulsar, PSR J1748-2446ad, that has been observed to date was discovered [13] in 2004. It has a rotation period of 1.397 ms and frequency of 7 ...
Global Seismology of the Sun
... zones of stars. Such oscillations, usually referred to as solar-like oscillations, can for most purposes be described using the theory of linear, adiabatic, oscillations. The behaviour of the modes on the stellar surface is described in terms of spherical harmonics since these functions are a natura ...
... zones of stars. Such oscillations, usually referred to as solar-like oscillations, can for most purposes be described using the theory of linear, adiabatic, oscillations. The behaviour of the modes on the stellar surface is described in terms of spherical harmonics since these functions are a natura ...
Atmospheric Chemistry of Venus-like Exoplanets
... 3.1 Surface-Atmosphere Equilibrium Figure 1b-1d shows results from our models for 3 hypothetical Venus-like exoplanets. The initial parameters of these models were chosen from intersections of different CO2 and H2O buffers. These intersections determine the total pressure of CO2 and the temperature. ...
... 3.1 Surface-Atmosphere Equilibrium Figure 1b-1d shows results from our models for 3 hypothetical Venus-like exoplanets. The initial parameters of these models were chosen from intersections of different CO2 and H2O buffers. These intersections determine the total pressure of CO2 and the temperature. ...