Quantitative evidence of an intrinsic luminosity spread in the Orion
... position of individual stars on the HR-diagram with theoretical isochrones and evolutionary tracks. For the majority of stars, the main uncertainties in age are related to the determination of the intrinsic luminosity, since the pre-main-sequence evolution of low mass stars takes place at nearly con ...
... position of individual stars on the HR-diagram with theoretical isochrones and evolutionary tracks. For the majority of stars, the main uncertainties in age are related to the determination of the intrinsic luminosity, since the pre-main-sequence evolution of low mass stars takes place at nearly con ...
The following descriptions are based on ancient Sumerian
... was that the Nibiru-Saturn encounter “changed the destiny of Nibiru” (i.e. determined its orbit about the Sun). [It might be noted, parenthetically, that it’s not necessary to the theory for Nibiru, after encountering Neptune, to have then proceeded directly to its rendezvous with Uranus. It may ver ...
... was that the Nibiru-Saturn encounter “changed the destiny of Nibiru” (i.e. determined its orbit about the Sun). [It might be noted, parenthetically, that it’s not necessary to the theory for Nibiru, after encountering Neptune, to have then proceeded directly to its rendezvous with Uranus. It may ver ...
A non-grey analytical model for irradiated atmospheres.
... be obtained for very restrictive approximations on the opacities, they provide nonetheless a useful tool to understand the physics of the radiative transfer and to compute with a low computational cost temperature profiles for a large variety of atmospheric properties. In the particular model derive ...
... be obtained for very restrictive approximations on the opacities, they provide nonetheless a useful tool to understand the physics of the radiative transfer and to compute with a low computational cost temperature profiles for a large variety of atmospheric properties. In the particular model derive ...
- Achieve the Core
... students’ time to read, and the video adds a multimedia component to make the task a more complete and authentic representation of research. The text meets the expectations for text complexity at grade 9. Assessments aligned to the CCSS will employ quality, complex texts such as these, and some asse ...
... students’ time to read, and the video adds a multimedia component to make the task a more complete and authentic representation of research. The text meets the expectations for text complexity at grade 9. Assessments aligned to the CCSS will employ quality, complex texts such as these, and some asse ...
Cygnus X-1 poster (Massive Star Workshop)
... We adopt the simplest formation scenario that can explain all the observations. • assume both stars, the BH progenitor and the O supergiant were born at the same time • assume there was no mass transfer at all in the history of Cygnus X-1. (This means we can model the O supergiant as a single isolat ...
... We adopt the simplest formation scenario that can explain all the observations. • assume both stars, the BH progenitor and the O supergiant were born at the same time • assume there was no mass transfer at all in the history of Cygnus X-1. (This means we can model the O supergiant as a single isolat ...
Probing the Dark Matter Content of Local Group Dwarf Spheroidal
... As this was significantly higher than the values typical of globular star clusters, this provided the first hint that the dSphs were a class of stellar system distinct from the globular clusters, despite the fact that in many cases their stellar mass was similar. Subsequent observations have borne o ...
... As this was significantly higher than the values typical of globular star clusters, this provided the first hint that the dSphs were a class of stellar system distinct from the globular clusters, despite the fact that in many cases their stellar mass was similar. Subsequent observations have borne o ...
Numerical modeling of plasma structures and turbulence transport in
... The thesis focuses on the modeling of the inner-heliospheric solar wind with its embedded magnetic field by numerically solving the equations of magnetohydrodynamics (MHD). The main numerical tool used throughout this work is the state-ofthe-art MHD code Cronos, which is extended from its basic setu ...
... The thesis focuses on the modeling of the inner-heliospheric solar wind with its embedded magnetic field by numerically solving the equations of magnetohydrodynamics (MHD). The main numerical tool used throughout this work is the state-ofthe-art MHD code Cronos, which is extended from its basic setu ...
Transport of angular momentum in massive stars
... force, the effective mass is reduced, this leads to a decrease in the luminosity (Langer, 2012b) of a star. The rotation can induce mixing, leading to a rejuvenation and hence, a longer lifetime of the star(Pols, 2009). The influence of rotation on a massive star is as strong as the influence of the ...
... force, the effective mass is reduced, this leads to a decrease in the luminosity (Langer, 2012b) of a star. The rotation can induce mixing, leading to a rejuvenation and hence, a longer lifetime of the star(Pols, 2009). The influence of rotation on a massive star is as strong as the influence of the ...
the fragmentation of magnetized, massive star-forming
... are described by a vector of state variables (ρ, ρ v , E, B , ER ) defined at every grid cell, where ρ is the gas density, ρ v the momentum, E the non-gravitational energy density (i.e., the total of the kinetic, thermal, and magnetic energy densities), B the magnetic field, and ER the radiation ene ...
... are described by a vector of state variables (ρ, ρ v , E, B , ER ) defined at every grid cell, where ρ is the gas density, ρ v the momentum, E the non-gravitational energy density (i.e., the total of the kinetic, thermal, and magnetic energy densities), B the magnetic field, and ER the radiation ene ...
View - ESA
... differing quality, scope and accuracy. It must be realized, however, that stellar catalogues are a difficult business, since they have to extract information from the original observation records, published papers, other repertories, etc. which themselves suffer from the same inconsistencies and lim ...
... differing quality, scope and accuracy. It must be realized, however, that stellar catalogues are a difficult business, since they have to extract information from the original observation records, published papers, other repertories, etc. which themselves suffer from the same inconsistencies and lim ...
IDENTIFICATION OF MAIN-SEQUENCE STARS WITH MID
... most found using high-resolution stellar spectroscopy capable of detecting Doppler shifts in the parent star. However, the process or processes by which these planets form is still unknown. Planetesimals may originate in circumstellar disks, formed as a by-product of star formation. The evolutionary ...
... most found using high-resolution stellar spectroscopy capable of detecting Doppler shifts in the parent star. However, the process or processes by which these planets form is still unknown. Planetesimals may originate in circumstellar disks, formed as a by-product of star formation. The evolutionary ...
Author`s personal copy - Observatoire de la Côte d`Azur
... When looking at the structure of the outer Solar System, i.e. the four giant planets and the populations of small bodies from the orbit of Jupiter outwards, one sees several puzzling aspects that do not fit the simple scenario of in-situ formation of planets from a circum-solar disk of gas and solids ...
... When looking at the structure of the outer Solar System, i.e. the four giant planets and the populations of small bodies from the orbit of Jupiter outwards, one sees several puzzling aspects that do not fit the simple scenario of in-situ formation of planets from a circum-solar disk of gas and solids ...
The Hamburg/ESO R-process Enhanced Star survey (HERES)
... Furthermore, and perhaps even more importantly, individual age determinations are possible for these stars using long-lived radioactive isotopes, such as 232 Th (half-life 14.05 Gyr) or 238 U (4.468 Gyr). By comparing the abundance ratio of these elements relative to a stable r-process element of si ...
... Furthermore, and perhaps even more importantly, individual age determinations are possible for these stars using long-lived radioactive isotopes, such as 232 Th (half-life 14.05 Gyr) or 238 U (4.468 Gyr). By comparing the abundance ratio of these elements relative to a stable r-process element of si ...
Astronomy Astrophysics
... Furthermore, and perhaps even more importantly, individual age determinations are possible for these stars using long-lived radioactive isotopes, such as 232 Th (half-life 14.05 Gyr) or 238 U (4.468 Gyr). By comparing the abundance ratio of these elements relative to a stable r-process element of si ...
... Furthermore, and perhaps even more importantly, individual age determinations are possible for these stars using long-lived radioactive isotopes, such as 232 Th (half-life 14.05 Gyr) or 238 U (4.468 Gyr). By comparing the abundance ratio of these elements relative to a stable r-process element of si ...
Cosmology with objects from the Hamburg Quasar Surveys
... The direct measurement of the SED is possible only in absorption line systems where a sufficient number of ionization stages can be observed simultaneously. And even in such a favourable case it is always possible that a neighbouring galaxy or AGN is dominant. Therefore in practice the SED and inten ...
... The direct measurement of the SED is possible only in absorption line systems where a sufficient number of ionization stages can be observed simultaneously. And even in such a favourable case it is always possible that a neighbouring galaxy or AGN is dominant. Therefore in practice the SED and inten ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... remove the fragile product from the high-temperature region where it might otherwise be destroyed. Convective burning in the oxygen-neon shell of a 20 M, star has been modeled in two dimensions by Bazan & Arnett (1994). They find that largescale plume structures dominate the velocity field, physical ...
... remove the fragile product from the high-temperature region where it might otherwise be destroyed. Convective burning in the oxygen-neon shell of a 20 M, star has been modeled in two dimensions by Bazan & Arnett (1994). They find that largescale plume structures dominate the velocity field, physical ...
Puzzling X-rays from the new colliding wind binary Wolf–Rayet 65
... systems that consist of a WR and an OB-type star (Wallace 2007). The collision between two stellar winds in these systems produces characteristic signatures in different wavelength bands that can include non-thermal radio emission (Eichler & Usov 1993), copious and variable X-rays (Stevens, Blondin ...
... systems that consist of a WR and an OB-type star (Wallace 2007). The collision between two stellar winds in these systems produces characteristic signatures in different wavelength bands that can include non-thermal radio emission (Eichler & Usov 1993), copious and variable X-rays (Stevens, Blondin ...