Two extremely luminous WN stars in the Galactic center with
... and contains many OB-type stars, the more evolved Quintuplet cluster (3–5 Myr old) harbors many Wolf-Rayet (WR) stars. Besides these compact stellar conglomerates, many high-mass stars whose association with stellar clusters is not obvious are scattered in the GC. Among these are the rather isolated ...
... and contains many OB-type stars, the more evolved Quintuplet cluster (3–5 Myr old) harbors many Wolf-Rayet (WR) stars. Besides these compact stellar conglomerates, many high-mass stars whose association with stellar clusters is not obvious are scattered in the GC. Among these are the rather isolated ...
STELLAR MASSES AND STAR FORMATION RATES OF LENSED DUSTY STAR-FORMING... FROM THE SPT SURVEY
... stellar masses, IR luminosities, and star formation rates (SFRs). The SED fits of six SPT sources show that the intrinsic stellar masses span a range more than one order of magnitude with a median value ∼ 5 ×1010 M⊙ . The intrinsic IR luminosities range from 4×1012 L⊙ to 4×1013 L⊙ . They all have pr ...
... stellar masses, IR luminosities, and star formation rates (SFRs). The SED fits of six SPT sources show that the intrinsic stellar masses span a range more than one order of magnitude with a median value ∼ 5 ×1010 M⊙ . The intrinsic IR luminosities range from 4×1012 L⊙ to 4×1013 L⊙ . They all have pr ...
U P C NIVERSITAT
... Because of their well known observational properties Type Ia, or thermonuclear, supernovae are used as standard candles, and have allowed the discovery of the accelerating expansion of the Universe. Yet, despite their importance, we still do not know exactly which stellar systems produce them. Howev ...
... Because of their well known observational properties Type Ia, or thermonuclear, supernovae are used as standard candles, and have allowed the discovery of the accelerating expansion of the Universe. Yet, despite their importance, we still do not know exactly which stellar systems produce them. Howev ...
Confronting Dark Matter Powered Stars with Recent Results from
... Explaining the nature of the non-luminous matter component, called dark matter (DM), is most crucial to both scienti c elds. This study combines considerations about the nature of the dark matter particle and fundamental questions concerning the nature of the rst stars forming in the history of th ...
... Explaining the nature of the non-luminous matter component, called dark matter (DM), is most crucial to both scienti c elds. This study combines considerations about the nature of the dark matter particle and fundamental questions concerning the nature of the rst stars forming in the history of th ...
Tidal interaction of a rotating 1 vec {M_sun} star with a - UvA-DARE
... In T98 the stellar normal mode spectrum was considered fixed, i.e. for simplicity effects of stellar rotation and stellar evolution were ignored. However, in orbits with a significant eccentricity the tidal forcing is characterised not by one but by a spectrum of forcing frequencies which can potent ...
... In T98 the stellar normal mode spectrum was considered fixed, i.e. for simplicity effects of stellar rotation and stellar evolution were ignored. However, in orbits with a significant eccentricity the tidal forcing is characterised not by one but by a spectrum of forcing frequencies which can potent ...
Chemical composition of B-type supergiants in the OB8, OB10
... association. The radial velocity for OB8-76 differs by some 70 kms−1 which could suggest the star is part of a binary system, or has a peculiar velocities within the OB association. Being part of a binary does not necessarily exclude using the star in a detailed model atmosphere analysis as the comp ...
... association. The radial velocity for OB8-76 differs by some 70 kms−1 which could suggest the star is part of a binary system, or has a peculiar velocities within the OB association. Being part of a binary does not necessarily exclude using the star in a detailed model atmosphere analysis as the comp ...
Symbiotic Stars as Laboratories for the Study of
... Abstract Symbiotic binary stars typically consist of a white dwarf (WD) that accretes material from the wind of a companion red giant. Orbital periods for these binaries are on the order of years, and their relatively small optical outbursts tend to occur every few years to decades. In some symbioti ...
... Abstract Symbiotic binary stars typically consist of a white dwarf (WD) that accretes material from the wind of a companion red giant. Orbital periods for these binaries are on the order of years, and their relatively small optical outbursts tend to occur every few years to decades. In some symbioti ...
The presence of gamma rays in space was known before they were
... heavier than iron. This effectively is the final stage in nucleosynthesis. As mentioned earlier a star stops undergoing fusion when it reaches iron as the amount of energy released in fusing iron is less than what is put in. However due to the explosion itself having so much energy released in a sma ...
... heavier than iron. This effectively is the final stage in nucleosynthesis. As mentioned earlier a star stops undergoing fusion when it reaches iron as the amount of energy released in fusing iron is less than what is put in. However due to the explosion itself having so much energy released in a sma ...
The CN/C15 N isotopic ratio towards dark clouds
... and C15 N lines towards L1498, which could not be ascribed to any obvious technical issue. We note, however, that the uncertainty on the rest frequency reported in the Cologne Database for Molecular Spectroscopy (Müller et al. 2005) is 0.1 MHz, or 0.25 km s−1 , which could account for the observed ...
... and C15 N lines towards L1498, which could not be ascribed to any obvious technical issue. We note, however, that the uncertainty on the rest frequency reported in the Cologne Database for Molecular Spectroscopy (Müller et al. 2005) is 0.1 MHz, or 0.25 km s−1 , which could account for the observed ...
Cross sections of the gamma, proton and gamma, proton neutron
... The interaction of high energy electromagnetic radiation with matter has been a subject of much interest to both the oretical and experimental physicists for many years. In general, the interaction is with either the electrons of an atom or with its nucleus. The photon-electron interaction has been ...
... The interaction of high energy electromagnetic radiation with matter has been a subject of much interest to both the oretical and experimental physicists for many years. In general, the interaction is with either the electrons of an atom or with its nucleus. The photon-electron interaction has been ...
How can double-barred galaxies be long-lived?
... a total mass of Mg distributed in a lg scalelength MiyamotoNagai disc. Some differences in the initial conditions should be noted. The disc scalelength of SimL (l2 = 6.5 kpc, hence the “L” for “long”) is almost twice that of SimS (3.5 kpc, “S” for “short”) for A7, page 2 of 14 ...
... a total mass of Mg distributed in a lg scalelength MiyamotoNagai disc. Some differences in the initial conditions should be noted. The disc scalelength of SimL (l2 = 6.5 kpc, hence the “L” for “long”) is almost twice that of SimS (3.5 kpc, “S” for “short”) for A7, page 2 of 14 ...
Fuzzy Dark Matter
... But it wasn't just that cluster. Today, we know that visible matter accounts for only five percent of the universe's total mass-energy. (As Einstein's famous equation, E=mc2, tells us, the concepts of matter and energy are intrinsically linked.) Dark matter makes up about a quarter of the total mas ...
... But it wasn't just that cluster. Today, we know that visible matter accounts for only five percent of the universe's total mass-energy. (As Einstein's famous equation, E=mc2, tells us, the concepts of matter and energy are intrinsically linked.) Dark matter makes up about a quarter of the total mas ...
What happened to discrete chaos, the Quenouille process, and the
... the probability of seeing six stars in a square degree, which he finds to be 1 in 7 790 638. Perhaps we would be inclined to compute the probability of finding at least six stars in a square degree, which in this case is 1 in 7 831 614. Stigler (1982) considers this the first application of the Pois ...
... the probability of seeing six stars in a square degree, which he finds to be 1 in 7 790 638. Perhaps we would be inclined to compute the probability of finding at least six stars in a square degree, which in this case is 1 in 7 831 614. Stigler (1982) considers this the first application of the Pois ...
Rotating White Dwarfs and Neutron Stars in - Padis
... White dwarfs and neutron stars are formed when normal (main sequence) stars end their thermonuclear evolution. They differ from normal stars in two fundamental ways. First, since they do not burn nuclear fuel, they cannot support themselves against gravitational collapse by generating thermal pressu ...
... White dwarfs and neutron stars are formed when normal (main sequence) stars end their thermonuclear evolution. They differ from normal stars in two fundamental ways. First, since they do not burn nuclear fuel, they cannot support themselves against gravitational collapse by generating thermal pressu ...
P-nuclei
p-Nuclei (p stands for proton-rich) are certain proton-rich, naturally occurring isotopes of some elements between selenium and mercury which cannot be produced in either s- or r-process.