The binary fractions in the massive young Large Magellanic Cloud
... where m1 and m2 are the magnitudes of the individual components. This means that the binary system will appear as a single object with a brighter magnitude than that of the primary star. Unresolved binaries with MS primary components will thus be biased towards the brighter envelope of the MS. We us ...
... where m1 and m2 are the magnitudes of the individual components. This means that the binary system will appear as a single object with a brighter magnitude than that of the primary star. Unresolved binaries with MS primary components will thus be biased towards the brighter envelope of the MS. We us ...
Astronomy Astrophysics
... orbital position of the individual signal was subtracted. Finally we averaged all non-discarded (typically 3) signals in order to derive a signal per chopper step. Due to detector transient effects, at the beginning of the observation the derived signals were systematically lower than those in the c ...
... orbital position of the individual signal was subtracted. Finally we averaged all non-discarded (typically 3) signals in order to derive a signal per chopper step. Due to detector transient effects, at the beginning of the observation the derived signals were systematically lower than those in the c ...
On the role of the WNH phase in the evolution of very massive stars
... peaks at 15–20 M⊙ , while WNH stars are spread more evenly over a large range of masses mostly above 30 M⊙ . There are only a few cases of mass overlap between the WN stars and a small fraction of the WNH stars. This may be because of WN stars in binary systems where H is present, or it may signify ...
... peaks at 15–20 M⊙ , while WNH stars are spread more evenly over a large range of masses mostly above 30 M⊙ . There are only a few cases of mass overlap between the WN stars and a small fraction of the WNH stars. This may be because of WN stars in binary systems where H is present, or it may signify ...
Formation of low-mass helium white dwarfs
... Today we know of the existence of more than 80 ELM WDs. The increasing number of discovered ELM WDs reveals that they are formed in different environments, from the Galactic disk to open and globular clusters. ELM WDs are most likely the result of binary evolution as they cannot be formed from singl ...
... Today we know of the existence of more than 80 ELM WDs. The increasing number of discovered ELM WDs reveals that they are formed in different environments, from the Galactic disk to open and globular clusters. ELM WDs are most likely the result of binary evolution as they cannot be formed from singl ...
White dwarfs, black holes and neutron stars in close binaries
... hite dwarfs, neutron stars and black holes are remnants of stars that have ended their ‘active’ life. A star is born when an interstellar gas cloud contracts and forms a sphere which in its centre has a temperature and pressure high enough to start hydrogen fusion. The star remains in this phase for ...
... hite dwarfs, neutron stars and black holes are remnants of stars that have ended their ‘active’ life. A star is born when an interstellar gas cloud contracts and forms a sphere which in its centre has a temperature and pressure high enough to start hydrogen fusion. The star remains in this phase for ...
the origin of binary stars - Institut d`Astronomie et d`Astrophysique
... of semimajor axis that is qualitatively consistent with the log-normal–like distribution found for main-sequence stars. With this evidence in hand, Mathieu (1994) concluded that “binary formation is the primary branch of the star-formation process.” Also, it seems clear that the process (or processe ...
... of semimajor axis that is qualitatively consistent with the log-normal–like distribution found for main-sequence stars. With this evidence in hand, Mathieu (1994) concluded that “binary formation is the primary branch of the star-formation process.” Also, it seems clear that the process (or processe ...
Navy Electricity and Electronics Training Series
... The series is designed to give small amounts of information that can be easily digested before advancing further into the more complex material. For a student just becoming acquainted with electricity or electronics, it is highly recommended that the modules be studied in their suggested sequence. W ...
... The series is designed to give small amounts of information that can be easily digested before advancing further into the more complex material. For a student just becoming acquainted with electricity or electronics, it is highly recommended that the modules be studied in their suggested sequence. W ...
BD−21 3873: another yellow-symbiotic barium star
... Abstract. An abundance analysis of the yellow symbiotic system BD−21◦ 3873 reveals it to be a metal-poor K-giant ([Fe/H] = −1.3) which is enriched in the heavy s-process elements. In that respect, this star appears to be a twin of AG Dra, another yellow symbiotic system analyzed in a previous paper ...
... Abstract. An abundance analysis of the yellow symbiotic system BD−21◦ 3873 reveals it to be a metal-poor K-giant ([Fe/H] = −1.3) which is enriched in the heavy s-process elements. In that respect, this star appears to be a twin of AG Dra, another yellow symbiotic system analyzed in a previous paper ...
A systematic study of X-ray variability in the ROSAT all
... variability studies of individual sources using the RASS data (Schmitt 1994), however, up to now no systematic search for variability in the total all-sky survey data has been carried out. The first great advantage of the RASS data set is that it is unbiased in the sense that no specific objects or ...
... variability studies of individual sources using the RASS data (Schmitt 1994), however, up to now no systematic search for variability in the total all-sky survey data has been carried out. The first great advantage of the RASS data set is that it is unbiased in the sense that no specific objects or ...
Annual Report 2014 - Max Planck Institute for Astrophysics
... particles, and the calculation of transition probThe Max-Planck-Institut für Astrophysik, usually abilities and cross–sections for astrophysical procalled MPA for short, was founded in 1958 under cesses in rarefied media. From its inception the the directorship of Ludwig Biermann. It was estab- MPA h ...
... particles, and the calculation of transition probThe Max-Planck-Institut für Astrophysik, usually abilities and cross–sections for astrophysical procalled MPA for short, was founded in 1958 under cesses in rarefied media. From its inception the the directorship of Ludwig Biermann. It was estab- MPA h ...
Spiral Density Waves in a Young Protoplanetary
... (P A). The emission local minima were fitted with a circular ring (R = a0 , with a0 the radius at which the gap is located), while the emission local maxima were fitted with two symmetric logarithmic spirals (R = R0 ebθ , with R0 the spiral radius at θ = 0◦ and b the rate at which the spirals incre ...
... (P A). The emission local minima were fitted with a circular ring (R = a0 , with a0 the radius at which the gap is located), while the emission local maxima were fitted with two symmetric logarithmic spirals (R = R0 ebθ , with R0 the spiral radius at θ = 0◦ and b the rate at which the spirals incre ...
black holes can play a constructive role as well
... clude that these particular objects are most likely foreground stars in our own Milky Way. The highest concentration of blue objects is found at the SWtip of the inner filament, which also harbours the brightest of the blue objects. It is also the only region that such blue objects are found in asso ...
... clude that these particular objects are most likely foreground stars in our own Milky Way. The highest concentration of blue objects is found at the SWtip of the inner filament, which also harbours the brightest of the blue objects. It is also the only region that such blue objects are found in asso ...
Hole spin dynamics and valenceband spin excitations in
... For k > 0, the spin–orbit interaction leads to a kdependent valence-band spin splitting even in the absence of an external magnetic field. This spin splitting originates either from bulk inversion asymmetry (Dresselhaus field), or from a growth-axis asymmetry of a heterostructure (Rashba field), whi ...
... For k > 0, the spin–orbit interaction leads to a kdependent valence-band spin splitting even in the absence of an external magnetic field. This spin splitting originates either from bulk inversion asymmetry (Dresselhaus field), or from a growth-axis asymmetry of a heterostructure (Rashba field), whi ...
Galactic Windmills - Dr. Karl Remeis
... source behind a large mass is bent around this mass and the observer sees a distorted image of the source (see Walsh et al., 1979, and references therein). The electromagnetic force is nonetheless very important for many processes in the world and the universe. The most direct evidence of the import ...
... source behind a large mass is bent around this mass and the observer sees a distorted image of the source (see Walsh et al., 1979, and references therein). The electromagnetic force is nonetheless very important for many processes in the world and the universe. The most direct evidence of the import ...
- Repository of the Academy`s Library
... 9.2.2 Moving sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9.3 Excitation of kink oscillations of solar coronal loops . . . . . . . . . . . . . . . Interaction of MHD waves with partly-ionised boundaries . . . . . . . . . . . . . . . 10.1 Interaction of long-period MHD wave ...
... 9.2.2 Moving sources . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 9.3 Excitation of kink oscillations of solar coronal loops . . . . . . . . . . . . . . . Interaction of MHD waves with partly-ionised boundaries . . . . . . . . . . . . . . . 10.1 Interaction of long-period MHD wave ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... 1.5.2. Are there Big Bang-less cosmologies? 1.6. Question 5 1.7. Question 6 1.7.1. How can we possibly see galaxies that are moving away from us at superluminal speeds? 1.7.2. Why can’t we explain the Hubble flow through the physical motion of galaxies through space? 1.7.3. Can galaxies with recessi ...
... 1.5.2. Are there Big Bang-less cosmologies? 1.6. Question 5 1.7. Question 6 1.7.1. How can we possibly see galaxies that are moving away from us at superluminal speeds? 1.7.2. Why can’t we explain the Hubble flow through the physical motion of galaxies through space? 1.7.3. Can galaxies with recessi ...
150 Million ly - Northern Michigan University
... Where did the Spirals Go? • Galactic collisions and mergers • Collisions often repeated would increase star formation, possibly using up available gas. Spirals no longer seen as they are not making new stars along spiral arms • Tidal forces among galaxies could have disrupted spiral arm patterns ...
... Where did the Spirals Go? • Galactic collisions and mergers • Collisions often repeated would increase star formation, possibly using up available gas. Spirals no longer seen as they are not making new stars along spiral arms • Tidal forces among galaxies could have disrupted spiral arm patterns ...
FERMI GBM detections of four AXPs at soft gamma-rays
... SWIFT SWIFT gamma-ray burst mission XRT X-Ray Telescope ...
... SWIFT SWIFT gamma-ray burst mission XRT X-Ray Telescope ...