Maximum Mass Restraint of Neutron Stars
... the core it begins accumulating until it reaches approximately 1.44 solar masses. At this point degeneracy pressures can no longer support the core and the process of star collapse begins. Core collapse is a rather violent process and is caused by the production of gamma rays within the core. Throug ...
... the core it begins accumulating until it reaches approximately 1.44 solar masses. At this point degeneracy pressures can no longer support the core and the process of star collapse begins. Core collapse is a rather violent process and is caused by the production of gamma rays within the core. Throug ...
The spin and orbit of the newly discovered pulsar IGR J17480-2446
... We reported on the spin and orbital properties of the newly discovered accreting pulsar, IGR J17480-2446. Its 90.6 ms period makes it the first confirmed accreting pulsar in the range 10–100 ms. Pulsations were detected in all observations performed by RXTE, as well as in two out of the three Swift ...
... We reported on the spin and orbital properties of the newly discovered accreting pulsar, IGR J17480-2446. Its 90.6 ms period makes it the first confirmed accreting pulsar in the range 10–100 ms. Pulsations were detected in all observations performed by RXTE, as well as in two out of the three Swift ...
Gamma Ray Burst Afterglows and Host Galaxies
... GRBs in Obscured Starbursts? • Recently, two GRB host galaxies have been shown to have unusually high submillimeter wavelength brightness. • This suggests strong star formation activity hidden by dust. ...
... GRBs in Obscured Starbursts? • Recently, two GRB host galaxies have been shown to have unusually high submillimeter wavelength brightness. • This suggests strong star formation activity hidden by dust. ...
Kepler-1647b: The Largest And Longest-Period Kepler
... cavity surrounding the binary star (Pierens & Nelson 2007, 2008, 2013, hereafter PN07, PN08, PN15). Additionally, the planets should be coplanar (within a few degrees) for binary stars with sub-AU separation due to disk–binary alignment on precession timescales (Foucart & Lai 2013, 2014). The orbita ...
... cavity surrounding the binary star (Pierens & Nelson 2007, 2008, 2013, hereafter PN07, PN08, PN15). Additionally, the planets should be coplanar (within a few degrees) for binary stars with sub-AU separation due to disk–binary alignment on precession timescales (Foucart & Lai 2013, 2014). The orbita ...
The age of elliptical galaxies and bulges in a merger model The age
... present-day object, such as a cluster, to be traced back to arbitrarily early times. Dark matter haloes are modelled as truncated isothermal spheres and it is assumed that, as the halo forms, the gas relaxes to a distribution that exactly parallels that of the dark matter. Gas then cools and condens ...
... present-day object, such as a cluster, to be traced back to arbitrarily early times. Dark matter haloes are modelled as truncated isothermal spheres and it is assumed that, as the halo forms, the gas relaxes to a distribution that exactly parallels that of the dark matter. Gas then cools and condens ...
AR2013 - Vatican Observatory
... archived data available, such as from HST, SDSS, Spitzer, GALEX, Kepler, and soon-to-be available GAIA data (just to name a few) with future observational projects with telescopes (such as VATT). Asteroseismology: The Kepler and CoRot missions have provided a wealth of data on pulsating stars (such ...
... archived data available, such as from HST, SDSS, Spitzer, GALEX, Kepler, and soon-to-be available GAIA data (just to name a few) with future observational projects with telescopes (such as VATT). Asteroseismology: The Kepler and CoRot missions have provided a wealth of data on pulsating stars (such ...
Evidence for Black Holes
... mergers in dense star clusters. Their existence (or lack thereof ) could tell us a lot about the conditions under which black holes formed and whether supermassive holes grew from much smaller ones, either by hierarchical mergers or by runaway accretion. As yet there is no solid evidence for such a ...
... mergers in dense star clusters. Their existence (or lack thereof ) could tell us a lot about the conditions under which black holes formed and whether supermassive holes grew from much smaller ones, either by hierarchical mergers or by runaway accretion. As yet there is no solid evidence for such a ...
PDF format
... galaxies, you'll have better luck looking in clusters of galaxies than elsewhere in the universe. a) True, galaxy clusters have a much higher percentage of elliptical galaxies than do other parts of the universe. b) True, elliptical galaxies are found exclusively in galaxy ...
... galaxies, you'll have better luck looking in clusters of galaxies than elsewhere in the universe. a) True, galaxy clusters have a much higher percentage of elliptical galaxies than do other parts of the universe. b) True, elliptical galaxies are found exclusively in galaxy ...
Galaxies - WordPress.com
... as our galaxy ages over the next few billion years it will A not change at all B get smaller and become an elliptical galaxy C get fainter till it fades from view ...
... as our galaxy ages over the next few billion years it will A not change at all B get smaller and become an elliptical galaxy C get fainter till it fades from view ...
high angular resolution studies of protoplanetary discs
... It is observationally challenging to directly probe the physical conditions in the planet-forming regions of discs (a few tens of AU from the star) as these observations require subarcsecond spatial resolution. Furthermore, the emission of gas and dust arising from these regions (in the near- and mi ...
... It is observationally challenging to directly probe the physical conditions in the planet-forming regions of discs (a few tens of AU from the star) as these observations require subarcsecond spatial resolution. Furthermore, the emission of gas and dust arising from these regions (in the near- and mi ...
Supervisors
... coefficient of stellar plasma. However, there can be no complex molecules in hot stellar atmospheres (Teff & 9000 K) because the collisions between the plasma particles are energetic enough to destroy molecular bonds (Aret et al., 2008). If an atmospheric model includes hydrodynamics then it is able ...
... coefficient of stellar plasma. However, there can be no complex molecules in hot stellar atmospheres (Teff & 9000 K) because the collisions between the plasma particles are energetic enough to destroy molecular bonds (Aret et al., 2008). If an atmospheric model includes hydrodynamics then it is able ...
Document
... A majority of the galaxies in rich clusters are ellipticals, not spirals. There is often a single, very large central elliptical galaxy (sometimes two) that is cannibalizing other galaxies in its vicinity, growing bigger with time (see figure, top). X-ray observations of rich clusters reveal a hot i ...
... A majority of the galaxies in rich clusters are ellipticals, not spirals. There is often a single, very large central elliptical galaxy (sometimes two) that is cannibalizing other galaxies in its vicinity, growing bigger with time (see figure, top). X-ray observations of rich clusters reveal a hot i ...
identifying seasonal stars in kaurna astronomical traditions
... records. In western Victoria and southeast South Australia many astronomical traditions were recorded but, curiously, some of the brightest stars in the sky were omitted. Scholars claimed these stars did not feature in Aboriginal traditions. This continues to be repeated in the literature, but curre ...
... records. In western Victoria and southeast South Australia many astronomical traditions were recorded but, curiously, some of the brightest stars in the sky were omitted. Scholars claimed these stars did not feature in Aboriginal traditions. This continues to be repeated in the literature, but curre ...
Yellow supergiants as supernova progenitors: an indication of
... a factor of ten, the same trend is observed, but much stronger. In that case, the surface H abundance is strongly depleted, becoming smaller than the He abundance. Measurements of the surface abundances indicating such trends would be a clue to strong mass loss during the RSG phase. As three of the ...
... a factor of ten, the same trend is observed, but much stronger. In that case, the surface H abundance is strongly depleted, becoming smaller than the He abundance. Measurements of the surface abundances indicating such trends would be a clue to strong mass loss during the RSG phase. As three of the ...
Influence of the Gould Belt on Interstellar Extinction
... higher than that of the model by Arenou et al. (1992) is unlikely to be possible. To achieve a high accuracy of the extinction correction, it is more preferable to reveal specific absorbing clouds or to determine the individual extinction for each star from its highly accurate multiband photometry. ...
... higher than that of the model by Arenou et al. (1992) is unlikely to be possible. To achieve a high accuracy of the extinction correction, it is more preferable to reveal specific absorbing clouds or to determine the individual extinction for each star from its highly accurate multiband photometry. ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.