The Relation between Interstellar Turbulence and Star Formation
... of the Milky Way. These are clouds of dust and Stars are important. They are the primary source gas that block the light from stars further away. of radiation, with competition only from the 3K Since about a century ago we know that these black body radiation of the cosmic microwave clouds are assoc ...
... of the Milky Way. These are clouds of dust and Stars are important. They are the primary source gas that block the light from stars further away. of radiation, with competition only from the 3K Since about a century ago we know that these black body radiation of the cosmic microwave clouds are assoc ...
Systematic Study of Mass Loss in the Evolution of Massive Stars
... However, because of its intrinsically dynamical nature, and because of the strong nonlinearity of the responsible physical processes driving it, mass loss is one of the largest sources of uncertainty in the simulation of massive star evolution. In most stellar evolution simulations, only wind mass l ...
... However, because of its intrinsically dynamical nature, and because of the strong nonlinearity of the responsible physical processes driving it, mass loss is one of the largest sources of uncertainty in the simulation of massive star evolution. In most stellar evolution simulations, only wind mass l ...
Multiple Jets from the High-Mass (Proto) stellar Cluster AFGL5142
... contribution from the ionized gas at mm and submm wavelengths is ∼ 1999). Thus, dust emission dominates the 1.3mm continuum flux of all the sources, and likely does so to wavelengths as long as ∼ 3 mm. Because of a lack of high resolution images at more than one wavelength, the emissivity index of t ...
... contribution from the ionized gas at mm and submm wavelengths is ∼ 1999). Thus, dust emission dominates the 1.3mm continuum flux of all the sources, and likely does so to wavelengths as long as ∼ 3 mm. Because of a lack of high resolution images at more than one wavelength, the emissivity index of t ...
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... subsequent shocks. The clump forms low-mass and massive protostars. For the massive protostars, much of the accretion flow is along extended filamentary paths. It seems doubtful that these complexities could be properly described by simple analytic models of 3D cluster structure and evolution. Yet t ...
... subsequent shocks. The clump forms low-mass and massive protostars. For the massive protostars, much of the accretion flow is along extended filamentary paths. It seems doubtful that these complexities could be properly described by simple analytic models of 3D cluster structure and evolution. Yet t ...
Evidence of suppression of star formation by quasar
... tribution of galaxy colors. If AGN feedback couples to the gas as efficiently as required by galaxy formation models, then massive, early-type galaxies will be gas-poor and passively aging, while younger galaxies, typically lower-mass, late-type galaxies will still have enough star formation materia ...
... tribution of galaxy colors. If AGN feedback couples to the gas as efficiently as required by galaxy formation models, then massive, early-type galaxies will be gas-poor and passively aging, while younger galaxies, typically lower-mass, late-type galaxies will still have enough star formation materia ...
Physical Processes in the Interstellar Medium
... by it, the CNM and WNM are two completely distinct phases in pressure equilibrium with each other, and all neutral atomic hydrogen in the ISM belongs to one phase or the other. However, observations of Hi in the ISM suggest that the true picture is more complicated, as there is good evidence that a ...
... by it, the CNM and WNM are two completely distinct phases in pressure equilibrium with each other, and all neutral atomic hydrogen in the ISM belongs to one phase or the other. However, observations of Hi in the ISM suggest that the true picture is more complicated, as there is good evidence that a ...
CENTRAL STARS OF PLANETARY NEBULAE IN THE LARGE
... agree. The procedure we typically adopted was to trust the LiF1A absolute flux calibration (which is most reliable; Sahnow et al. 2000) and scale the flux of the other detectors if needed. The LiF1B segment is severely affected by an artifact known as ‘‘the worm’’ (FUSE Data Handbook, ver. 1.3) and ...
... agree. The procedure we typically adopted was to trust the LiF1A absolute flux calibration (which is most reliable; Sahnow et al. 2000) and scale the flux of the other detectors if needed. The LiF1B segment is severely affected by an artifact known as ‘‘the worm’’ (FUSE Data Handbook, ver. 1.3) and ...
Chemical gradients in the Milky Way from the RAVE data
... estimates (Breddels et al. 2010; Zwitter et al. 2010; Burnett et al. 2011; Binney et al. 2013) enable one to locate the stars in three-dimensional space. Proper motions are listed in a variety of catalogues: Tycho2 (Høg et al. 2000), the PPM-Extended catalogues PPMX and PPMXL (Roeser et al. 2008, 20 ...
... estimates (Breddels et al. 2010; Zwitter et al. 2010; Burnett et al. 2011; Binney et al. 2013) enable one to locate the stars in three-dimensional space. Proper motions are listed in a variety of catalogues: Tycho2 (Høg et al. 2000), the PPM-Extended catalogues PPMX and PPMXL (Roeser et al. 2008, 20 ...
First Results from the WISE Enhanced Resolution Galaxy Atlas
... a fossil record of galaxy evolution, the boundary condition for cosmological models that explain past and current state of the universe. Although galaxies come in all shapes, sizes, mass and morphological cases, the physics governing their structure and evolution should be elemental: we expect that ...
... a fossil record of galaxy evolution, the boundary condition for cosmological models that explain past and current state of the universe. Although galaxies come in all shapes, sizes, mass and morphological cases, the physics governing their structure and evolution should be elemental: we expect that ...
doctoral thesis (Dissertation)
... Stars form by gravitational collapse from giant molecular clouds. Due to the conservation of angular momentum this collapse does not happen radially, but the matter forms circumstellar disk first and is consequently accreted from the disk onto the star. This thesis deals with the high-energy emissio ...
... Stars form by gravitational collapse from giant molecular clouds. Due to the conservation of angular momentum this collapse does not happen radially, but the matter forms circumstellar disk first and is consequently accreted from the disk onto the star. This thesis deals with the high-energy emissio ...
Lithium abundances in nearby FGK dwarf and subgiant stars
... high resolution spectroscopic study of nearby stars from about 500 to 800 objects (Ramı́rez, Allende Prieto, & Lambert, in preparation, hereafter RAL). Their data are being used to study oxygen abundances in local stellar populations, but their spectra cover the 6708 Å region, which contains the li ...
... high resolution spectroscopic study of nearby stars from about 500 to 800 objects (Ramı́rez, Allende Prieto, & Lambert, in preparation, hereafter RAL). Their data are being used to study oxygen abundances in local stellar populations, but their spectra cover the 6708 Å region, which contains the li ...
The Evolution of Protostars - Max-Planck
... Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass accretes from the core onto a protostar, likely through an accretion disk, and it is during this phase that the initial masses of stars and the initial conditions for planet formation are set. ...
... Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass accretes from the core onto a protostar, likely through an accretion disk, and it is during this phase that the initial masses of stars and the initial conditions for planet formation are set. ...
THE FUTURE IS NOW: THE FORMATION OF SINGLE LOW
... then decline monotonically for the four oldest bins. With this procedure they derived formation rates of 0.4, 4.5, and 0:9 ; 1013 pc3 yr1 for the 0.4, 0.6, and >0.8 M components, respectively. They also applied a binary correction to the He WD population. In the discussion that follows we will o ...
... then decline monotonically for the four oldest bins. With this procedure they derived formation rates of 0.4, 4.5, and 0:9 ; 1013 pc3 yr1 for the 0.4, 0.6, and >0.8 M components, respectively. They also applied a binary correction to the He WD population. In the discussion that follows we will o ...
thesis
... which the formation of massive stars occurs, the smaller numbers of massive stars, and the greater distances between us and the nearest regions where massive stars are forming. As an additional consequence of the short times scales over which the formation of massive stars occurs a much greater port ...
... which the formation of massive stars occurs, the smaller numbers of massive stars, and the greater distances between us and the nearest regions where massive stars are forming. As an additional consequence of the short times scales over which the formation of massive stars occurs a much greater port ...
Analysis of cool DO-type white dwarfs from the Sloan Digital Sky
... 52 additional DO WDs, 28 of them previously analyzed with non-LTE model atmospheres. The remaining 24 had spectra with a too low signal-to noise ratio (S/N) or were either a misclassified cataclysmic variable (CV), misclassified He-sdO stars (log g ≤ 7.0), or DAO WDs. J0839 is listed as DAO WD, but ...
... 52 additional DO WDs, 28 of them previously analyzed with non-LTE model atmospheres. The remaining 24 had spectra with a too low signal-to noise ratio (S/N) or were either a misclassified cataclysmic variable (CV), misclassified He-sdO stars (log g ≤ 7.0), or DAO WDs. J0839 is listed as DAO WD, but ...
The X-shooter Spectral Library (XSL): I. DR1. Near
... libraries with extended wavelength coverage at moderate resolution are still largely missing. With the high-efficiency, broad-wavelength coverage and high/moderate resolution of the X-shooter spectrograph at ESO’s VLT (Vernet et al. 2011), we can now fill the gap between highresolution theoretical s ...
... libraries with extended wavelength coverage at moderate resolution are still largely missing. With the high-efficiency, broad-wavelength coverage and high/moderate resolution of the X-shooter spectrograph at ESO’s VLT (Vernet et al. 2011), we can now fill the gap between highresolution theoretical s ...
Circumstellar Material in Young Stellar Objects
... with the cloud. However, the study of molecular clouds did not reach its full growth until it became possible to observe mm and submm transitions of molecular species such as CO and NH (Cheung et al. 1968; Wilson et al. 1970; Kutner et al. 1977), allowing more detailed studies of the kinematics and ...
... with the cloud. However, the study of molecular clouds did not reach its full growth until it became possible to observe mm and submm transitions of molecular species such as CO and NH (Cheung et al. 1968; Wilson et al. 1970; Kutner et al. 1977), allowing more detailed studies of the kinematics and ...
A Herschel/HIFI study of Water in Two Intermediate
... Stars are large, luminous, gravitationally bound spheres of hot gas. Their luminosity lights up the galaxy, providing much of the energy that illuminates the less luminous features such as large molecular clouds of gas. Studying other galaxies in the universe is also possible because of stars. Galax ...
... Stars are large, luminous, gravitationally bound spheres of hot gas. Their luminosity lights up the galaxy, providing much of the energy that illuminates the less luminous features such as large molecular clouds of gas. Studying other galaxies in the universe is also possible because of stars. Galax ...
spatially resolved star formation history of milky way satellites
... in their own halos but whose history is oftenly influenced by larger galaxies lying in their proximity. The main difference between these two types of systems is the presence of dark matter, which is not found in globular clusters but conformes large fraction of the mass of the dwarf galaxies. Dark ...
... in their own halos but whose history is oftenly influenced by larger galaxies lying in their proximity. The main difference between these two types of systems is the presence of dark matter, which is not found in globular clusters but conformes large fraction of the mass of the dwarf galaxies. Dark ...
Master Thesis - Sterrenkunde RU Nijmegen
... stars span a large range of different masses, from ∼0.08M to &100M . As can be seen in figure 1.1, the luminosity of main-sequence stars strongly increases with mass (L ∝ M3−4 ). This means that more massive stars burn through their hydrogen supply faster, with timescales of a few millions of year ...
... stars span a large range of different masses, from ∼0.08M to &100M . As can be seen in figure 1.1, the luminosity of main-sequence stars strongly increases with mass (L ∝ M3−4 ). This means that more massive stars burn through their hydrogen supply faster, with timescales of a few millions of year ...
SN 2006gy: DISCOVERY OF THE MOST LUMINOUS
... However, there are reasons to suspect that the mass-loss properties of stars in the local universe may not be so different from these early stars. Namely, recent studies of line-driven winds from O-type stars and WR stars have shown that their winds are highly clumped, requiring that their mass-loss ...
... However, there are reasons to suspect that the mass-loss properties of stars in the local universe may not be so different from these early stars. Namely, recent studies of line-driven winds from O-type stars and WR stars have shown that their winds are highly clumped, requiring that their mass-loss ...
Models of the Structure and Evolution of Protoplanetary Disks
... from other grains in the disk. The iterative absorption and reemission of infrared radiation by dust grains in the disk causes the radiation to propagate through the disk in a diffusive way. Net energy input comes from absorption of direct stellar light in the disk’s surface layers, and from viscous ...
... from other grains in the disk. The iterative absorption and reemission of infrared radiation by dust grains in the disk causes the radiation to propagate through the disk in a diffusive way. Net energy input comes from absorption of direct stellar light in the disk’s surface layers, and from viscous ...
The APEX-CHAMP+ view of the Orion Molecular Cloud 1 core
... nearness makes the OMC-1 core region a touchstone for research on the dense molecular interstellar medium and PDRs. Methods. Using the Atacama Pathfinder Experiment telescope (APEX), we have imaged the line emission from the multiple transitions of several carbon monoxide (CO) isotopologues over the ...
... nearness makes the OMC-1 core region a touchstone for research on the dense molecular interstellar medium and PDRs. Methods. Using the Atacama Pathfinder Experiment telescope (APEX), we have imaged the line emission from the multiple transitions of several carbon monoxide (CO) isotopologues over the ...
ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION
... of massive stars. This is the period between the rapid accretion phase of star formation, when the central protostar is being formed, and the period when the UC phase gives way to a larger, more diffuse, less obscured HII region either by destruction of the natal molecular core or by moving out of t ...
... of massive stars. This is the period between the rapid accretion phase of star formation, when the central protostar is being formed, and the period when the UC phase gives way to a larger, more diffuse, less obscured HII region either by destruction of the natal molecular core or by moving out of t ...
Equations of state and structure of neutron stars
... First theoretical idea of neutron stars comes from Baade and Zwicky [13], being based on the analysis of supernova explosions. They stated that supernova explosion could be transition a from star to a neutron star. They also predicted that neutron stars consist of closely packed neutrons in the obje ...
... First theoretical idea of neutron stars comes from Baade and Zwicky [13], being based on the analysis of supernova explosions. They stated that supernova explosion could be transition a from star to a neutron star. They also predicted that neutron stars consist of closely packed neutrons in the obje ...