DUSTY CIRCUMSTELLAR DISKS B. Zuckerman
... light from the central star and then radiate this energy away in the IR. Such stars have been dubbed “Vega-like.” At most stars, the particles emit most vigorously at wavelengths between 25 and 200 µm. Such wavelengths are difficult or impossible to study from the ground. Thus, in the years since IR ...
... light from the central star and then radiate this energy away in the IR. Such stars have been dubbed “Vega-like.” At most stars, the particles emit most vigorously at wavelengths between 25 and 200 µm. Such wavelengths are difficult or impossible to study from the ground. Thus, in the years since IR ...
sections 19-22 instructor notes
... rotation curve in the outermost regions, including the region at the Sun’s distance from the Galactic centre. Dynamical theory suggests that A and B should also be related through the parameters of the velocity ellipsoid, ...
... rotation curve in the outermost regions, including the region at the Sun’s distance from the Galactic centre. Dynamical theory suggests that A and B should also be related through the parameters of the velocity ellipsoid, ...
Do We Know of Any Maunder Minimum Stars?
... log RHK < −5.1, the latter of which they considered Maunder minimum candidates. Baliunas & Jastrow (1990) suggested that the activity level of the sun during the Maunder Minimum corresponded to that of these low-activity stars, S = 0.1451. Zhang et al. (1994) applied this value to an analysis of the ...
... log RHK < −5.1, the latter of which they considered Maunder minimum candidates. Baliunas & Jastrow (1990) suggested that the activity level of the sun during the Maunder Minimum corresponded to that of these low-activity stars, S = 0.1451. Zhang et al. (1994) applied this value to an analysis of the ...
Isotopic composition of Hg and Pt in 5 slowly rotating HgMn stars *
... stars often relied on spectra of rather low resolution and low S/N ratio, so that only limited information could be derived from the centroid wavelength of unresolved isotopic blends. In this paper we present the results of a study of the isotopic compositions of Hg and Pt in 5 very slowly rotating ...
... stars often relied on spectra of rather low resolution and low S/N ratio, so that only limited information could be derived from the centroid wavelength of unresolved isotopic blends. In this paper we present the results of a study of the isotopic compositions of Hg and Pt in 5 very slowly rotating ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... of three CO lines in two high-redshift gravitationally lensed dusty star-forming galaxies, discovered by the South Pole Telescope. Strong lensing allows us to probe the structure and dynamics of the molecular gas in these two objects, at z = 2.78 and z = 5.66, with effective source-plane resolution ...
... of three CO lines in two high-redshift gravitationally lensed dusty star-forming galaxies, discovered by the South Pole Telescope. Strong lensing allows us to probe the structure and dynamics of the molecular gas in these two objects, at z = 2.78 and z = 5.66, with effective source-plane resolution ...
Hunting for Substructure in the Milky Way
... has evolved over time with ongoing research in the area. At its most basic level, the Milky Way is a barred disk galaxy with spiral arms. Its main components are the central bulge, the disk and the surrounding halo. When analysed in further detail, the disk can be divided into two components; a thin ...
... has evolved over time with ongoing research in the area. At its most basic level, the Milky Way is a barred disk galaxy with spiral arms. Its main components are the central bulge, the disk and the surrounding halo. When analysed in further detail, the disk can be divided into two components; a thin ...
X. Nuclear star clusters in low-mass early-type galaxies
... formation mechanisms, most of which are analytically derived. One of the few qualitative predictions for the relation between NSC mass and host galaxy velocity dispersion for in situ formation is given by McLaughlin, King & Nayakshin (2006), where it is assumed that the winds from giant stars and su ...
... formation mechanisms, most of which are analytically derived. One of the few qualitative predictions for the relation between NSC mass and host galaxy velocity dispersion for in situ formation is given by McLaughlin, King & Nayakshin (2006), where it is assumed that the winds from giant stars and su ...
Exposing the hidden white dwarf binary origin by means of a
... derived (DS2010) a binary and multiple star fraction of 71 per cent among the young local population of stars for stellar masses above 1.1 M . By comparison, in our first study of the single-star population (Schröder & Pagel 2003, hereafter referred to as SP2003) we only subtracted the binary syst ...
... derived (DS2010) a binary and multiple star fraction of 71 per cent among the young local population of stars for stellar masses above 1.1 M . By comparison, in our first study of the single-star population (Schröder & Pagel 2003, hereafter referred to as SP2003) we only subtracted the binary syst ...
Chemical composition of 90 F and G disk dwarfs
... kinematics of disk stars, but substantial dispersions imposed on weak statistical trends. (2) There exists a real scatter in the run of [α/Fe] vs. [Fe/H] possibly due to the mixture of stars with different origins. The scatter seems to increase with decreasing metallicity starting at [Fe/H] ' −0.4. ...
... kinematics of disk stars, but substantial dispersions imposed on weak statistical trends. (2) There exists a real scatter in the run of [α/Fe] vs. [Fe/H] possibly due to the mixture of stars with different origins. The scatter seems to increase with decreasing metallicity starting at [Fe/H] ' −0.4. ...
The Evolution of Molecular Clouds
... formation of molecular clouds must itself be a rather rapid process, and cannot take many dynamical timescales. Since the timescales for the formation, internal evolution, and destruction of molecular clouds are all of the same order, these processes probably cannot be clearly separated in time, and ...
... formation of molecular clouds must itself be a rather rapid process, and cannot take many dynamical timescales. Since the timescales for the formation, internal evolution, and destruction of molecular clouds are all of the same order, these processes probably cannot be clearly separated in time, and ...
A Star - Cloudy Nights
... A few stars in the sky are actually multiple star systems, which can have anywhere from three to ten stars orbiting around a common point. Most of the time, there will be two or three brighter stars, with the rest being extremely faint or extremely close to each other. Almaak, or Gamma Andromeda i ...
... A few stars in the sky are actually multiple star systems, which can have anywhere from three to ten stars orbiting around a common point. Most of the time, there will be two or three brighter stars, with the rest being extremely faint or extremely close to each other. Almaak, or Gamma Andromeda i ...
The Chemical Composition of Carbon-Rich, Very Metal
... put forward to account for the moderately metal-poor classical CH stars ([Fe/H]∼ −1.5). These are usually explained by a model involving mass transfer from a carbon-enhanced asymptotic giant branch (AGB) star (one that has since evolved to the white dwarf stage and cannot now be seen) to its lower-m ...
... put forward to account for the moderately metal-poor classical CH stars ([Fe/H]∼ −1.5). These are usually explained by a model involving mass transfer from a carbon-enhanced asymptotic giant branch (AGB) star (one that has since evolved to the white dwarf stage and cannot now be seen) to its lower-m ...
Lecture 2
... • Lyman- is characteristically asymmetric due to galaxyscale outflows • Absorption by the intervening IGM suppresses flux shortwards of Lyman- • The degree of suppression increases with redshift • This leads to a characteristic spectral break ...
... • Lyman- is characteristically asymmetric due to galaxyscale outflows • Absorption by the intervening IGM suppresses flux shortwards of Lyman- • The degree of suppression increases with redshift • This leads to a characteristic spectral break ...
Hot subdwarf stars-galactic orbits and distribution perpendicular to
... Hot subdwarfs are blue, horizontal-branch like stars, representing the late stages of evolution of stars having started with less than about 2.5 M⊙ on the main sequence. The hotter subdwarf B (sdB) stars form a well defined group. Their luminosity is of the order of 10 L⊙ and their surface temperatu ...
... Hot subdwarfs are blue, horizontal-branch like stars, representing the late stages of evolution of stars having started with less than about 2.5 M⊙ on the main sequence. The hotter subdwarf B (sdB) stars form a well defined group. Their luminosity is of the order of 10 L⊙ and their surface temperatu ...
Cygnus X-2, super-Eddington mass transfer, and pulsar binaries
... rapid Case B mass transfer may end with the donor on the Hayashi line, still retaining a large fraction of its original hydrogen envelope. However, there will be no long-lasting phase of mass transfer with the donor on the Hayashi line because the star starts shrinking with ignition of central heliu ...
... rapid Case B mass transfer may end with the donor on the Hayashi line, still retaining a large fraction of its original hydrogen envelope. However, there will be no long-lasting phase of mass transfer with the donor on the Hayashi line because the star starts shrinking with ignition of central heliu ...
A catalogue of the Chandra Deep Field South with multi
... 3.1. Image reduction and object search All procedures used for the data reduction are based on the MIDAS package. A WFI image processing pipeline was developed by Wolf et al. (2001) and makes intensive use of programmes developed by K. Meisenheimer, H.-J. Röser and H. Hippelein for the Calar Alto D ...
... 3.1. Image reduction and object search All procedures used for the data reduction are based on the MIDAS package. A WFI image processing pipeline was developed by Wolf et al. (2001) and makes intensive use of programmes developed by K. Meisenheimer, H.-J. Röser and H. Hippelein for the Calar Alto D ...
Effect of the stellar spin history on the tidal evolution of close
... been detected (Benedict et al. 1998; Kiraga & Stepien 2007; Charbonneau et al. 2009). In contrast to Sun-like stars that are mostly radiative except for a small (in terms of mass) convective region at the surface, very low-mass stars (M∗ < 0.35 M ) are entirely convective (Chabrier & Baraffe 1997). ...
... been detected (Benedict et al. 1998; Kiraga & Stepien 2007; Charbonneau et al. 2009). In contrast to Sun-like stars that are mostly radiative except for a small (in terms of mass) convective region at the surface, very low-mass stars (M∗ < 0.35 M ) are entirely convective (Chabrier & Baraffe 1997). ...
Accuracy of spectroscopy-based radioactive dating of stars
... interest here. Moreover, the diagnostic lines of Th and Hf emerge from low lying energy levels which makes the Boltzmann factor and consequently the temperature sensitivity of the level populations modest. The similar atomic properties of Th and Hf lead to similar formation regions in the photospher ...
... interest here. Moreover, the diagnostic lines of Th and Hf emerge from low lying energy levels which makes the Boltzmann factor and consequently the temperature sensitivity of the level populations modest. The similar atomic properties of Th and Hf lead to similar formation regions in the photospher ...
The first carbon-enhanced metal-poor star found in the Sculptor
... The origin of carbon-enhanced metal-poor (CEMP) stars and their possible connection with the chemical elements produced by the first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way ...
... The origin of carbon-enhanced metal-poor (CEMP) stars and their possible connection with the chemical elements produced by the first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way ...
The Milky Way disk
... same Oort formulae cannot be used outside the solar ring, and other independent distance indicators have to be adopted. Besides this, other limitations are that our galaxy is filled with HI, and apparently inter-arm regions have the same physical size as spiral arms. It is therefore extremely diffic ...
... same Oort formulae cannot be used outside the solar ring, and other independent distance indicators have to be adopted. Besides this, other limitations are that our galaxy is filled with HI, and apparently inter-arm regions have the same physical size as spiral arms. It is therefore extremely diffic ...