Giant molecular clouds in the Local Group galaxy M 33⋆⋆⋆
... We present an analysis of a systematic CO(2–1) survey at 1200 resolution covering most of the Local Group spiral M 33, which, at a distance of 840 kpc, is close enough for individual giant molecular clouds (GMCs) to be identified. The goal of this work is to study the properties of the GMCs in this ...
... We present an analysis of a systematic CO(2–1) survey at 1200 resolution covering most of the Local Group spiral M 33, which, at a distance of 840 kpc, is close enough for individual giant molecular clouds (GMCs) to be identified. The goal of this work is to study the properties of the GMCs in this ...
The masses and spins of neutron stars and stellar
... of isolated neutron stars except perhaps by microlensing (and then the identification of the object as a neutron star is not certain). The current spins of pulsars are obviously straightforward to measure, but these spins have been affected strongly by magnetic spindown. However, as we discuss in Se ...
... of isolated neutron stars except perhaps by microlensing (and then the identification of the object as a neutron star is not certain). The current spins of pulsars are obviously straightforward to measure, but these spins have been affected strongly by magnetic spindown. However, as we discuss in Se ...
Stellar Intensity Interferometry: The Background John Davis Sydney Institute for Astronomy
... and Cassiopeia A, were unknown and some thought they were “radio stars”. Robert Hanbury Brown (RHB) was determined to measure them • If these sources were galaxies their angular sizes would be of the order of a minute of arc and easy to measure with a conventional interferometer but, if they were s ...
... and Cassiopeia A, were unknown and some thought they were “radio stars”. Robert Hanbury Brown (RHB) was determined to measure them • If these sources were galaxies their angular sizes would be of the order of a minute of arc and easy to measure with a conventional interferometer but, if they were s ...
Astronomy Astrophysics Excitation of solar-like oscillations across the HR diagram &
... Aims. We extend semi-analytical computations of excitation rates for solar oscillation modes to those of other solar-like oscillating stars to compare them with recent observations Methods. Numerical 3D simulations of surface convective zones of several solar-type oscillating stars are used to chara ...
... Aims. We extend semi-analytical computations of excitation rates for solar oscillation modes to those of other solar-like oscillating stars to compare them with recent observations Methods. Numerical 3D simulations of surface convective zones of several solar-type oscillating stars are used to chara ...
Understanding Variable Stars - Central Florida Astronomical Society
... Understanding Variable Stars Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique ...
... Understanding Variable Stars Variable stars are those that change brightness. Their variability may be due to geometric processes such as rotation, or eclipse by a companion star, or physical processes such as vibration, flares, or cataclysmic explosions. In each case, variable stars provide unique ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... subdwarfs and main sequence tting. The results are compared with other distance measurements to the Large Magellanic Cloud and M31. 3. Radial velocities of the Milky Way clusters are used to derive the kinematics of various subsamples of the clusters (the mean rotation speed about the Galactic cent ...
... subdwarfs and main sequence tting. The results are compared with other distance measurements to the Large Magellanic Cloud and M31. 3. Radial velocities of the Milky Way clusters are used to derive the kinematics of various subsamples of the clusters (the mean rotation speed about the Galactic cent ...
The CCD Photometric Calibration Cookbook
... CCD (Charge-Coupled Device) photometric calibration is concerned with converting the arbitrary units in which CCD images are recorded into standard, reproducible units. In principle the observed brightness could be calibrated into genuine physical units, such as W m , and indeed this is occasionally ...
... CCD (Charge-Coupled Device) photometric calibration is concerned with converting the arbitrary units in which CCD images are recorded into standard, reproducible units. In principle the observed brightness could be calibrated into genuine physical units, such as W m , and indeed this is occasionally ...
T3-Cosmic Star Formation History
... metals and ejected. (In this review, the term “yield” generally indicates the net yield y of a stellar population as defined in Equation 7; instead, we explicitly speak of “stellar yields” to indicate the ym resulting from nucleosynthesis calculations.) The above equations have been written under the ...
... metals and ejected. (In this review, the term “yield” generally indicates the net yield y of a stellar population as defined in Equation 7; instead, we explicitly speak of “stellar yields” to indicate the ym resulting from nucleosynthesis calculations.) The above equations have been written under the ...
- Isaac Newton Group of Telescopes
... to derive its spectral classification and an estimate of its effective surface temperature, which turned out to be some 2350 K. The spectrum allowed to infere a velocity measurement of this object in regard to the Sun, which happened to be very similar to that of the stars in the cluster. All the en ...
... to derive its spectral classification and an estimate of its effective surface temperature, which turned out to be some 2350 K. The spectrum allowed to infere a velocity measurement of this object in regard to the Sun, which happened to be very similar to that of the stars in the cluster. All the en ...
Unfolding the Milky Way bulge - International Max Planck Research
... corresponds to the same resolution described in Fig. 2. The blue dashed line shows the relation E(J − H) = 0.638E(J − K s ) corresponding to the extinction law from Cardelli et al. (1989) and red solid line to E(J − H) = 0.671E(J − K s ) from Nishiyama et al. (2009) . . . . . . . . . . . . . . . . . ...
... corresponds to the same resolution described in Fig. 2. The blue dashed line shows the relation E(J − H) = 0.638E(J − K s ) corresponding to the extinction law from Cardelli et al. (1989) and red solid line to E(J − H) = 0.671E(J − K s ) from Nishiyama et al. (2009) . . . . . . . . . . . . . . . . . ...
Astronomy Astrophysics
... disk, and the competing influences of cluster formation and disruption that shape the properties of the current cluster population. However, to draw reliable conclusions, a sizable sample exhibiting accurately and homogeneously determined properties is desirable. The new generation of all-sky survey ...
... disk, and the competing influences of cluster formation and disruption that shape the properties of the current cluster population. However, to draw reliable conclusions, a sizable sample exhibiting accurately and homogeneously determined properties is desirable. The new generation of all-sky survey ...
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... Testing the validity of the theoretical model of stochastic excitation with the help of 3D simulations of the outer layers of stellar models is the main goal of the present paper. For that purpose, we compare the p-mode excitation rates for stars with different temperatures and luminosities as obtai ...
... Testing the validity of the theoretical model of stochastic excitation with the help of 3D simulations of the outer layers of stellar models is the main goal of the present paper. For that purpose, we compare the p-mode excitation rates for stars with different temperatures and luminosities as obtai ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... Way! Elmegreen & Scalo (2006) provide a detailed exploration of the degeneracies involved in inferring a stellar population’s IMF from its measured PDMF and adopted SFH. It is somewhat disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the plac ...
... Way! Elmegreen & Scalo (2006) provide a detailed exploration of the degeneracies involved in inferring a stellar population’s IMF from its measured PDMF and adopted SFH. It is somewhat disconcerting that the break from the Salpeter law identified in many IMF studies needs to be invoked near the plac ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... resolution is required in order to detect supernovae in the extremely bright nuclear environments of LIRGs. Alternatively, infrared spectroscopy would reveal the telltale spectral features of nuclear supernovae. Spectroscopic observations of the Arp 220 nuclei were conducted using Keck in July 2013 ...
... resolution is required in order to detect supernovae in the extremely bright nuclear environments of LIRGs. Alternatively, infrared spectroscopy would reveal the telltale spectral features of nuclear supernovae. Spectroscopic observations of the Arp 220 nuclei were conducted using Keck in July 2013 ...
X-ray astronomy of stellar coronae (Review)
... solar corona has been admired in scattered visible light ever since humans first wondered about solar eclipses, but only during the last very few decades have we started to seriously grasp solutions to some of the fundamental astrophysical problems within the field of solar and stellar astronomy. Ma ...
... solar corona has been admired in scattered visible light ever since humans first wondered about solar eclipses, but only during the last very few decades have we started to seriously grasp solutions to some of the fundamental astrophysical problems within the field of solar and stellar astronomy. Ma ...
- National Optical Astronomy Observatory
... magnetic field lines unless there was an indirect mechanism for their flow, namely, other materials that are directed by the magnetic field. The data seems to indicate that the mechanism for the nickel’s movement is not the flow of iron directed by the magnetic fields. The nickel displays greater va ...
... magnetic field lines unless there was an indirect mechanism for their flow, namely, other materials that are directed by the magnetic field. The data seems to indicate that the mechanism for the nickel’s movement is not the flow of iron directed by the magnetic fields. The nickel displays greater va ...
Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of
... translating the main sections of this book. The other objective was to try and point out the importance of this author and this book in the history of astronomy. I found that al-Ṣūfī’s ...
... translating the main sections of this book. The other objective was to try and point out the importance of this author and this book in the history of astronomy. I found that al-Ṣūfī’s ...
Observations, Modeling and Theory of Debris Disks
... Observations of debris disks help not only to study the properties of individual disks, but also to ascertain their incidence and their correlation with stellar properties – e.g., age, spectral type, metallicity, stellar and/or planetary companions. Therefore, their study is imperative to understand ...
... Observations of debris disks help not only to study the properties of individual disks, but also to ascertain their incidence and their correlation with stellar properties – e.g., age, spectral type, metallicity, stellar and/or planetary companions. Therefore, their study is imperative to understand ...
Observations, Modeling and Theory of Debris Disks
... Observations of debris disks help not only to study the properties of individual disks, but also to ascertain their incidence and their correlation with stellar properties – e.g., age, spectral type, metallicity, stellar and/or planetary companions. Therefore, their study is imperative to understand ...
... Observations of debris disks help not only to study the properties of individual disks, but also to ascertain their incidence and their correlation with stellar properties – e.g., age, spectral type, metallicity, stellar and/or planetary companions. Therefore, their study is imperative to understand ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.