Asteroseismology and stellar rotation - IAG-Usp
... Mass loss or transport mechanism is dominant in influencing Prot depending on the mass of the star (M >12 <12Msol) Determination of Prot versus distance from the ZAMS ...
... Mass loss or transport mechanism is dominant in influencing Prot depending on the mass of the star (M >12 <12Msol) Determination of Prot versus distance from the ZAMS ...
Colour-magnitude diagrams of the post
... presence of a blue HB is made more clear in Fig. 3c where essentially no blue MS contamination is seen, and stars in the locus of the blue HB are still seen. A quantitative check of the presence of an HB was carried out by counting stars in frames with different apertures around the cluster center. ...
... presence of a blue HB is made more clear in Fig. 3c where essentially no blue MS contamination is seen, and stars in the locus of the blue HB are still seen. A quantitative check of the presence of an HB was carried out by counting stars in frames with different apertures around the cluster center. ...
Astrometry of Asteroids
... Astrometrical Coordinate systems and the Technique of Astrometry The techniques you will be using for this lab involve the measurement of precise star positions, a technique called astrometry, which is one of the fundamental tools of astronomers. Astrometry, of course, enables us to make charts of o ...
... Astrometrical Coordinate systems and the Technique of Astrometry The techniques you will be using for this lab involve the measurement of precise star positions, a technique called astrometry, which is one of the fundamental tools of astronomers. Astrometry, of course, enables us to make charts of o ...
12C13C1414N21312C/13C3he43He/4He Sub-surface
... evolution of hot massive stars, they may cause observable phenomena at the stellar surface. The reason is that the zones are located very close to the photosphere for some mass interval (see below). Here, we will discuss which observed features in hot stars might be produced by these near surface co ...
... evolution of hot massive stars, they may cause observable phenomena at the stellar surface. The reason is that the zones are located very close to the photosphere for some mass interval (see below). Here, we will discuss which observed features in hot stars might be produced by these near surface co ...
The science case for - Astrophysics
... traditional astronomical categories appropriate to currently available facilities divide the subject into three almost distinct disciplines, broadly Planets, Stars and Galaxies. In the Extremely Large Telescope era we will study planets around stars other than our own Sun, study individual stars in ...
... traditional astronomical categories appropriate to currently available facilities divide the subject into three almost distinct disciplines, broadly Planets, Stars and Galaxies. In the Extremely Large Telescope era we will study planets around stars other than our own Sun, study individual stars in ...
Superbubble Activity in Star-Forming Galaxies M. S. Oey
... will cool and depart from energy conservation. Indeed, whether and how the hot interior cools has long been a major question for superbubble evolution and the fate of the hot gas. Thermal conduction at the interface between the cool shell wall and hot gas should cause a high rate of mass-loading int ...
... will cool and depart from energy conservation. Indeed, whether and how the hot interior cools has long been a major question for superbubble evolution and the fate of the hot gas. Thermal conduction at the interface between the cool shell wall and hot gas should cause a high rate of mass-loading int ...
Dynamical Mass Measurements of Pre-Main
... radial velocities of the primary stars relative to their secondaries (e.g., Rucinski, 1999). These effects can be minimized by selecting templates that are well matched to the target stars in spectral type, by avoiding orbital phases subject to strong line blending, and by employing techniques desig ...
... radial velocities of the primary stars relative to their secondaries (e.g., Rucinski, 1999). These effects can be minimized by selecting templates that are well matched to the target stars in spectral type, by avoiding orbital phases subject to strong line blending, and by employing techniques desig ...
Astrometry of Asteroids
... Astrometrical Coordinate systems and the Technique of Astrometry The techniques you will be using for this lab involve the measurement of precise star positions, a technique called astrometry, which is one of the fundamental tools of astronomers. Astrometry, of course, enables us to make charts of o ...
... Astrometrical Coordinate systems and the Technique of Astrometry The techniques you will be using for this lab involve the measurement of precise star positions, a technique called astrometry, which is one of the fundamental tools of astronomers. Astrometry, of course, enables us to make charts of o ...
Project Description - SDSS-III
... expansion of the Universe. Large-scale imaging and spectroscopic surveys have revealed rich, complex structure in the outer Milky Way, residual traces of the Galaxy’s hierarchical formation history. These surveys have discovered more than a dozen new members of the Local Group of galaxies and identi ...
... expansion of the Universe. Large-scale imaging and spectroscopic surveys have revealed rich, complex structure in the outer Milky Way, residual traces of the Galaxy’s hierarchical formation history. These surveys have discovered more than a dozen new members of the Local Group of galaxies and identi ...
1. INTRODUCTION - Institut für Theoretische Astrophysik
... code, the same height grid, and also employ the same radiation treatment. The starting models are then constructed by using the usual temperature and Ñux correction procedures as discussed by Cuntz, Rammacher, & Ulmschneider (1994). The energy Ñux and spectrum of acoustic waves generated in the conv ...
... code, the same height grid, and also employ the same radiation treatment. The starting models are then constructed by using the usual temperature and Ñux correction procedures as discussed by Cuntz, Rammacher, & Ulmschneider (1994). The energy Ñux and spectrum of acoustic waves generated in the conv ...
- ANU Repository
... that was flat in logarithmic P. Morton & Swift (2014) also found f = 2.0 ± 0.45 for P < 150 d and a similar radius distribution using a weighted density kernel estimation. Dressing & Charbonneau (2015, hereafter DC15) performed an analysis of the Kepler detection efficiency independent of the Kepler p ...
... that was flat in logarithmic P. Morton & Swift (2014) also found f = 2.0 ± 0.45 for P < 150 d and a similar radius distribution using a weighted density kernel estimation. Dressing & Charbonneau (2015, hereafter DC15) performed an analysis of the Kepler detection efficiency independent of the Kepler p ...
A catalogue of the Chandra Deep Field South with multi
... The spectral shapes of the objects in the R-band selected catalogue were measured with a different approach. Photometry in all 17 passbands was done by projecting the object coordinates into the frames of reference of each single exposure and measuring the object fluxes at the given locations. In or ...
... The spectral shapes of the objects in the R-band selected catalogue were measured with a different approach. Photometry in all 17 passbands was done by projecting the object coordinates into the frames of reference of each single exposure and measuring the object fluxes at the given locations. In or ...
Quantitative constraints on starburst cycles in galaxies with stellar
... zero, which are essentially identical to the models in the continuous library, so the new minimum χ2 is guaranteed to be equal to or smaller than the old one. If the new χ2min /Nd lies in the range 2.37-6.25, the probability that the model is consistent with the data is still between 10-50%, so thes ...
... zero, which are essentially identical to the models in the continuous library, so the new minimum χ2 is guaranteed to be equal to or smaller than the old one. If the new χ2min /Nd lies in the range 2.37-6.25, the probability that the model is consistent with the data is still between 10-50%, so thes ...
RApid Temporal Survey-RATS I: Overview and first results
... between frames. For each chip we flat-fielded and bias subtracted each image. The analysis (for each chip) consisted of following steps: the first 5 frames of each field were combined in order to form a ‘master’ image of the field. This master image was then searched for all the sources above a 5σ d ...
... between frames. For each chip we flat-fielded and bias subtracted each image. The analysis (for each chip) consisted of following steps: the first 5 frames of each field were combined in order to form a ‘master’ image of the field. This master image was then searched for all the sources above a 5σ d ...
The Young Stars
... Certain stars in star formation regions have been found to increase in brightness by several orders of magnitude over a period of months to years. These are called FU Orionis eruptive variables, or FU Ori objects. The luminosities can reach a few hundred L . The two best studied members of the clas ...
... Certain stars in star formation regions have been found to increase in brightness by several orders of magnitude over a period of months to years. These are called FU Orionis eruptive variables, or FU Ori objects. The luminosities can reach a few hundred L . The two best studied members of the clas ...
Ursa Major
Ursa Major /ˈɜrsə ˈmeɪdʒər/ (also known as the Great Bear and Charles' Wain) is a constellation in the northern celestial hemisphere. One of the 48 constellations listed by Ptolemy (second century AD), it remains one of the 88 modern constellations. It can be visible throughout the year in most of the northern hemisphere. Its name, Latin for ""the greater (or larger) she-bear"", stands as a reference to and in direct contrast with Ursa Minor, ""the smaller she-bear"", with which it is frequently associated in mythology and amateur astronomy. The constellation's most recognizable asterism, a group of seven relatively bright stars commonly known as the ""Big Dipper"", ""the Wagon"" or ""the Plough"" (among others), both mimicks the shape of the lesser bear (the ""Little Dipper"") and is commonly used as a navigational pointer towards the current northern pole star, Polaris in Ursa Minor. The Big Dipper and the constellation as a whole have mythological significance in numerous world cultures, usually as a symbol of the north.The third largest constellation in the sky, Ursa Major is home to many deep-sky objects including seven Messier objects, four other NGC objects and I Zwicky 18, the youngest known galaxy in the visible universe.