Development of a Software Package for the Reduction and Analysis
... for the reduction and analysis of meteor videos. The uncertainty in determining the position of a meteor was computed to be 0.2−3.0 pixels, with a median value of 0.3 pixels. Sub-pixel accuracy (0.2−0.5 pixels) was also reached for the uncertainties in the astrometric transformation. Different modul ...
... for the reduction and analysis of meteor videos. The uncertainty in determining the position of a meteor was computed to be 0.2−3.0 pixels, with a median value of 0.3 pixels. Sub-pixel accuracy (0.2−0.5 pixels) was also reached for the uncertainties in the astrometric transformation. Different modul ...
STARLAB
... you told the first time. If time allows, show the Earth Cylinder or other cylinders. Try some activities from your Planetarium Activities for Student Success (PASS) volumes. (Did you send in your Product Registration form? See Note.) 6. It’s important that the students realize that you are learning ...
... you told the first time. If time allows, show the Earth Cylinder or other cylinders. Try some activities from your Planetarium Activities for Student Success (PASS) volumes. (Did you send in your Product Registration form? See Note.) 6. It’s important that the students realize that you are learning ...
possible chronological markers in the vedic texts
... little or no information to identify the stellar markers; neither relative position nor the shape of an asterism are given. The number of stars in each naks. atra is of some help, that is, naks. atras whose names are dual probably have two stars and plural names suggest a group of stars. In South As ...
... little or no information to identify the stellar markers; neither relative position nor the shape of an asterism are given. The number of stars in each naks. atra is of some help, that is, naks. atras whose names are dual probably have two stars and plural names suggest a group of stars. In South As ...
CoRoT III programme
... yet and their evolution is the driver of the chemical evolution of the galaxy. Since CoRoT can, contrary to Kepler, observe two very different regions of the Galaxy, it will test whether the planetary system characteristics and star-to-planet ratio are the same in these two regions. In its seismolog ...
... yet and their evolution is the driver of the chemical evolution of the galaxy. Since CoRoT can, contrary to Kepler, observe two very different regions of the Galaxy, it will test whether the planetary system characteristics and star-to-planet ratio are the same in these two regions. In its seismolog ...
The impact of mass-loss on the evolution and pre
... core He-burning stage of all massive stars with masses between about 9 and 25 M . Therefore, a large number of post-Main Sequence massive stars are expected to be in this evolutionary stage. This kind of stars represent the end point of the evolution of about half of the massive stars. When such a ...
... core He-burning stage of all massive stars with masses between about 9 and 25 M . Therefore, a large number of post-Main Sequence massive stars are expected to be in this evolutionary stage. This kind of stars represent the end point of the evolution of about half of the massive stars. When such a ...
The Day We Found the Universe
... spiraling nebulae were nothing less than separate galaxies. At the same time, a few hundred miles south at Mount Wilson, near Los Angeles, Harlow Shapley resized the Milky Way, measuring it as far larger than previously thought and shoving our Sun o to the side, away from the galaxy's hub. As Shaple ...
... spiraling nebulae were nothing less than separate galaxies. At the same time, a few hundred miles south at Mount Wilson, near Los Angeles, Harlow Shapley resized the Milky Way, measuring it as far larger than previously thought and shoving our Sun o to the side, away from the galaxy's hub. As Shaple ...
The Lupus clouds - European Southern Observatory
... The Lupus clouds are projected on the sky against the nearest and one of the best studied OB associations, Scorpius-Centaurus (e.g. Blaauw 1991, de Geus et al. 1989, de Geus 1992, Preibisch et al. 2002; see also chapter by Preibisch & Mamajek). The Scorpius-Centaurus association is a vast complex in ...
... The Lupus clouds are projected on the sky against the nearest and one of the best studied OB associations, Scorpius-Centaurus (e.g. Blaauw 1991, de Geus et al. 1989, de Geus 1992, Preibisch et al. 2002; see also chapter by Preibisch & Mamajek). The Scorpius-Centaurus association is a vast complex in ...
The most metal-poor galaxies
... is found to depend on their age, and depends on which elements are investigated. That a star or nebula is deficient of a certain element does not automatically mean that the overall chemical abundances are low. Thus, one must be careful in defining what metallicity means for a given galaxy before co ...
... is found to depend on their age, and depends on which elements are investigated. That a star or nebula is deficient of a certain element does not automatically mean that the overall chemical abundances are low. Thus, one must be careful in defining what metallicity means for a given galaxy before co ...
Star Formation in the Milky Way and Nearby Galaxies Further
... between the community studying individual star-forming regions and stars in the Milky Way (MW; also sometimes referred to as the Galaxy) and the largely extragalactic community that attempts to characterize the star-formation process on galactic and cosmological scales. Some aspects of this separati ...
... between the community studying individual star-forming regions and stars in the Milky Way (MW; also sometimes referred to as the Galaxy) and the largely extragalactic community that attempts to characterize the star-formation process on galactic and cosmological scales. Some aspects of this separati ...
Here - NASA/IPAC Extragalactic Database
... the morphology of H ii regions is generally rather complex on all scales. Typical hydrogen densities n are 103 – 104 cm−3 for compact H ii regions. The average densities in giant extragalactic H ii regions are lower, typically 102 cm−3 since giant H ii regions encompass also zones of diffuse materia ...
... the morphology of H ii regions is generally rather complex on all scales. Typical hydrogen densities n are 103 – 104 cm−3 for compact H ii regions. The average densities in giant extragalactic H ii regions are lower, typically 102 cm−3 since giant H ii regions encompass also zones of diffuse materia ...
Europium, Samarium, and Neodymium Isotopic Fractions in Metal
... exhibits radial velocity variations (Lucatello et al. 2005), indicating that it is a member of a binary or multiple star system. These characteristics have led to the classification of HD 196944 as a carbon-enhanced metal-poor senriched (CEMP-s) star, as defined in Beers & Christlieb (2005). Gallino ...
... exhibits radial velocity variations (Lucatello et al. 2005), indicating that it is a member of a binary or multiple star system. These characteristics have led to the classification of HD 196944 as a carbon-enhanced metal-poor senriched (CEMP-s) star, as defined in Beers & Christlieb (2005). Gallino ...
Lichtenknecker- Database of the BAV
... For some stars changes in their name were published in Namelist 78 (IBVS 5721) because of more precise measurement of the position. If an "old" starname is entered it is recognized automatically and changed to the new name. A hint about this is displayed below the starname (see picture 7). ...
... For some stars changes in their name were published in Namelist 78 (IBVS 5721) because of more precise measurement of the position. If an "old" starname is entered it is recognized automatically and changed to the new name. A hint about this is displayed below the starname (see picture 7). ...
Tidal Effects on the Oort Cloud Comets and Dynamics of the Sun in
... The Solar System presents a complex dynamical structure and is not isolated from the Galaxy. In particular the comet reservoir of our planetary system, the Oort cloud, is extremely sensitive to the the galactic environment due to its peripheral collocation inside the Solar System. In this framework, ...
... The Solar System presents a complex dynamical structure and is not isolated from the Galaxy. In particular the comet reservoir of our planetary system, the Oort cloud, is extremely sensitive to the the galactic environment due to its peripheral collocation inside the Solar System. In this framework, ...
Galaxy Disks Further
... Despite the correlations between overall properties, there are galaxies with very similar properties but very different morphologies. M33 and the Large Magellanic Cloud (LMC) provide an example. Both galaxies have very similar central surface brightnesses (∼21.2 B-mag arcsec−2 ), scalelengths (∼1.6 ...
... Despite the correlations between overall properties, there are galaxies with very similar properties but very different morphologies. M33 and the Large Magellanic Cloud (LMC) provide an example. Both galaxies have very similar central surface brightnesses (∼21.2 B-mag arcsec−2 ), scalelengths (∼1.6 ...
An Atlas of Stellar Spectra
... sequence are not touched on; as a consequence, emphasis is placed on ``ordinary'' stars. These are the stars most important statistically and the only ones suitable for large-scale investigations of galactic structure. The plan of the Atlas can be stated as follows: a) To set up a classification sys ...
... sequence are not touched on; as a consequence, emphasis is placed on ``ordinary'' stars. These are the stars most important statistically and the only ones suitable for large-scale investigations of galactic structure. The plan of the Atlas can be stated as follows: a) To set up a classification sys ...
Radio Emission Toward Regions of Massive Star Formation
... stars with accretion disks and bipolar outflows have been directly observed (Kraus et al. 2010). Therefore, there must be some other important physics simple models do not take into account. The review by Zinnecker & Yorke (2007) discusses three prevailing theories: monolithic collapse in cores with ...
... stars with accretion disks and bipolar outflows have been directly observed (Kraus et al. 2010). Therefore, there must be some other important physics simple models do not take into account. The review by Zinnecker & Yorke (2007) discusses three prevailing theories: monolithic collapse in cores with ...
Astronomy
... few milliseconds to thousands of seconds before fading away. Only 10% of gamma-ray sources are non-transient sources. These steady gamma-ray emitters include pulsars, neutron stars, and black hole candidates such as active galactic nuclei.[33] ...
... few milliseconds to thousands of seconds before fading away. Only 10% of gamma-ray sources are non-transient sources. These steady gamma-ray emitters include pulsars, neutron stars, and black hole candidates such as active galactic nuclei.[33] ...
Observations and Theory of Dynamical Triggers for Star Formation
... been found in the Sco-Cen association (Bertoldi & Jenkins 1992). Some of these neutral regions may be protostellar disks, as argued in the papers on Orion, but Hester et al. (1996) claims that many are evaporating globules rather than disks. This follows from the short exposure times of the neutral ...
... been found in the Sco-Cen association (Bertoldi & Jenkins 1992). Some of these neutral regions may be protostellar disks, as argued in the papers on Orion, but Hester et al. (1996) claims that many are evaporating globules rather than disks. This follows from the short exposure times of the neutral ...
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.