Stellarium User Guide
... scipting facility is Stellarium’s version of a “Presentation”, a feature that may be used to run an astronomical or other presentation for instruction or entertainment from within the Stellarium program. The original Stratoscript was quite limited in what it could do so a new Stellarium Scripting Sy ...
... scipting facility is Stellarium’s version of a “Presentation”, a feature that may be used to run an astronomical or other presentation for instruction or entertainment from within the Stellarium program. The original Stratoscript was quite limited in what it could do so a new Stellarium Scripting Sy ...
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... predictions of the density-wave theory with the observed spiral structure and for estimating the pattern velocity (ωp) of the density wave. In the present investigation, however, we have used birthsites of the classical Cepheids to study the local variation of metallicity in the galactic disc. The p ...
... predictions of the density-wave theory with the observed spiral structure and for estimating the pattern velocity (ωp) of the density wave. In the present investigation, however, we have used birthsites of the classical Cepheids to study the local variation of metallicity in the galactic disc. The p ...
maximum likelihood fitting of tidal streams with application
... of a particular set of parameters given the data and the model into the product of two terms, the first being the likelihood of the parameters and the second being the prior probability of the parameters. When the prior probability distribution over the parameters is uniform (as is typically assumed ...
... of a particular set of parameters given the data and the model into the product of two terms, the first being the likelihood of the parameters and the second being the prior probability of the parameters. When the prior probability distribution over the parameters is uniform (as is typically assumed ...
The Kuiper Belt Explored by Serendipitous Stellar Occultations
... The possibility of exploring the Kuiper belt by searching for fortuitous stellar occultations has been under development for several years. This technique has the potential to permit exploration of the Kuiper belt down to objects of subkilometer radius. High-speed photometric observations provide li ...
... The possibility of exploring the Kuiper belt by searching for fortuitous stellar occultations has been under development for several years. This technique has the potential to permit exploration of the Kuiper belt down to objects of subkilometer radius. High-speed photometric observations provide li ...
Statistical properties of a sample of periodically variable B-type supergiants ⋆
... We selected all southern stars of luminosity class I or II brighter than 9th mag in the sample by Waelkens et al. (1998) which fitted the observation window of the assigned telescope time. This concerns 21 stars. To this we added 10 more candidate α Cyg variables from the Catalogue of Periodic Varia ...
... We selected all southern stars of luminosity class I or II brighter than 9th mag in the sample by Waelkens et al. (1998) which fitted the observation window of the assigned telescope time. This concerns 21 stars. To this we added 10 more candidate α Cyg variables from the Catalogue of Periodic Varia ...
Pulsed Accretion in the Young Binary &
... these have been identified as possible sites for the study of early stellar evolution and planetary formation. Stellar formation starts when a gravitational collapse is triggered in dense regions of slowly rotating gaseous clouds. As the gravitational force depends on the inverse-square of the dista ...
... these have been identified as possible sites for the study of early stellar evolution and planetary formation. Stellar formation starts when a gravitational collapse is triggered in dense regions of slowly rotating gaseous clouds. As the gravitational force depends on the inverse-square of the dista ...
The spectroscopic Hertzsprung
... The Hertzsprung-Russell (HR) diagram has been an important diagram for the understanding of stellar evolution for more than a hundred years (Nielsen 1964). Hertzsprung (1905) and later independently Russell (1919) realized that the knowledge of the absolute brightness of stars together with their sp ...
... The Hertzsprung-Russell (HR) diagram has been an important diagram for the understanding of stellar evolution for more than a hundred years (Nielsen 1964). Hertzsprung (1905) and later independently Russell (1919) realized that the knowledge of the absolute brightness of stars together with their sp ...
Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of
... important books in the history of Arabic and Islamic astronomy. This book was called Șuwar al-Kawākib al-Thamāniyah wa-al-Ārba'een, later known by its short name The Book of the Fixed Stars. It was written in Arabic by the famous Persian author and astronomer ′Abd alRaḥmān al-Ṣūfī around A.D. 964. E ...
... important books in the history of Arabic and Islamic astronomy. This book was called Șuwar al-Kawākib al-Thamāniyah wa-al-Ārba'een, later known by its short name The Book of the Fixed Stars. It was written in Arabic by the famous Persian author and astronomer ′Abd alRaḥmān al-Ṣūfī around A.D. 964. E ...
Article PDF - IOPscience
... light curves (12 epochs in each of five bands, taken over a 4.5 year period). We present a novel template fitting technique that uses well-defined and physically motivated multi-band light curves of RR Lyrae stars, and demonstrate that we get accurate period estimates, precise to 2 s in >80% of cases. ...
... light curves (12 epochs in each of five bands, taken over a 4.5 year period). We present a novel template fitting technique that uses well-defined and physically motivated multi-band light curves of RR Lyrae stars, and demonstrate that we get accurate period estimates, precise to 2 s in >80% of cases. ...
A spectroscopic investigation of the O-type star - ORBi
... if in the cases where significant variations of the RVs are measured on all the spectral lines without any periodic motion, the object will be labelled as a “binary candidate”. Finally, we also calculate the Temporal Variance Spectrum (TVS, Fullerton et al. 1996) to search for line profile variation ...
... if in the cases where significant variations of the RVs are measured on all the spectral lines without any periodic motion, the object will be labelled as a “binary candidate”. Finally, we also calculate the Temporal Variance Spectrum (TVS, Fullerton et al. 1996) to search for line profile variation ...
A Search for Extrasolar Planets Using Echoes Produced in Flare
... The two-ribbon flare begins with a filament, essentially a mass of cool charged particles producing a line current suspended in a magnetic field “tube” extending through the stellar atmosphere (Haisch et. al., 1991; Martens and Kuin, 1989). The connection points of the line current with the photosph ...
... The two-ribbon flare begins with a filament, essentially a mass of cool charged particles producing a line current suspended in a magnetic field “tube” extending through the stellar atmosphere (Haisch et. al., 1991; Martens and Kuin, 1989). The connection points of the line current with the photosph ...
A catalogue of the Chandra Deep Field South with multi
... which is 31 5 30 in size. This catalogue lists astrometry, photometry in 17 passbands from 350 to 930 nm, and ground-based morphological data for 63,501 objects. The catalogue also contains multi-colour classification into the categories Star, Galaxy and Quasar as well as photometric redshifts. We i ...
... which is 31 5 30 in size. This catalogue lists astrometry, photometry in 17 passbands from 350 to 930 nm, and ground-based morphological data for 63,501 objects. The catalogue also contains multi-colour classification into the categories Star, Galaxy and Quasar as well as photometric redshifts. We i ...
The isotopic mixture of barium in the metal-poor
... occur in the helium and carbon shells of massive stars in their hydrostatic burning phases. The r-process is likely associated with the deep interior of Type II supernovae. Since massive stars dying as Type II supernovae evolve faster than the stars that populate and evolve from the AGB, one anticip ...
... occur in the helium and carbon shells of massive stars in their hydrostatic burning phases. The r-process is likely associated with the deep interior of Type II supernovae. Since massive stars dying as Type II supernovae evolve faster than the stars that populate and evolve from the AGB, one anticip ...
A spectroscopic investigation of the O
... 2. Observations and binary criteria Deriving the binary fraction of a given population requires an intense survey of the stars but also a good time sampling to constrain the short- as well as the long-period systems. This monitoring has to be as homogeneous as possible because combining data from th ...
... 2. Observations and binary criteria Deriving the binary fraction of a given population requires an intense survey of the stars but also a good time sampling to constrain the short- as well as the long-period systems. This monitoring has to be as homogeneous as possible because combining data from th ...
2 Statistical properties of a sample of periodically variable B-type supergiants
... the solar neighbourhood with unprecedented precision of 2 milli-arcsecond for the parallax. This was achieved by measuring each star on average 100 times during the 3.3 years lifetime of the mission. These time series are very different from those obtained with ground-based instruments, in the sense ...
... the solar neighbourhood with unprecedented precision of 2 milli-arcsecond for the parallax. This was achieved by measuring each star on average 100 times during the 3.3 years lifetime of the mission. These time series are very different from those obtained with ground-based instruments, in the sense ...
The spectroscopic Hertzsprung-Russell diagram
... the understanding of stellar evolution since more than hundred years (Nielsen 1964). Hertzsprung (1905) and later independently Russell (1919) realized that the knowledge of the absolute brightness of stars, or at least of the absolute brightness differences, together with their spectral type or sur ...
... the understanding of stellar evolution since more than hundred years (Nielsen 1964). Hertzsprung (1905) and later independently Russell (1919) realized that the knowledge of the absolute brightness of stars, or at least of the absolute brightness differences, together with their spectral type or sur ...
Open clusters and associations in the Gaia era
... and distance (for clusters only - for associations, individual parallax measurements are mandatory to take each star distance into account), their location in the HR diagram defines an isochrone whose color and luminosity can be used to distinguish members from field interlopers. Deep large scale ph ...
... and distance (for clusters only - for associations, individual parallax measurements are mandatory to take each star distance into account), their location in the HR diagram defines an isochrone whose color and luminosity can be used to distinguish members from field interlopers. Deep large scale ph ...
Silicon isotopic abundance toward evolved stars and its application
... stars were born and the different ratios are the results of different ages, which mainly depend on their masses and metallicities. The other possibility is that the stellar evolution can significantly change the silicon isotope ratios. The first possibility implies that the 29 Si/30 Si ratio in the IS ...
... stars were born and the different ratios are the results of different ages, which mainly depend on their masses and metallicities. The other possibility is that the stellar evolution can significantly change the silicon isotope ratios. The first possibility implies that the 29 Si/30 Si ratio in the IS ...
Astronomers` Observing Guides
... and edification to those that actually have the potential of contributing to the science of double star astronomy itself. The highlight of the second section (and, indeed, perhaps of the entire book!) are two carefully compiled observing rosters – one showcasing 100 of the sky’s finest double and mult ...
... and edification to those that actually have the potential of contributing to the science of double star astronomy itself. The highlight of the second section (and, indeed, perhaps of the entire book!) are two carefully compiled observing rosters – one showcasing 100 of the sky’s finest double and mult ...
Article PDF - IOPscience
... the volume of the NSTARS database, the goal of which is to compile information on all possible stellar sources near the Sun, in order to achieve a better understanding of the local stellar population. As Holberg et al. (2002) further discussed in their work, the volume defined by this 20 pc limit wa ...
... the volume of the NSTARS database, the goal of which is to compile information on all possible stellar sources near the Sun, in order to achieve a better understanding of the local stellar population. As Holberg et al. (2002) further discussed in their work, the volume defined by this 20 pc limit wa ...
exploring anticorrelations and light element variations
... literature. Targets were selected as cluster members if (1) there is published abundance information on the star as a cluster member, (2) the star is a radial velocity member, or (3) if it has a probability >50% of being a cluster member based on their proper motion adopted from the literature. Afte ...
... literature. Targets were selected as cluster members if (1) there is published abundance information on the star as a cluster member, (2) the star is a radial velocity member, or (3) if it has a probability >50% of being a cluster member based on their proper motion adopted from the literature. Afte ...
PDF - ASSA
... and False Crosses, this amazing variable star requires no optical aid to follow throughout its light cycle. Even under average urban sky conditions, without the need for a telescope or even binoculars, it can be seen to vary between magnitudes 3.4 and 4.1 over a period of 35.5 days. The light curve ...
... and False Crosses, this amazing variable star requires no optical aid to follow throughout its light cycle. Even under average urban sky conditions, without the need for a telescope or even binoculars, it can be seen to vary between magnitudes 3.4 and 4.1 over a period of 35.5 days. The light curve ...
Ages of young stars
... rapidly. This creates a sharp, age-dependent, lithium depletion boundary (LDB) between stars at low luminosities retaining all their initial Li and those at only slightly higher luminosities with total Li depletion. The LDB technique is “semi-fundamental” because it relies on well-understood physics ...
... rapidly. This creates a sharp, age-dependent, lithium depletion boundary (LDB) between stars at low luminosities retaining all their initial Li and those at only slightly higher luminosities with total Li depletion. The LDB technique is “semi-fundamental” because it relies on well-understood physics ...
celestial navigation heaven`s guide for mere
... the galaxy, one of several events might occur to cause its gravitational collapse. GMCs may either collide with each other or pass through dense regions of spiral arms. Spiral arms are regions of stars which extend from the centre of spiral and barred spiral galaxies. Sometimes, nearby supernova exp ...
... the galaxy, one of several events might occur to cause its gravitational collapse. GMCs may either collide with each other or pass through dense regions of spiral arms. Spiral arms are regions of stars which extend from the centre of spiral and barred spiral galaxies. Sometimes, nearby supernova exp ...
Ages of Young Stars
... rapidly. This creates a sharp, age-dependent, lithium depletion boundary (LDB) between stars at low luminosities retaining all their initial Li and those at only slightly higher luminosities with total Li depletion. The LDB technique is “semi-fundamental” because it relies on well-understood physics ...
... rapidly. This creates a sharp, age-dependent, lithium depletion boundary (LDB) between stars at low luminosities retaining all their initial Li and those at only slightly higher luminosities with total Li depletion. The LDB technique is “semi-fundamental” because it relies on well-understood physics ...
Star catalogue
A star catalogue, or star catalog, is an astronomical catalogue that lists stars. In astronomy, many stars are referred to simply by catalogue numbers. There are a great many different star catalogues which have been produced for different purposes over the years, and this article covers only some of the more frequently quoted ones. Star catalogues were compiled by many different ancient peoples, including the Babylonians, Greeks, Chinese, Persians, and Arabs. Most modern catalogues are available in electronic format and can be freely downloaded from NASA's Astronomical Data Center.Completeness and accuracy is described by the weakest apparent magnitude V (largest number) and the accuracy of the positions.