The Lupus clouds - European Southern Observatory
... evolution and perhaps the origin of the complex. The entire variety of objects related to the various stages of early stellar evolution are represented in Lupus, including some of the best studied T Tauri stars like RU Lup. The determination of many properties of the clouds, as well as their associa ...
... evolution and perhaps the origin of the complex. The entire variety of objects related to the various stages of early stellar evolution are represented in Lupus, including some of the best studied T Tauri stars like RU Lup. The determination of many properties of the clouds, as well as their associa ...
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 ...
THE COMET`S TALE - Institute of Astronomy
... Than Ours, from his Sunday school library which led him to an interest in astronomy. This interest was further inspired by the conjunction of Jupiter and Mars on May 7th, 1879, when the planets were slightly over one degree apart, and/or July 22nd, 1881, when the two planets were separated by only s ...
... Than Ours, from his Sunday school library which led him to an interest in astronomy. This interest was further inspired by the conjunction of Jupiter and Mars on May 7th, 1879, when the planets were slightly over one degree apart, and/or July 22nd, 1881, when the two planets were separated by only s ...
Communications in Asteroseismology
... about in order not to lose valuable time. The answer to the second question, however, is hidden in a rather long story which the participants of this workshop have now been told. In short, a long chain of events made one of the organizers make a joke, resulting in a full hall of variable-star resear ...
... about in order not to lose valuable time. The answer to the second question, however, is hidden in a rather long story which the participants of this workshop have now been told. In short, a long chain of events made one of the organizers make a joke, resulting in a full hall of variable-star resear ...
The Evolution of Star Formation Activity in . Cory R. Wagner
... Snyder et al. (2012, hereafter S12) found that red-sequence members have roughly constant stellar ages across 1.0 < z < 1.5—indicating that star formation must be ongoing—and bluer and more stochastic colors at 1.0 < z < 1.3 than would be expected of a passive population. Zeimann et al. (2013), B13, ...
... Snyder et al. (2012, hereafter S12) found that red-sequence members have roughly constant stellar ages across 1.0 < z < 1.5—indicating that star formation must be ongoing—and bluer and more stochastic colors at 1.0 < z < 1.3 than would be expected of a passive population. Zeimann et al. (2013), B13, ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
... these heavily reddened clusters remained surprisingly poor, and even today there are still a few clusters with exceptionally high reddenings embedded deep in the Galactic bulge about which we know almost nothing (see the listings in Harris 1996a). However, progress over the years has been steady and ...
Understanding Variable Stars - Central Florida Astronomical Society
... perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and ...
... perspective, an introduction to stars in general, the techniques for discovering and studying variable stars, and a description of the main types of variable stars. It ends with short reflections about the connection between the study of variable stars, and research, education, amateur astronomy, and ...
A spectroscopic study of detached binary systems using precise radial velocities
... The orbital periods of these systems range from about 10 days to 26 years, with a median of about 6 years. Orbital solutions were determined for the seven systems with shorter periods. The measurement of the mass ratio of the longest-period system, HD 217166, demonstrates that this important astroph ...
... The orbital periods of these systems range from about 10 days to 26 years, with a median of about 6 years. Orbital solutions were determined for the seven systems with shorter periods. The measurement of the mass ratio of the longest-period system, HD 217166, demonstrates that this important astroph ...
Clusters: age scales for stellar physics
... were identified as the culprit (Bethe 1939). This is an important lesson: pieces which do not match in this enormous puzzle (our understanding of natural phenomena) do provide, eventually, very interesting hints for new avenues and discoveries. Age and related issues belong to this category. In the ...
... were identified as the culprit (Bethe 1939). This is an important lesson: pieces which do not match in this enormous puzzle (our understanding of natural phenomena) do provide, eventually, very interesting hints for new avenues and discoveries. Age and related issues belong to this category. In the ...
Book Describing Techniques to Detect Transiting ExoPlanets
... regular intervals (~3 days, typically), a larger aperture telescope with good spatial resolution must be used to determine if the brightest star in the survey camera’s image faded a small amount or a nearby fainter star faded by a large amount (e.g., an eclipsing binary). Amateur telescopes are capa ...
... regular intervals (~3 days, typically), a larger aperture telescope with good spatial resolution must be used to determine if the brightest star in the survey camera’s image faded a small amount or a nearby fainter star faded by a large amount (e.g., an eclipsing binary). Amateur telescopes are capa ...
Spectroscopic Atlas for Amateur Astronomers
... 13 Herbig Ae/Be and T Tauri Protostars ......................................................................... 48 14 Spectral Class A............................................................................................................. 53 15 Spectral Class F ................................ ...
... 13 Herbig Ae/Be and T Tauri Protostars ......................................................................... 48 14 Spectral Class A............................................................................................................. 53 15 Spectral Class F ................................ ...
Type Ia Supernovae
... themselves have been studied well over the past 75 years. We now know that there are two main physical causes of these cataclysmic events. One of these channels is the collapse of the core of a massive star. The observationally motivated classes Type II, Type Ib and Type Ic have been attributed to t ...
... themselves have been studied well over the past 75 years. We now know that there are two main physical causes of these cataclysmic events. One of these channels is the collapse of the core of a massive star. The observationally motivated classes Type II, Type Ib and Type Ic have been attributed to t ...
Article PDF - IOPscience
... Pan-STARRS1 (Kaiser et al. 2010, PS1) is a wide-field optical/near-IR survey telescope system located at the Haleakalā Observatory on the island of Maui in Hawai‘i. The largest survey undertaken by the telescope, the PS1 3p survey (Chambers 2011), has observed the entire sky north of decl. -30 in fi ...
... Pan-STARRS1 (Kaiser et al. 2010, PS1) is a wide-field optical/near-IR survey telescope system located at the Haleakalā Observatory on the island of Maui in Hawai‘i. The largest survey undertaken by the telescope, the PS1 3p survey (Chambers 2011), has observed the entire sky north of decl. -30 in fi ...
A Variability Study of the Typical Red Supergiant Antares A
... Red giants and red supergiants have long been known to be variable. In the last 40 years many of the features of this variability have been associated with large convective cells. Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the brigh ...
... Red giants and red supergiants have long been known to be variable. In the last 40 years many of the features of this variability have been associated with large convective cells. Unfortunately, due to the long timescales of these variations they are not well studied, with the exception of the brigh ...
DUSTiNGS III: Distribution of Intermediate
... in the near-infrared, carbon-rich AGB stars were photometrically separated from the RGB population in a few Local Group dwarf galaxies (Albert et al. 2000; Battinelli & Demers 2000; Demers & Battinelli 2002; Letarte et al. 2002; Demers et al. 2004; Battinelli & Demers 2004c,b,a). Based on comparison ...
... in the near-infrared, carbon-rich AGB stars were photometrically separated from the RGB population in a few Local Group dwarf galaxies (Albert et al. 2000; Battinelli & Demers 2000; Demers & Battinelli 2002; Letarte et al. 2002; Demers et al. 2004; Battinelli & Demers 2004c,b,a). Based on comparison ...
X. Nuclear star clusters in low-mass early-type galaxies
... sizes of the NSCs, although not without some uncertainty, since also a widely accepted theory for the formation of GCs is still lacking. Bekki et al. (2004) present scaling relations for the sizes of NSCs based on N-body simulations of the merging of equal-mass star clusters; however, they do not pr ...
... sizes of the NSCs, although not without some uncertainty, since also a widely accepted theory for the formation of GCs is still lacking. Bekki et al. (2004) present scaling relations for the sizes of NSCs based on N-body simulations of the merging of equal-mass star clusters; however, they do not pr ...
Luminosity profiles and sizes of massive star clusters in NGC 7252
... Cluster profiles and sizes in NGC 7252 Observations of young cluster systems have shown that the clusters themselves are often grouped into larger structures, cluster complexes, with radii of tens to hundreds of parsecs (e.g. Zhang, Fall & Whitmore 2001; Larsen 2004). These complexes often appear t ...
... Cluster profiles and sizes in NGC 7252 Observations of young cluster systems have shown that the clusters themselves are often grouped into larger structures, cluster complexes, with radii of tens to hundreds of parsecs (e.g. Zhang, Fall & Whitmore 2001; Larsen 2004). These complexes often appear t ...
Auriga (constellation)
Auriga is one of the 48 constellations listed by the 2nd-century astronomer Ptolemy and remains one of the 88 modern constellations. Located north of the celestial equator, its name is the Latin word for ""charioteer"", associating it with various mythological charioteers, including Erichthonius and Myrtilus. Auriga is most prominent during winter evenings in the Northern Hemisphere, along with the five other constellations that have stars in the Winter Hexagon asterism. Because of its northern declination, Auriga is only visible in its entirety as far as 34° south; for observers farther south it lies partially or fully below the horizon. A large constellation, with an area of 657 square degrees, it is half the size of the largest constellation, Hydra.Its brightest star, Capella, is an unusual multiple star system among the brightest stars in the night sky. Beta Aurigae is an interesting variable star in the constellation; Epsilon Aurigae, a nearby eclipsing binary with an unusually long period, has been studied intensively. Because of its position near the winter Milky Way, Auriga has many bright open clusters in its borders, including M36, M37, and M38, popular targets for amateur astronomers. In addition, it has one prominent nebula, the Flaming Star Nebula, associated with the variable star AE Aurigae.In Chinese mythology, Auriga's stars were incorporated into several constellations, including the celestial emperors' chariots, made up of the modern constellation's brightest stars. Auriga is home to the radiant for the Aurigids, Zeta Aurigids, Delta Aurigids, and the hypothesized Iota Aurigids.