arXiv:1705.00964v1 [astro-ph.GA] 2 May 2017
... J1819+3845 might be related to the foreground, bright star Vega. We therefore examined whether ionized gas associated with foreground stars provides a good explanation for the IDV phenomenon. Although we continue to monitor PKS1322-110, it will be some time before that data set rivals the coverage o ...
... J1819+3845 might be related to the foreground, bright star Vega. We therefore examined whether ionized gas associated with foreground stars provides a good explanation for the IDV phenomenon. Although we continue to monitor PKS1322-110, it will be some time before that data set rivals the coverage o ...
WORD - Astrophysics
... relevant to the sort of abundances modelled in the big codes. However, lines of sight through these regions are currently completely inaccessible. In our galaxy, optical studies of highly reddened stars in or behind dense clouds is certainly important, to determine properties which are currently est ...
... relevant to the sort of abundances modelled in the big codes. However, lines of sight through these regions are currently completely inaccessible. In our galaxy, optical studies of highly reddened stars in or behind dense clouds is certainly important, to determine properties which are currently est ...
Astronomy Astrophysics Circumstellar emission in Be/X-ray binaries of the Magellanic
... Our main goals are exploring whether previously published relations, valid for isolated Be stars, are applicable to Be/X-ray binaries and computing the distance to these systems after correcting for the effects of the circumstellar contamination. Methods. Simultaneous U BVRI photometry and spectra in ...
... Our main goals are exploring whether previously published relations, valid for isolated Be stars, are applicable to Be/X-ray binaries and computing the distance to these systems after correcting for the effects of the circumstellar contamination. Methods. Simultaneous U BVRI photometry and spectra in ...
Colloquial Jakartan Indonesian
... The best scholarly minds of Europe had spent centuries developing ways of representing a curved world on a flat map and ways in which explorers could locate changing positions on their flat maps by using compass, sextant, chronometer, almanacs and various mathematical tables. When Europeans first ve ...
... The best scholarly minds of Europe had spent centuries developing ways of representing a curved world on a flat map and ways in which explorers could locate changing positions on their flat maps by using compass, sextant, chronometer, almanacs and various mathematical tables. When Europeans first ve ...
astro-ph/0303282 PDF
... planet detection. At 3.3 pc, it is one of the closest stars to Earth. Eps Eri is thought to have a relatively young age of ~730 Myr (Song et al. 2000), and has a mass similar to that of our sun. There is also tentative radial-velocity evidence for a companion in an a=3.4 AU orbit (Hatzes et al. 2000 ...
... planet detection. At 3.3 pc, it is one of the closest stars to Earth. Eps Eri is thought to have a relatively young age of ~730 Myr (Song et al. 2000), and has a mass similar to that of our sun. There is also tentative radial-velocity evidence for a companion in an a=3.4 AU orbit (Hatzes et al. 2000 ...
What Can You See With a Telescope
... No asteroids were found until 1845—almost forty years later—even though groups of amateur and professional astronomers designed special sky-mapping projects to search for them. ...
... No asteroids were found until 1845—almost forty years later—even though groups of amateur and professional astronomers designed special sky-mapping projects to search for them. ...
Galaxies
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
... The Universe is filled with these star systems which themselves cluster together into larger systems. ...
The accretion disk paradigm for young stars
... whereas the observed excess luminosity can be greater than L in extreme CTTSs. Even though the value of a typical CTTS luminosity excess was unknown in the early 1950s, it was already clear that it was orders of magnitude larger than what the accretion of interstellar cloud gas could provide. Faced ...
... whereas the observed excess luminosity can be greater than L in extreme CTTSs. Even though the value of a typical CTTS luminosity excess was unknown in the early 1950s, it was already clear that it was orders of magnitude larger than what the accretion of interstellar cloud gas could provide. Faced ...
Protostellar/PMS Mass Infall Luminosity Problem
... mass, as in the Herschel Orion Protostar Survey (HOPS, Manoj et al. 2013; Fisher et al. 2013; Stutz et al. 2013) ...
... mass, as in the Herschel Orion Protostar Survey (HOPS, Manoj et al. 2013; Fisher et al. 2013; Stutz et al. 2013) ...
The Classification of Stellar Spectra
... prominence of certain spectral lines. In Secchi’s scheme, for instance, stars with very strong hydrogen lines were called type I, stars with strong lines from metallic ions like iron and calcium were called type II, stars with wide bands of absorption that got darker toward the blue were called type ...
... prominence of certain spectral lines. In Secchi’s scheme, for instance, stars with very strong hydrogen lines were called type I, stars with strong lines from metallic ions like iron and calcium were called type II, stars with wide bands of absorption that got darker toward the blue were called type ...
Annual report 2004 - Département d`Astrophysique, Géophysique et
... combination at La Silla in 1996-1998, and on synthetic data. HD140873 and HD123515 are both noneclipsing double-lined binaries in eccentric orbits of 39 and 26 days. The broad-lined primary of HD140873 is an apparently monoperiodic SPB, while the sharp-lined primary of HD123515 is a multiperiodic SP ...
... combination at La Silla in 1996-1998, and on synthetic data. HD140873 and HD123515 are both noneclipsing double-lined binaries in eccentric orbits of 39 and 26 days. The broad-lined primary of HD140873 is an apparently monoperiodic SPB, while the sharp-lined primary of HD123515 is a multiperiodic SP ...
Stellar Spectroscopy
... surface of the star, but most of what is known about stars is determined from the many spectral lines seen in their spectrum. A close inspection of a star’s spectrum will reveal many absorption lines, and for some stars, emission lines as well. These spectral lines can be used to determine an incred ...
... surface of the star, but most of what is known about stars is determined from the many spectral lines seen in their spectrum. A close inspection of a star’s spectrum will reveal many absorption lines, and for some stars, emission lines as well. These spectral lines can be used to determine an incred ...
Compare/Order Decimals
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
24.1 Hubble`s Galaxy Classification
... 24.2 The Distribution of Galaxies in Space In order to find how galaxies are distributed in the universe, we have to be able to estimate their distances. We therefore need to understand which “standard candles” can be used for this purpose. Recall that RR Lyrae variables allowed us to get distances ...
... 24.2 The Distribution of Galaxies in Space In order to find how galaxies are distributed in the universe, we have to be able to estimate their distances. We therefore need to understand which “standard candles” can be used for this purpose. Recall that RR Lyrae variables allowed us to get distances ...
CORONAL EVOLUTION OF THE SUN IN TIME: HIGH
... transporting it to coronal heights, they may be important tracers for the coronal heating mechanism. For example, it has been suggested that the Ne enrichment seen in active stars may be related to increased levels of flaring ( Brinkman et al. 2001). This paper presents a study of six solar analogs ...
... transporting it to coronal heights, they may be important tracers for the coronal heating mechanism. For example, it has been suggested that the Ne enrichment seen in active stars may be related to increased levels of flaring ( Brinkman et al. 2001). This paper presents a study of six solar analogs ...
Polaris
... But you can find it easily, and, once you do, you’ll see it shining in the northern sky every night, from N. Hemisphere locations. ***In the Northern Hemisphere, the altitude of Polaris is equal to the observer’s latitude. In the Southern Hemisphere, an observer cannot see Polaris. Altitude is measu ...
... But you can find it easily, and, once you do, you’ll see it shining in the northern sky every night, from N. Hemisphere locations. ***In the Northern Hemisphere, the altitude of Polaris is equal to the observer’s latitude. In the Southern Hemisphere, an observer cannot see Polaris. Altitude is measu ...
Lithium abundances along the red giant branch: FLAMES
... agreed with the expected value for the difference in heliocentric correction, and the same shift was found for all spectra obtained at a given time. Therefore, we can exclude that these shifts are the result of orbital motion in a binary system. No other velocity shifts were found within the accuracy ...
... agreed with the expected value for the difference in heliocentric correction, and the same shift was found for all spectra obtained at a given time. Therefore, we can exclude that these shifts are the result of orbital motion in a binary system. No other velocity shifts were found within the accuracy ...
Chromospherically young, kinematically old stars
... The chromospheric activity of a late-type star is frequently interpreted as a sign of its youth. Young dwarfs show high rotation rates, and the interaction between rotation and outer envelope convection is expected to drive the chromospheric activity. Nevertheless, not only young single stars presen ...
... The chromospheric activity of a late-type star is frequently interpreted as a sign of its youth. Young dwarfs show high rotation rates, and the interaction between rotation and outer envelope convection is expected to drive the chromospheric activity. Nevertheless, not only young single stars presen ...
The old globular cluster system of the dIrr galaxy NGC 1427A in the
... In all these models, the GCSs of low-mass dwarf galaxies, the most numerous galaxy type in galaxy clusters (Sandage 2005, and references therein), are envisioned as the building blocks of the GCSs of the more massive galaxies. At present the role of the GCSs of dIrr galaxies in the frame of galaxy f ...
... In all these models, the GCSs of low-mass dwarf galaxies, the most numerous galaxy type in galaxy clusters (Sandage 2005, and references therein), are envisioned as the building blocks of the GCSs of the more massive galaxies. At present the role of the GCSs of dIrr galaxies in the frame of galaxy f ...
Corona Australis
Corona Australis /kɵˈroʊnə ɒˈstreɪlɨs/ or Corona Austrina /kɵˈroʊnə ɒˈstraɪnə/ is a constellation in the Southern Celestial Hemisphere. Its Latin name means ""southern crown"", and it is the southern counterpart of Corona Borealis, the northern crown. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The Ancient Greeks saw Corona Australis as a wreath rather than a crown and associated it with Sagittarius or Centaurus. Other cultures have likened the pattern to a turtle, ostrich nest, a tent, or even a hut belonging to a rock hyrax.Although fainter than its namesake, the oval- or horseshoe-shaped pattern of its brighter stars renders it distinctive. Alpha and Beta Coronae Australis are the two brightest stars with an apparent magnitude of around 4.1. Epsilon Coronae Australis is the brightest example of a W Ursae Majoris variable in the southern sky. Lying alongside the Milky Way, Corona Australis contains one of the closest star-forming regions to our Solar System—a dusty dark nebula known as the Corona Australis Molecular Cloud, lying about 430 light years away. Within it are stars at the earliest stages of their lifespan. The variable stars R and TY Coronae Australis light up parts of the nebula, which varies in brightness accordingly.