Hot Horizontal Branch Stars in the Galactic Bulge. I
... http://www.cfht.hawaii.edu/∼ bernt/gsc/gscbrowser.html to identify 271 guide stars from Hubble Space Telescope. An astrometric solution was found which included a single frame scale in α, δ, a rotation angle, and quadratic terms in row and column position. The resulting solution had an r.m.s. scatte ...
... http://www.cfht.hawaii.edu/∼ bernt/gsc/gscbrowser.html to identify 271 guide stars from Hubble Space Telescope. An astrometric solution was found which included a single frame scale in α, δ, a rotation angle, and quadratic terms in row and column position. The resulting solution had an r.m.s. scatte ...
Open clusters and associations in the Gaia era
... In order to identify bona fide cluster/association members from observations, several criteria can be used. First of all, since they share the same age, metallicity and distance (for clusters only - for associations, individual parallax measurements are mandatory to take each star distance into acco ...
... In order to identify bona fide cluster/association members from observations, several criteria can be used. First of all, since they share the same age, metallicity and distance (for clusters only - for associations, individual parallax measurements are mandatory to take each star distance into acco ...
Colour-magnitude diagrams of the post
... numbers corresponding to: HB contained in the box of stars bluer than V − I < 1.6 and in the magnitude interval 18.2 < V < 19.8 and for the field the stars in a box defined along the subgiant branch (SGB) at the same magnitude level, and in the colour interval 2.8 < (V −I) < 3.3; in order to check i ...
... numbers corresponding to: HB contained in the box of stars bluer than V − I < 1.6 and in the magnitude interval 18.2 < V < 19.8 and for the field the stars in a box defined along the subgiant branch (SGB) at the same magnitude level, and in the colour interval 2.8 < (V −I) < 3.3; in order to check i ...
The first carbon-enhanced metal-poor star found in the Sculptor
... spheroidal galaxies around the Milky Way. Here we present detailed abundances from ESO VLT/UVES high-resolution spectroscopy for ET0097, the first CEMP star found in the Sculptor dwarf spheroidal, which is one of the best studied dwarf galaxies in the Local Group. This star has [Fe/H] = −2.03 ± 0.10 ...
... spheroidal galaxies around the Milky Way. Here we present detailed abundances from ESO VLT/UVES high-resolution spectroscopy for ET0097, the first CEMP star found in the Sculptor dwarf spheroidal, which is one of the best studied dwarf galaxies in the Local Group. This star has [Fe/H] = −2.03 ± 0.10 ...
Isotopic composition of Hg and Pt in 5 slowly rotating HgMn stars *
... neither extreme overabundances of rare earths, nor signicant overabundances of Si. Their spectral lines do not show conspicuous intensity variations. Neither have strong Send oprint requests to : G. Mathys ? Based on observations obtained at the European Southern Observatory, La Silla, Chile (ESO ...
... neither extreme overabundances of rare earths, nor signicant overabundances of Si. Their spectral lines do not show conspicuous intensity variations. Neither have strong Send oprint requests to : G. Mathys ? Based on observations obtained at the European Southern Observatory, La Silla, Chile (ESO ...
... In the RRL data base of GEOS (2012) one can find a list of 96 times of maxima and the corresponding O-C diagram built with the ephemerides 2419130.305+0.28779276 E is reproduced in Figure 4. Visual observations show a particularly large scatter at HJD ∼ 2443800 which may be due to their larger uncer ...
preprint, pdf version - LESIA
... (23 June 2011). These last two events, as in 22 June 2008, were double events in which Charon and Pluto occulted the same star. In the 4 June 2011 event in particular, both occultations could be recorded at each site. The population of TNOs in general, have been far more poorly studied. Up to the ti ...
... (23 June 2011). These last two events, as in 22 June 2008, were double events in which Charon and Pluto occulted the same star. In the 4 June 2011 event in particular, both occultations could be recorded at each site. The population of TNOs in general, have been far more poorly studied. Up to the ti ...
SherwoodWA_1973redux - Edinburgh Research Archive
... 1970; Gottesman and Davis, 1970) found that the HII regions and blue supergiants (in associations) lie within the ...
... 1970; Gottesman and Davis, 1970) found that the HII regions and blue supergiants (in associations) lie within the ...
The old globular cluster system of the dIrr galaxy NGC 1427A in the
... level, hence it is expected to be variable toward the central galaxy regions. This effect should be accounted for if the photometric study is devoted mainly to the objects in those inner most regions. However, the GCs which we study here are typically located at large galactocentric distances and th ...
... level, hence it is expected to be variable toward the central galaxy regions. This effect should be accounted for if the photometric study is devoted mainly to the objects in those inner most regions. However, the GCs which we study here are typically located at large galactocentric distances and th ...
Chemical abundances and winds of massive stars in M31: a B
... types), Mg, Si, S, Al, Ca, Fe, Ti, Cr, Ni; Venn et al. 2000, Smartt, Dufton & Lennon 1997). Further they can also provide new information on the distances of galaxies through the detailed study of the strengths of their radiatively driven winds using the wind momentum – luminosity relationship (WLR, ...
... types), Mg, Si, S, Al, Ca, Fe, Ti, Cr, Ni; Venn et al. 2000, Smartt, Dufton & Lennon 1997). Further they can also provide new information on the distances of galaxies through the detailed study of the strengths of their radiatively driven winds using the wind momentum – luminosity relationship (WLR, ...
Binarity in carbon-enhanced metal-poor stars
... (iii) CEMP-r/s: [C/Fe] > +1.0 and 0.0 < [Ba/Eu] < +0.5 and (iv) CEMP-no: [C/Fe] > +1.0 and [Ba/Fe] < 0. The large class of CEMP-s stars is thought to obtain their overabundant carbon and s-process elements from a companion star that has gone through the asymptotic giant branch (AGB) phase and deposi ...
... (iii) CEMP-r/s: [C/Fe] > +1.0 and 0.0 < [Ba/Eu] < +0.5 and (iv) CEMP-no: [C/Fe] > +1.0 and [Ba/Fe] < 0. The large class of CEMP-s stars is thought to obtain their overabundant carbon and s-process elements from a companion star that has gone through the asymptotic giant branch (AGB) phase and deposi ...
1 Pau Amaro Seoane - modest 15-s
... of turbulent molecular clouds. The stars are assumed to form in the densest regions in the collapsing cloud after an initial free-fall times of the molecular cloud. The dynamical evolution of these stellar distributions are continued by means of direct N-body simulations. The molecular clouds typica ...
... of turbulent molecular clouds. The stars are assumed to form in the densest regions in the collapsing cloud after an initial free-fall times of the molecular cloud. The dynamical evolution of these stellar distributions are continued by means of direct N-body simulations. The molecular clouds typica ...
Distance determination for RAVE stars using stellar models
... be done without a reliable estimate of the distances to the stars under consideration. Therefore obtaining accurate distances and velocities for a representative sample of stars in our Galaxy will be essential if we are to understand both the structure of our own Galaxy and galaxy formation in gener ...
... be done without a reliable estimate of the distances to the stars under consideration. Therefore obtaining accurate distances and velocities for a representative sample of stars in our Galaxy will be essential if we are to understand both the structure of our own Galaxy and galaxy formation in gener ...
Chemical abundances and winds of massive stars in M31: a Btype
... B- and A-type supergiants in Local Group galaxies with welldefined distances will, therefore, allow us to test the concept of the WLR and its applicability for distance determinations. Numerous surveys have identified OB and WR stars beyond the Magellanic Clouds, e.g. Massey et al. (1986) and Moffat ...
... B- and A-type supergiants in Local Group galaxies with welldefined distances will, therefore, allow us to test the concept of the WLR and its applicability for distance determinations. Numerous surveys have identified OB and WR stars beyond the Magellanic Clouds, e.g. Massey et al. (1986) and Moffat ...
Colloquial Jakartan Indonesian
... which one steers) and the Micronesian etak (a ‘moving’ reference point) which refer to concepts incompatible with Western navigation theory. For some of these we may be able to offer a Proto Oceanic (POc) origin. Undoubtedly, as navigation skills developed and were refined in the Pacific, new terms ...
... which one steers) and the Micronesian etak (a ‘moving’ reference point) which refer to concepts incompatible with Western navigation theory. For some of these we may be able to offer a Proto Oceanic (POc) origin. Undoubtedly, as navigation skills developed and were refined in the Pacific, new terms ...
Metal-poor Stars
... because no stars were known with metallicities lower than 1/1000 of the solar iron abundance. Even at [Fe/H] ∼ −3.0, only extremely few objects were known although more were predicted to exist by a simple model of chemical evolution in the Galactic halo. Bond (1981) reported on unsuccessful searches ...
... because no stars were known with metallicities lower than 1/1000 of the solar iron abundance. Even at [Fe/H] ∼ −3.0, only extremely few objects were known although more were predicted to exist by a simple model of chemical evolution in the Galactic halo. Bond (1981) reported on unsuccessful searches ...
here - NASA/IPAC Extragalactic Database
... has finally been demonstrated to be dependent on stellar wind strengths, although nitrogen abundance also plays an important role (Rivero Gonzáez et al. 2011). Of course, a significant problem occurs when one looks at O stars in other galaxies that are more metal-poor than the Milky Way where the v ...
... has finally been demonstrated to be dependent on stellar wind strengths, although nitrogen abundance also plays an important role (Rivero Gonzáez et al. 2011). Of course, a significant problem occurs when one looks at O stars in other galaxies that are more metal-poor than the Milky Way where the v ...
POSTERS SESSION I: Atmospheres of Massive Stars
... Massive stars have strong stellar winds that exhibit variability on timescales ranging from hours to years. Many classes of these stars are also seen, via photometric or line-profile variability, to pulsate radially or nonradially. It has been suspected for some time that these oscillations can indu ...
... Massive stars have strong stellar winds that exhibit variability on timescales ranging from hours to years. Many classes of these stars are also seen, via photometric or line-profile variability, to pulsate radially or nonradially. It has been suspected for some time that these oscillations can indu ...
Do We Know of Any Maunder Minimum Stars?
... (Perryman et al. 1997; Perryman & ESA 1997). To increase the confidence in the results here, only those WMBV stars with more than two Keck observations are used in this work. The bulk of the ∼ 1000 stars in WMBV are currently being monitored for radial velocity variations and are typically bright, w ...
... (Perryman et al. 1997; Perryman & ESA 1997). To increase the confidence in the results here, only those WMBV stars with more than two Keck observations are used in this work. The bulk of the ∼ 1000 stars in WMBV are currently being monitored for radial velocity variations and are typically bright, w ...
Stars & Galaxies - newmanlib.ibri.org
... that they differ in brightness. • As one looks at the stars more carefully, it becomes apparent that they are not all the same color. • Look at the constellation of Orion shown in the next panel. ...
... that they differ in brightness. • As one looks at the stars more carefully, it becomes apparent that they are not all the same color. • Look at the constellation of Orion shown in the next panel. ...
to - NexStar Resource Site
... 9) Jupiter The king of our Solar System of planets. It is believed that with a little more mass, Jupiter could have become a small star. What a different place our Earth would be with 2 Suns. Jupiter orbits 778,330,000 km (5.20 AU) from the Sun. Its mass is about 318 times that of the Earth and cont ...
... 9) Jupiter The king of our Solar System of planets. It is believed that with a little more mass, Jupiter could have become a small star. What a different place our Earth would be with 2 Suns. Jupiter orbits 778,330,000 km (5.20 AU) from the Sun. Its mass is about 318 times that of the Earth and cont ...
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.