THE VELOCITY DISTRIBUTION OF THE NEAREST
... find that this procedure yields a predicted flow velocity V flow , which is relatively insensitive to the detailed set of the selected velocity components, provided that sky coverage is good and that several stars with components at anomalous velocities are removed from the sample (next section). In p ...
... find that this procedure yields a predicted flow velocity V flow , which is relatively insensitive to the detailed set of the selected velocity components, provided that sky coverage is good and that several stars with components at anomalous velocities are removed from the sample (next section). In p ...
RApid Temporal Survey-RATS I: Overview and first results
... master image was then searched for all the sources above a 5σ detection limit. Next, we determined for each of the remaining frames an accurate image shift in relation to the master image. This was done in order to be able to use small enough apertures for light curve extraction, thus maximizing the ...
... master image was then searched for all the sources above a 5σ detection limit. Next, we determined for each of the remaining frames an accurate image shift in relation to the master image. This was done in order to be able to use small enough apertures for light curve extraction, thus maximizing the ...
WAS THE SUN BORN IN A MASSIVE CLUSTER?
... A number of authors have argued that the Sun must have been born in a cluster of no more than several thousand stars, on the basis that, in a larger cluster, close encounters between the Sun and other stars would have truncated the outer solar system or excited the outer planets into eccentric orbit ...
... A number of authors have argued that the Sun must have been born in a cluster of no more than several thousand stars, on the basis that, in a larger cluster, close encounters between the Sun and other stars would have truncated the outer solar system or excited the outer planets into eccentric orbit ...
HOPS 383: An Outbursting Class 0 Protostar in Orion
... in the submillimeter by comparing APEX/SABOCA to SCUBA data, and a scattered-light nebula appeared in NEWFIRM Ks imaging. The post-outburst spectral energy distribution indicates a Class 0 source with a dense envelope and a luminosity between 6 and 14 L⊙ . Post-outburst time-series midand far-infrar ...
... in the submillimeter by comparing APEX/SABOCA to SCUBA data, and a scattered-light nebula appeared in NEWFIRM Ks imaging. The post-outburst spectral energy distribution indicates a Class 0 source with a dense envelope and a luminosity between 6 and 14 L⊙ . Post-outburst time-series midand far-infrar ...
Debris disks and the search for life in the universe Gianni Cataldi
... (∼28%), the rest being heavier elements referred to as metals in astronomy. The ISM is far from homogeneous. Temperature and density vary considerably for its different components. Table 1.1 gives an overview of temperatures and hydrogen nuclei densities encountered in the ISM. About half of the ISM ...
... (∼28%), the rest being heavier elements referred to as metals in astronomy. The ISM is far from homogeneous. Temperature and density vary considerably for its different components. Table 1.1 gives an overview of temperatures and hydrogen nuclei densities encountered in the ISM. About half of the ISM ...
Betelgeuse - TeacherWeb
... bar?q=does+betelgeuse+have+any+planets+orbiting+it&page=1&qsrc=0&dm=all&ab=0&title=Betelgeuse%3A+The+ incredible+shrinking+star%3F+-+space+-+10+June+2009+-&u=http%3A%2F%2Fwww.newscientist.com%2Farticle%2 Fdn17282-betelgeuse-the-incredible-shrinking-star.html&sg=Tg5Jp0P9HJP34hrORVjtKiFjVQQx%2FdKgrwDF ...
... bar?q=does+betelgeuse+have+any+planets+orbiting+it&page=1&qsrc=0&dm=all&ab=0&title=Betelgeuse%3A+The+ incredible+shrinking+star%3F+-+space+-+10+June+2009+-&u=http%3A%2F%2Fwww.newscientist.com%2Farticle%2 Fdn17282-betelgeuse-the-incredible-shrinking-star.html&sg=Tg5Jp0P9HJP34hrORVjtKiFjVQQx%2FdKgrwDF ...
Stardust--Snapshots of Stars
... different astrophysical origins. One grain has massive enrichments in 17O, 25Mg, and 26Mg, which are considered isotopic signatures of condensation from nova ejecta. Two other spinel grains have large 25Mg and 26Mg isotopic anomalies that are difficult to explain by standard nucleosynthesis in a low ...
... different astrophysical origins. One grain has massive enrichments in 17O, 25Mg, and 26Mg, which are considered isotopic signatures of condensation from nova ejecta. Two other spinel grains have large 25Mg and 26Mg isotopic anomalies that are difficult to explain by standard nucleosynthesis in a low ...
1. INTRODUCTION
... sets with more than 5 days of monitoring or with a signiÐcant number of Ñares (more than ten Ñares identiÐed by eye) were selected. Active coronal sources were our prime choice, as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do ...
... sets with more than 5 days of monitoring or with a signiÐcant number of Ñares (more than ten Ñares identiÐed by eye) were selected. Active coronal sources were our prime choice, as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do ...
McDonald I....Tisserand, P. et al ExELS an
... three-dimensional dust model to compute extinction and reddening (Marshall et al. 2005). The populations included in the model are such that stars are limited to between 0.08 and 4 M (B–M type stars). No transiting planets have yet been found around stars outside this range and the proposed target ...
... three-dimensional dust model to compute extinction and reddening (Marshall et al. 2005). The populations included in the model are such that stars are limited to between 0.08 and 4 M (B–M type stars). No transiting planets have yet been found around stars outside this range and the proposed target ...
Stars: HR Diagaram Stellar Evolution Astronomy 1 — Elementary Astronomy LA Mission College
... Image ESA/NASA ...
... Image ESA/NASA ...
Behaviour of elements from lithium to europium in stars with and
... with Teff lower than 5000 K, we used only the trigonometric parallax method. The microturbulence velocity Vt was derived providing that the iron abundance log A(Fe) obtained from Fe I lines was not correlated with the equivalent width, EW. The adopted metallicity value [Fe/H] was the iron abundance ...
... with Teff lower than 5000 K, we used only the trigonometric parallax method. The microturbulence velocity Vt was derived providing that the iron abundance log A(Fe) obtained from Fe I lines was not correlated with the equivalent width, EW. The adopted metallicity value [Fe/H] was the iron abundance ...
LCM Analysis for PLATO 2.0
... Separation of the brightness maxima in EW-type lightcurves produced by a (near) contact binary is affected mostly by the limb darkening and stellar activity. Our simulations show that if in the primary minimum the more massive star is beeing eclipsed by a less massive component, then the secondary m ...
... Separation of the brightness maxima in EW-type lightcurves produced by a (near) contact binary is affected mostly by the limb darkening and stellar activity. Our simulations show that if in the primary minimum the more massive star is beeing eclipsed by a less massive component, then the secondary m ...
ULX accretion states
... Director’s cut for this talk Two or 3 ULXs are in a weird “supersoft state”, T <~ 0.1 keV Like Galactic SS sources (= nuclear burning WDs) But can a WD reach L ~ 1E39 erg/s Photosphere of massive outflows around a BH? ...
... Director’s cut for this talk Two or 3 ULXs are in a weird “supersoft state”, T <~ 0.1 keV Like Galactic SS sources (= nuclear burning WDs) But can a WD reach L ~ 1E39 erg/s Photosphere of massive outflows around a BH? ...
PPT presentation
... found that the PN and HII region abundances of oxygen and neon agreed within the same galaxy but that the PN nitrogen was enhanced by 0.9 dex in the SMC and LMC. Interpreted as due to CN cycle processing of almost all of the original carbon into nitrogen at the time of the first dredge-up. This proc ...
... found that the PN and HII region abundances of oxygen and neon agreed within the same galaxy but that the PN nitrogen was enhanced by 0.9 dex in the SMC and LMC. Interpreted as due to CN cycle processing of almost all of the original carbon into nitrogen at the time of the first dredge-up. This proc ...
ULXs: General Properties and Variability - X
... Ultra- Luminous X-ray Sources in Nearby Galaxies Numerous ( in ~1/4 of all galaxies) population of possible intermediate mass (20-5,000M) black holes. Unique properties not shared by AGN or galactic black holes True nature not well understood -several types of objects ? ...
... Ultra- Luminous X-ray Sources in Nearby Galaxies Numerous ( in ~1/4 of all galaxies) population of possible intermediate mass (20-5,000M) black holes. Unique properties not shared by AGN or galactic black holes True nature not well understood -several types of objects ? ...
Properties of Wolf-Rayet Stars - Paul Crowther, University of Sheffield
... emission equivalent width which is an order of magnitude smaller than that observed in other WN6 stars; the ‘ha’ nomenclature indicates that hydrogen is seen both in absorption and emission. From a standard spectroscopic viewpoint, such stars possess mid to late WN spectral classifications. However, ...
... emission equivalent width which is an order of magnitude smaller than that observed in other WN6 stars; the ‘ha’ nomenclature indicates that hydrogen is seen both in absorption and emission. From a standard spectroscopic viewpoint, such stars possess mid to late WN spectral classifications. However, ...
IK Pegasi
IK Pegasi (or HR 8210) is a binary star system in the constellation Pegasus. It is just luminous enough to be seen with the unaided eye, at a distance of about 150 light years from the Solar System.The primary (IK Pegasi A) is an A-type main-sequence star that displays minor pulsations in luminosity. It is categorized as a Delta Scuti variable star and it has a periodic cycle of luminosity variation that repeats itself about 22.9 times per day. Its companion (IK Pegasi B) is a massive white dwarf—a star that has evolved past the main sequence and is no longer generating energy through nuclear fusion. They orbit each other every 21.7 days with an average separation of about 31 million kilometres, or 19 million miles, or 0.21 astronomical units (AU). This is smaller than the orbit of Mercury around the Sun.IK Pegasi B is the nearest known supernova progenitor candidate. When the primary begins to evolve into a red giant, it is expected to grow to a radius where the white dwarf can accrete matter from the expanded gaseous envelope. When the white dwarf approaches the Chandrasekhar limit of 1.44 solar masses (M☉), it may explode as a Type Ia supernova.