![PDF only - at www.arxiv.org.](http://s1.studyres.com/store/data/017588686_1-36f559fc88697a239b3191e4c5eeefaa-300x300.png)
PDF only - at www.arxiv.org.
... should be noted in this respect that the planets HD 47536 b (Fe/H = -0,68, SMA = 1,61 AU) and HD 11755 b (Fe/H = -0,74, SMA = 1,08 AU), at very low metallicities, and unknown in 2005, are located below the ZAPO curve. The only planets in this group which are not compatible with the scenario of the Z ...
... should be noted in this respect that the planets HD 47536 b (Fe/H = -0,68, SMA = 1,61 AU) and HD 11755 b (Fe/H = -0,74, SMA = 1,08 AU), at very low metallicities, and unknown in 2005, are located below the ZAPO curve. The only planets in this group which are not compatible with the scenario of the Z ...
Terzan 5`s Pulsars Fastest
... because the enormous stellar densities of their cores promote exchange interactions that can form binaries capable of creating MSPs. There are ~110 pulsars known in the Galactic globular cluster system. Remarkably, half of these are contained in only two clusters: Terzan 5 and 47 Tuc. ...
... because the enormous stellar densities of their cores promote exchange interactions that can form binaries capable of creating MSPs. There are ~110 pulsars known in the Galactic globular cluster system. Remarkably, half of these are contained in only two clusters: Terzan 5 and 47 Tuc. ...
Chapter 4 [PDF only] - Princeton University Press
... the horizontal branch, and then evolves more slowly to the right along this branch, as seen in Fig. 4.1. Horizontal branch evolution last only about 1% of the main-sequence lifetime. Once the helium in the core has been exhausted, the core (now composed mainly of oxygen and carbon) contracts again, ...
... the horizontal branch, and then evolves more slowly to the right along this branch, as seen in Fig. 4.1. Horizontal branch evolution last only about 1% of the main-sequence lifetime. Once the helium in the core has been exhausted, the core (now composed mainly of oxygen and carbon) contracts again, ...
The star-forming environment of an ultraluminous X-ray
... a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass ≈20 M and age ≈10 Myr. A few other stars are resolved inside th ...
... a small group of OB stars, but is not associated with any massive young clusters nor with any extraordinary massive stars. The brightest point source in the Chandra error circle is consistent with a single blue supergiant (BSG) of mass ≈20 M and age ≈10 Myr. A few other stars are resolved inside th ...
Slide 1
... New class of massive WDs: “Hot DQ” Very little H (or He) in atmosphere. Dufour et al. (2007) ...
... New class of massive WDs: “Hot DQ” Very little H (or He) in atmosphere. Dufour et al. (2007) ...
Some notes on the Inka constellations
... its location the names and significance of celestial objects. It is important to emphasize that within the astronomy of the Inkas there are two types of constellations: (a) Stellar constellations or bright stars, made up of individual bright stars which constitute a ‘constellation’ and grouped togeth ...
... its location the names and significance of celestial objects. It is important to emphasize that within the astronomy of the Inkas there are two types of constellations: (a) Stellar constellations or bright stars, made up of individual bright stars which constitute a ‘constellation’ and grouped togeth ...
The Use of Astronomical Filters
... doubly ionized oxygen wavelengths. This is the filter of choice for the Veil and does amazing things with other emission nebulae whose predominant emissions are in the doubly ionized oxygen range.Grins and Giggles: Having difficulty splitting Antares? Try the OIII on it. It turns the primary star in ...
... doubly ionized oxygen wavelengths. This is the filter of choice for the Veil and does amazing things with other emission nebulae whose predominant emissions are in the doubly ionized oxygen range.Grins and Giggles: Having difficulty splitting Antares? Try the OIII on it. It turns the primary star in ...
Searching for the Secrets of Massive Star Birth
... molecular lines. Although ALMA will improve our view of protoclusters, even higher resolution will be needed to resolve binary and multiple systems. Proto-binaries with separations similar to 1Ori C in Orion (0.03”) at distances of 1 to 10 kpc require resolution of 10 to 1 milli-arseconds. High-re ...
... molecular lines. Although ALMA will improve our view of protoclusters, even higher resolution will be needed to resolve binary and multiple systems. Proto-binaries with separations similar to 1Ori C in Orion (0.03”) at distances of 1 to 10 kpc require resolution of 10 to 1 milli-arseconds. High-re ...
www.astro.utu.fi
... Whence and wither the halo stars? Inner halo : well mixed, stars on elliptical orbits Outer halo: stars on roundish orbits? State of play Finally, there is plenty of data; the models are really naïve ...
... Whence and wither the halo stars? Inner halo : well mixed, stars on elliptical orbits Outer halo: stars on roundish orbits? State of play Finally, there is plenty of data; the models are really naïve ...
Planetary compositions from disrupting exoplanets
... – many progenitor low-mass short period rocky planets should exist. ...
... – many progenitor low-mass short period rocky planets should exist. ...
v1 - ESO
... the Horizontal Branch (to detect the presence of stars > 10 Gyr old) and also to obtain main sequence turnoffs down to intermediate ages (∼ 6 − 8 Gyr). Two galaxies are selected for observing run A. The goal is to make accurate Colour-Magnitude Diagrams (CMDs), with errors in magnitude < 0.05 mag at ...
... the Horizontal Branch (to detect the presence of stars > 10 Gyr old) and also to obtain main sequence turnoffs down to intermediate ages (∼ 6 − 8 Gyr). Two galaxies are selected for observing run A. The goal is to make accurate Colour-Magnitude Diagrams (CMDs), with errors in magnitude < 0.05 mag at ...
ppt - lenac
... known, a mayor goal of the subject is to put constrains in the matter density Omega_m sigma_8 and in the shape of the primordial power spectrum of density perturbations. In this project a new scheme to select galaxy clusters is used, starting from small groups with two (cluster number richness, m=2) ...
... known, a mayor goal of the subject is to put constrains in the matter density Omega_m sigma_8 and in the shape of the primordial power spectrum of density perturbations. In this project a new scheme to select galaxy clusters is used, starting from small groups with two (cluster number richness, m=2) ...
Spectral modeling of nebular-phase supernovae Anders Jerkstrand Department of Astronomy
... Massive stars live fast and die young. They shine furiously for a few million years, during which time they synthesize most of the heavy elements in the universe in their cores. They end by blowing themselves up in a powerful explosion known as a supernova (SN). During this process, the core collaps ...
... Massive stars live fast and die young. They shine furiously for a few million years, during which time they synthesize most of the heavy elements in the universe in their cores. They end by blowing themselves up in a powerful explosion known as a supernova (SN). During this process, the core collaps ...
The hot-Jupiter Kepler-17b: discovery, obliquity from stroboscopic
... weighted distribution, with the error bars assigned from the nearest ±34% of values. In this way, we find M⋆ = ...
... weighted distribution, with the error bars assigned from the nearest ±34% of values. In this way, we find M⋆ = ...
WFIRSTSurveyScience
... Studies of low mass populations (encompassing stars, brown dwarfs, and even free-floating planetary mass objects) are hindered in star forming regions due to observational and astrophysical effects. These include: the large angular sizes of the nearby molecular clouds harboring newborn and young ste ...
... Studies of low mass populations (encompassing stars, brown dwarfs, and even free-floating planetary mass objects) are hindered in star forming regions due to observational and astrophysical effects. These include: the large angular sizes of the nearby molecular clouds harboring newborn and young ste ...
laboratory analysis of presolar silicate stardust from a
... which leads to 18 O/16 O ratios orders of magnitude lower than the nearly solar value observed for grain GR95_13_29. Therefore, we can exclude an AGB star origin for GR95_13_29. We explored the SNII models by Rauscher et al. (2002)5 to investigate a possible core-collapse supernova origin. No single ...
... which leads to 18 O/16 O ratios orders of magnitude lower than the nearly solar value observed for grain GR95_13_29. Therefore, we can exclude an AGB star origin for GR95_13_29. We explored the SNII models by Rauscher et al. (2002)5 to investigate a possible core-collapse supernova origin. No single ...
Winds from clusters with non-uniform stellar distribution
... massive stars first identified in NGC 1705 by Melnick et al. (1985) and in NGC 1569 by Arp & Sandage (1985). Recently, they have been observed in a wide range of starforming galaxies, such as merging systems (NGC 4038/4039), dwarf galaxies, classical starbursts, as well as in our galaxy amongst many ...
... massive stars first identified in NGC 1705 by Melnick et al. (1985) and in NGC 1569 by Arp & Sandage (1985). Recently, they have been observed in a wide range of starforming galaxies, such as merging systems (NGC 4038/4039), dwarf galaxies, classical starbursts, as well as in our galaxy amongst many ...
A seismic and gravitationally-bound double star observed by Kepler
... same parallax and proper motion (van Leeuwen 2007) but their relative motion observed between 1850 and 2007 does not allow one to derive a meaningful orbit. These binary systems are clearly resolved such that the time series of each component can be separately observed. When the two components are t ...
... same parallax and proper motion (van Leeuwen 2007) but their relative motion observed between 1850 and 2007 does not allow one to derive a meaningful orbit. These binary systems are clearly resolved such that the time series of each component can be separately observed. When the two components are t ...
“End-of-the-Line” W UMa Eclipsing Binary V523
... the W Ursae Majoris (W UMa) class where the dominant energy transport mechanism within the common envelope is convection—similar to the situation in the outer layers of the Sun. In these binaries, significant energy is transferred from the higher mass star to the lower mass star, resulting in a near ...
... the W Ursae Majoris (W UMa) class where the dominant energy transport mechanism within the common envelope is convection—similar to the situation in the outer layers of the Sun. In these binaries, significant energy is transferred from the higher mass star to the lower mass star, resulting in a near ...
Two distinct sequences of blue straggler stars in the globular cluster
... Creek ACT 2611, Australia Stars in globular clusters are generally believed to have all formed at the same time, early in the Galaxy's history1. 'Blue stragglers' are stars sufficiently massive2 that they should have evolved into white dwarfs long ago. Two possible mechanisms have been proposed for ...
... Creek ACT 2611, Australia Stars in globular clusters are generally believed to have all formed at the same time, early in the Galaxy's history1. 'Blue stragglers' are stars sufficiently massive2 that they should have evolved into white dwarfs long ago. Two possible mechanisms have been proposed for ...
extrasolar planets
... is still very faint: factor of ~1 million • Imaging of planets around Sun-like stars is currently not possible. Several ground-based and space-based 4/13/2009 projects in near future Habbal Astro110-01 Ch 6 Lecture 30 goal. are tackling this ...
... is still very faint: factor of ~1 million • Imaging of planets around Sun-like stars is currently not possible. Several ground-based and space-based 4/13/2009 projects in near future Habbal Astro110-01 Ch 6 Lecture 30 goal. are tackling this ...
Gamma - Ray Observations of Olaf Reimer
... indicative for rapid expansion into a ambient low-density medium (superbubble?) ...
... indicative for rapid expansion into a ambient low-density medium (superbubble?) ...
Pan-Planets: Searching for hot Jupiters around cool dwarfs⋆
... The procedure to select the 100 best images is the following: after removing all frames with a masking higher than 50%, we select the 120 images with the best seeing. We determine the weight of each image on the reference frame by determining the PSF FWHM and S/N and reject frames that possess a ver ...
... The procedure to select the 100 best images is the following: after removing all frames with a masking higher than 50%, we select the 120 images with the best seeing. We determine the weight of each image on the reference frame by determining the PSF FWHM and S/N and reject frames that possess a ver ...
Planetary nebula
![](https://commons.wikimedia.org/wiki/Special:FilePath/NGC6543.jpg?width=300)
A planetary nebula, often abbreviated as PN or plural PNe, is a kind of emission nebula consisting of an expanding glowing shell of ionized gas ejected from old red giant stars late in their lives. The word ""nebula"" is Latin for mist or cloud and the term ""planetary nebula"" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years.A mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energises the shell of nebulous gas around the central star, appearing as a bright coloured planetary nebula at several discrete visible wavelengths.Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances.In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. About one-fifth are roughly spherical, but the majority are not spherically symmetric. The mechanisms which produce such a wide variety of shapes and features are not yet well understood, but binary central stars, stellar winds and magnetic fields may play a role.