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Resultados del Concurso 2008A para Observaciones en
... Resumen: Planets and brown dwarfs in close orbits around main sequence stars will inevitably interact with their stellar hosts once they ascend the red giant branch. The details and outcomes of these interactions are currently unclear. Recent discoveries of brown dwarfs and planets orbiting post-red ...
... Resumen: Planets and brown dwarfs in close orbits around main sequence stars will inevitably interact with their stellar hosts once they ascend the red giant branch. The details and outcomes of these interactions are currently unclear. Recent discoveries of brown dwarfs and planets orbiting post-red ...
Type II supernovae (Inma Dominguez)
... The chemical composition of this shell, that will be active till the collapse, tends to get frozen because the evolution of the star is more and more rapid at the advanced phases. ...
... The chemical composition of this shell, that will be active till the collapse, tends to get frozen because the evolution of the star is more and more rapid at the advanced phases. ...
MS-SCI-PS-Unit 4 -- Chapter 15- Stars, Galaxies
... atmosphere. To detect these wavelengths, astronomers have placed telescopes in space. Some space telescopes are designed to detect visible light or infrared radiation, since Earth's atmosphere also interferes with the transmission of these forms of radiation. The Hubble Space Telescope is a reflecti ...
... atmosphere. To detect these wavelengths, astronomers have placed telescopes in space. Some space telescopes are designed to detect visible light or infrared radiation, since Earth's atmosphere also interferes with the transmission of these forms of radiation. The Hubble Space Telescope is a reflecti ...
Age dating stellar populations in the near infrared
... 0.4Vc . Weighting these three measurements we measure a time of RSG appearance of 5.7 ± 0.8 Myr. As discussed in Section 3.2, the effects of these initial populations of RSGs on the near-IR cluster colours are expected to appear as a significant hysteresis jump allowing for a clear differentiation b ...
... 0.4Vc . Weighting these three measurements we measure a time of RSG appearance of 5.7 ± 0.8 Myr. As discussed in Section 3.2, the effects of these initial populations of RSGs on the near-IR cluster colours are expected to appear as a significant hysteresis jump allowing for a clear differentiation b ...
Ridgway - Betelgeuse Workshop 2016
... The enigmatic nature of the circumstellar envelope and bow shock surrounding Betelgeuse as revealed by Herschel The influence of a variable mass loss rate on the dust and gas dynamics in the bowshock of α-Orionis 3D Smoothed Particle Hydrodynamics Models of Betelgeuse’s Bow Shock Numerical models fo ...
... The enigmatic nature of the circumstellar envelope and bow shock surrounding Betelgeuse as revealed by Herschel The influence of a variable mass loss rate on the dust and gas dynamics in the bowshock of α-Orionis 3D Smoothed Particle Hydrodynamics Models of Betelgeuse’s Bow Shock Numerical models fo ...
Read the report
... hemisphere. Deep in its interior, energy is generated by thermo nuclear fusion reactions, converting hydrogen into helium. It takes millions of years for this energy to slowly flow from the hot central regions to the star’s cooler surface, where the radiation can finally escape into space. For both ...
... hemisphere. Deep in its interior, energy is generated by thermo nuclear fusion reactions, converting hydrogen into helium. It takes millions of years for this energy to slowly flow from the hot central regions to the star’s cooler surface, where the radiation can finally escape into space. For both ...
THE ORION NEBULA AND ITS ASSOCIATED POPULATION C. R. O
... was inconsistent with a spherically symmetric nebula and was used independently and essentially simultaneously by Balick et al. (1974) and Zuckerman (1973) to come up with today’s model. In a simple manner, the assumption of a thin emitting layer of radially decreasing density lying beyond the ioniz ...
... was inconsistent with a spherically symmetric nebula and was used independently and essentially simultaneously by Balick et al. (1974) and Zuckerman (1973) to come up with today’s model. In a simple manner, the assumption of a thin emitting layer of radially decreasing density lying beyond the ioniz ...
3. Measuring Distances and Magnitudes
... always appear less bright below the Earth's atmosphere than above it. 1 clear unit airmass transmits 82% in the visual, i.e. it dims by 0.215mag. Air Mass is the path length that light from a celestial object takes through Earth’s atmosphere relative to the length at the zenith. The airmass is 1 at ...
... always appear less bright below the Earth's atmosphere than above it. 1 clear unit airmass transmits 82% in the visual, i.e. it dims by 0.215mag. Air Mass is the path length that light from a celestial object takes through Earth’s atmosphere relative to the length at the zenith. The airmass is 1 at ...
Cosmology with objects from the Hamburg Quasar Surveys
... which accurate abundances can be obtained only with knowledge of the spectral energy distribution (SED) of the ionizing background. Consequently, one has to admit that the metallicity of the largest part of the baryons is at present not known. The direct measurement of the SED is possible only in ab ...
... which accurate abundances can be obtained only with knowledge of the spectral energy distribution (SED) of the ionizing background. Consequently, one has to admit that the metallicity of the largest part of the baryons is at present not known. The direct measurement of the SED is possible only in ab ...
Stellar Population Modeling of Galaxies in Nearby Groups
... astrophysical parameters also impact the observed distribution: the distance to the galaxy, internal and external extinction and photometric errors. The observed data and synthetic data are stored in Hess diagram. This grid forms as a two-dimensional histogram indicating the number of stars in some ...
... astrophysical parameters also impact the observed distribution: the distance to the galaxy, internal and external extinction and photometric errors. The observed data and synthetic data are stored in Hess diagram. This grid forms as a two-dimensional histogram indicating the number of stars in some ...
Light n-Capture Element Abundances in Metal
... D. Burris, E. Jones, and J. Lusk 1989). The conditions needed are also generated in the shell-burning phase of Asymptotic Giant Branch (AGB) low to intermediate mass stars (Busso et al. 1999). These stars have lifetimes measured in billions of years. This is significant because n-capture elements c ...
... D. Burris, E. Jones, and J. Lusk 1989). The conditions needed are also generated in the shell-burning phase of Asymptotic Giant Branch (AGB) low to intermediate mass stars (Busso et al. 1999). These stars have lifetimes measured in billions of years. This is significant because n-capture elements c ...
Formation of Massive Stars
... • Massive stars are expected to modify their environment soon after a stellar core has formed since their Kelvin-Helmholtz time scale (< 104 yrs for an O star) is short ( tKH = E/L ~ GM2/LR) (Shu et al. 1987 AARA 25 23) ...
... • Massive stars are expected to modify their environment soon after a stellar core has formed since their Kelvin-Helmholtz time scale (< 104 yrs for an O star) is short ( tKH = E/L ~ GM2/LR) (Shu et al. 1987 AARA 25 23) ...
Gamma-ray burst has highest redshift yet seen
... because a GRB’s afterglow fades rapidly after a few hours, the spectra were too noisy to reveal absorption features that could address two cosmologically important issues: the abundance of “metals” (astronomers’ jargon for anything heavier than helium) in this very early star and its galaxy, and the ...
... because a GRB’s afterglow fades rapidly after a few hours, the spectra were too noisy to reveal absorption features that could address two cosmologically important issues: the abundance of “metals” (astronomers’ jargon for anything heavier than helium) in this very early star and its galaxy, and the ...
Using AO to Measure the Star Formation Histories of Massive Galaxies
... Magnitudes at which 10% photometry is possible in regions of surface brightness SV=22, SK=19 for galaxies at the indicated distances. ...
... Magnitudes at which 10% photometry is possible in regions of surface brightness SV=22, SK=19 for galaxies at the indicated distances. ...
Stars Stellar Lifetimes Life cycles of low
... What happens when the Hydrogen is gone? As the hydrogen “burns”, the helium “ash” builds up in the core. This interferes with hydrogen burning. The star’s core contracts to become hotter and denser to continue the “burning”. The outer layers of the star expand and become cooler as the core contract ...
... What happens when the Hydrogen is gone? As the hydrogen “burns”, the helium “ash” builds up in the core. This interferes with hydrogen burning. The star’s core contracts to become hotter and denser to continue the “burning”. The outer layers of the star expand and become cooler as the core contract ...
Astronomy Astrophysics
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
The Hamburg/ESO R-process Enhanced Star survey (HERES)
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
... In conclusion, larger samples of r-process-enhanced metalpoor stars are needed in order to make progress in our understanding of the phenomenon of r-process enhancement, investigate how common the “actinide boost” phenomenon is and what its physical reasons might be, identification of reliable chron ...
The HARPS-N Rocky Planet Search - Pure
... Received 24 June 2015 / Accepted 30 July 2015 ABSTRACT ...
... Received 24 June 2015 / Accepted 30 July 2015 ABSTRACT ...
Red Supergiants, Luminous Blue Variables and Wolf
... no detection by chance is only 0.018 for a Salpeter IMF. The authors invoke two reasons for explaining this lack of massive Type IIP SNe progenitors: 1) the underestimate of the progenitor masses due to dust extinction; 2) the stars in the mass range between 18 and 25 M do not produce type IIP SNe. ...
... no detection by chance is only 0.018 for a Salpeter IMF. The authors invoke two reasons for explaining this lack of massive Type IIP SNe progenitors: 1) the underestimate of the progenitor masses due to dust extinction; 2) the stars in the mass range between 18 and 25 M do not produce type IIP SNe. ...
Chapter 21 - apel slice
... dreamed of. He was the first to see sunspots, Saturn's rings, and the four large moons of Jupiter. Galileo could see fine details, such as mountains on the moon, which cannot be seen clearly by the unaided eye. Since Galileo's time, astronomers have built ever larger and more powerful telescopes. Th ...
... dreamed of. He was the first to see sunspots, Saturn's rings, and the four large moons of Jupiter. Galileo could see fine details, such as mountains on the moon, which cannot be seen clearly by the unaided eye. Since Galileo's time, astronomers have built ever larger and more powerful telescopes. Th ...
Astrophysical Journal - Harvard-Smithsonian Center for Astrophysics
... timescales of stars from their brightness or velocity variations, is a powerful means of probing stellar interiors. Asteroseismic measurements derived from photometry require a long observational baseline at high cadence (to detect typically mHz frequencies) and photometric precision at the level of ...
... timescales of stars from their brightness or velocity variations, is a powerful means of probing stellar interiors. Asteroseismic measurements derived from photometry require a long observational baseline at high cadence (to detect typically mHz frequencies) and photometric precision at the level of ...
Planetary Masses and Orbital Parameters from
... oplanet (GQ Lupi) only occurred in 2005 with VLT and, as of July 2006, three other exoplanets have also been imaged (2M1207, AB Pic and SCR 1845). However, most of the exoplanetary bodies have never been seen at all. If an exoplanet cannot be seen, how can we know it is there? The basic idea is that ...
... oplanet (GQ Lupi) only occurred in 2005 with VLT and, as of July 2006, three other exoplanets have also been imaged (2M1207, AB Pic and SCR 1845). However, most of the exoplanetary bodies have never been seen at all. If an exoplanet cannot be seen, how can we know it is there? The basic idea is that ...
Evolution of low- and intermediate mass stars
... first glance, the Eu evolution in dSph galaxies resembles that of their respective α-elements (see Figure 11), as expected for an r-process originating in massive stars. In the Milky Way, Ba and Y are dominated by the r-process for [Fe/H] ! −2.0 (e.g., Johnson & Bolte 2002, Simmerer et al. 2004), wh ...
... first glance, the Eu evolution in dSph galaxies resembles that of their respective α-elements (see Figure 11), as expected for an r-process originating in massive stars. In the Milky Way, Ba and Y are dominated by the r-process for [Fe/H] ! −2.0 (e.g., Johnson & Bolte 2002, Simmerer et al. 2004), wh ...
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.