White dwarf cooling sequences and cosmochronology
... uniformity of the models with log(L/L ) ≤ −1.5. Furthermore, since the time necessary to reach this value is ≤ 8 × 107 years for any model, its influence in the total cooling time is negligible [19], except of course at large luminosities. Fluid cooling: This phase occurs at luminosities −1.5 ≥ log ...
... uniformity of the models with log(L/L ) ≤ −1.5. Furthermore, since the time necessary to reach this value is ≤ 8 × 107 years for any model, its influence in the total cooling time is negligible [19], except of course at large luminosities. Fluid cooling: This phase occurs at luminosities −1.5 ≥ log ...
The AcroCoRoT objectives (10 min) - IAG-Usp
... Do we correctly understand and model surface structures such as spots and stellar granulation ? What is the exact nature of the interplay between rotation, convection and activity ? ...
... Do we correctly understand and model surface structures such as spots and stellar granulation ? What is the exact nature of the interplay between rotation, convection and activity ? ...
m82 as a galaxy: morphology and stellar content of the disk and halo
... Figure 3, we display the modeled image of the spiral arms. The absence of a dominating bulge, and the relatively open arms (pitch angle=14◦ ) suggest that M82 is a late-type spiral (SBc), which is consistent with the gross properties discussed above. In normal galaxies, the spiral arms are easily tr ...
... Figure 3, we display the modeled image of the spiral arms. The absence of a dominating bulge, and the relatively open arms (pitch angle=14◦ ) suggest that M82 is a late-type spiral (SBc), which is consistent with the gross properties discussed above. In normal galaxies, the spiral arms are easily tr ...
Metallicity distribution for planet
... relation: occurrence of gas giant planets around FGK-type dwarfs is very sensitive to metallicity of host star. Santos et al. (2001) and Ghezzi et al. (2010) showed that there is planet-metallicity relation which means that gas giant planets host stars (FGK-type dwarfs) tend to be more metal-rich co ...
... relation: occurrence of gas giant planets around FGK-type dwarfs is very sensitive to metallicity of host star. Santos et al. (2001) and Ghezzi et al. (2010) showed that there is planet-metallicity relation which means that gas giant planets host stars (FGK-type dwarfs) tend to be more metal-rich co ...
Spectroscopic Studies of Evolved Stars and Planetary Nebulae
... formation. These objects undergo dramatic mass loss which ultimately enriches the interstellar medium. In this thesis, a number of studies, outlined below, have been undertaken to better understand the chemical and physical properties of these diverse objects. A molecular line survey of a sample of ...
... formation. These objects undergo dramatic mass loss which ultimately enriches the interstellar medium. In this thesis, a number of studies, outlined below, have been undertaken to better understand the chemical and physical properties of these diverse objects. A molecular line survey of a sample of ...
November News Letter - Boise Astronomical Society
... the Dog Star or Sirius. Procyon appears bright in our sky not because it is a truly bright star, but because it’s so close to our solar system. The star is a little less than 12 light years away. So if you know someone born in 2002, Procyon is their birthday star this year. Did you know that Procyon ...
... the Dog Star or Sirius. Procyon appears bright in our sky not because it is a truly bright star, but because it’s so close to our solar system. The star is a little less than 12 light years away. So if you know someone born in 2002, Procyon is their birthday star this year. Did you know that Procyon ...
The Polarization of Light
... separated in frequency by ∼ 1 GHz (note this is only a part in 105 of the optical frequency, so it still looks monochromatic). We will learn more about lasers later in the course, but at the moment, what you need to know is that over time (minutes to hours) the amount of light in the two modes can d ...
... separated in frequency by ∼ 1 GHz (note this is only a part in 105 of the optical frequency, so it still looks monochromatic). We will learn more about lasers later in the course, but at the moment, what you need to know is that over time (minutes to hours) the amount of light in the two modes can d ...
Document
... • Either most unobscured AGNs are affected by strong selection effects (“Lauer’s bias”) • Or obscured and unobscured AGNs follow different evolutionary paths ...
... • Either most unobscured AGNs are affected by strong selection effects (“Lauer’s bias”) • Or obscured and unobscured AGNs follow different evolutionary paths ...
Dispersion measurements with white-light interferometry
... is often categorized as incoherent light and is therefore presumed to be of little use in a modern optics lab where lasers abound. Indeed, if one is to define temporal coherence as the ability of an electric field to interfere with a delayed version of itself, then the light from a helium –neon lase ...
... is often categorized as incoherent light and is therefore presumed to be of little use in a modern optics lab where lasers abound. Indeed, if one is to define temporal coherence as the ability of an electric field to interfere with a delayed version of itself, then the light from a helium –neon lase ...
Waves & Oscillations Physics 42200 Spring 2014 Semester Lecture 39 – Review
... (b) Calculate the intensity of transmitted light if the incident light is unpolarized (c) Calculate the intensity of transmitted light if the incident light is left circular polarized (d) Is the system symmetric? That is, is the intensity of transmitted light the same if the paths of all light rays ...
... (b) Calculate the intensity of transmitted light if the incident light is unpolarized (c) Calculate the intensity of transmitted light if the incident light is left circular polarized (d) Is the system symmetric? That is, is the intensity of transmitted light the same if the paths of all light rays ...
Regenerating evanescent waves from a silver superlens
... ensures a concentricity of better than 300 µm. The coupling mechanism is shown in Fig. 2(b). Instead of placing a near-field object for the case of real superlens imaging, we now utilize the subwavelength surface roughness at the silver–air interface to scatter the incident beam to all possible kx d ...
... ensures a concentricity of better than 300 µm. The coupling mechanism is shown in Fig. 2(b). Instead of placing a near-field object for the case of real superlens imaging, we now utilize the subwavelength surface roughness at the silver–air interface to scatter the incident beam to all possible kx d ...
The GAPS Programme with HARPS-N@ TNG II: No giant planets
... and no obvious trend in the RVs over that time span is apparent. Furthermore, Latham (private communication) obtained five new RVs with the Tillinghast Reflector Echelle Spectrograph (TRES) at the FLWO observatory over a span of eight nights during December 2012 with typical errors of 0.1 km s−1 . T ...
... and no obvious trend in the RVs over that time span is apparent. Furthermore, Latham (private communication) obtained five new RVs with the Tillinghast Reflector Echelle Spectrograph (TRES) at the FLWO observatory over a span of eight nights during December 2012 with typical errors of 0.1 km s−1 . T ...
Red Supergiants, Luminous Blue Variables and Wolf
... agreement for dust-enshrouded objects, but not for optically bright ones. Dust enshrouded objects show mass loss rates which are greater by a factor 3-50 than those deduced from optically bright ones! In this context the questions of which stars do become dust-enshrouded, at which stage, for how lon ...
... agreement for dust-enshrouded objects, but not for optically bright ones. Dust enshrouded objects show mass loss rates which are greater by a factor 3-50 than those deduced from optically bright ones! In this context the questions of which stars do become dust-enshrouded, at which stage, for how lon ...
hr diagrams of star clusters
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
HR DIAGRAMS OF STAR CLUSTERS
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
THE PERIOD OF ROTATION OF THE SUN
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
Chapter 6 Experiment 4: Wave Interference
... and mark the locations of the interference fringes (the finely spaced bright spots) on a strip of fresh tape. Mark all visible spots; if fewer than five spots are visible on each side of the beam axis, choose a different double-slit pattern. Also measure the distance from the double-slit slide to th ...
... and mark the locations of the interference fringes (the finely spaced bright spots) on a strip of fresh tape. Mark all visible spots; if fewer than five spots are visible on each side of the beam axis, choose a different double-slit pattern. Also measure the distance from the double-slit slide to th ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.