starry night companion
... azimuth of your viewing direction (compasses point to “magnetic north”, which is not exactly the same as “true north”, but the two directions are practically identical unless you are observing from a far northern latitude). Once you have your bearing, it is just a matter of looking up to the proper ...
... azimuth of your viewing direction (compasses point to “magnetic north”, which is not exactly the same as “true north”, but the two directions are practically identical unless you are observing from a far northern latitude). Once you have your bearing, it is just a matter of looking up to the proper ...
arXiv:astro-ph/9701131v1 18 Jan 1997
... stratified radiative cores. Second, as recognized by Salpeter (1982), full convection precludes the buildup of composition gradients which are ultimately responsible (in part) for a star’s ascent up the red giant branch. The lowest mass stars burn all their hydrogen into helium over an η = 13 time ...
... stratified radiative cores. Second, as recognized by Salpeter (1982), full convection precludes the buildup of composition gradients which are ultimately responsible (in part) for a star’s ascent up the red giant branch. The lowest mass stars burn all their hydrogen into helium over an η = 13 time ...
1 Discovery of peculiar periodic spectral
... to find additional information in the SDSS web site (http://data.sdss3.org/advancedSearch). In particular, the finding charts and u, g, i, r, z magnitudes are given. Figure 3 shows the Fourier modulus of the frequency spectrum (after subtraction of its smoothed spectrum) of a star that had a statist ...
... to find additional information in the SDSS web site (http://data.sdss3.org/advancedSearch). In particular, the finding charts and u, g, i, r, z magnitudes are given. Figure 3 shows the Fourier modulus of the frequency spectrum (after subtraction of its smoothed spectrum) of a star that had a statist ...
WILLIAM HERSCHEL AND THE `GARNET` STARS: μ CEPHEI AND
... this famous red star is not well documented. Prior to and after Herschel, the identification of this star was the subject of confusion in various catalogues and atlases. The case is complex and involves other stars in southern Cepheus, including double stars, found by Herschel in the course of his s ...
... this famous red star is not well documented. Prior to and after Herschel, the identification of this star was the subject of confusion in various catalogues and atlases. The case is complex and involves other stars in southern Cepheus, including double stars, found by Herschel in the course of his s ...
Joint formation of QSOs and spheroids: QSOs as clocks of star
... shine in the core of early-type protogalaxies during their main episode of star formation. Exploiting this fact, we derive the rate of formation of this kind of stellar system at high redshift by using the QSO luminosity function. The elemental proportions in elliptical galaxies, the descendants of ...
... shine in the core of early-type protogalaxies during their main episode of star formation. Exploiting this fact, we derive the rate of formation of this kind of stellar system at high redshift by using the QSO luminosity function. The elemental proportions in elliptical galaxies, the descendants of ...
Chemical composition of B-type supergiants in the OB8, OB10
... Previous studies have shown that quantitative spectroscopy of B-type supergiants in Local Group galaxies can be carried out successfully using 4 m telescopes (see Monteverde et al. 2000, Smartt et al. 2001b). The added advantage of using blue supergiants over H II regions is that their rich metal li ...
... Previous studies have shown that quantitative spectroscopy of B-type supergiants in Local Group galaxies can be carried out successfully using 4 m telescopes (see Monteverde et al. 2000, Smartt et al. 2001b). The added advantage of using blue supergiants over H II regions is that their rich metal li ...
Book Describing Techniques to Detect Transiting ExoPlanets
... of planets must exist! This is the message from the tally of ~ 400 extra-solar planetary systems (as of mid-2009). Among them are 60 exoplanets that transit in front of their star (46 that are brighter than 14th magnitude), and the number is growing with a doubling time of 1.1 years. It is important ...
... of planets must exist! This is the message from the tally of ~ 400 extra-solar planetary systems (as of mid-2009). Among them are 60 exoplanets that transit in front of their star (46 that are brighter than 14th magnitude), and the number is growing with a doubling time of 1.1 years. It is important ...
Debris Disks: Seeing Dust, Thinking of Planetesimals and Planets
... An efficient, and historically the first successful, way of detecting circumstellar dust is the infrared (IR) photometry. If dust is present around a star, it comes to a thermal equilibrium with the stellar radiation. With equilibrium temperatures of dust orbiting a solar-type star at several tens o ...
... An efficient, and historically the first successful, way of detecting circumstellar dust is the infrared (IR) photometry. If dust is present around a star, it comes to a thermal equilibrium with the stellar radiation. With equilibrium temperatures of dust orbiting a solar-type star at several tens o ...
Spin-driven tidal pumping: Tidally driven changes in planetary spin
... in multiplanet systems, where angular momentum is periodically exchanged among the planets through secular interactions (e.g. RodrÌguez et al. 2011). The periodic changes in the eccentricities can be described by a sum of eigenmodes that affect all the planets (e.g. Brouwer and Clemence 1961, Murray ...
... in multiplanet systems, where angular momentum is periodically exchanged among the planets through secular interactions (e.g. RodrÌguez et al. 2011). The periodic changes in the eccentricities can be described by a sum of eigenmodes that affect all the planets (e.g. Brouwer and Clemence 1961, Murray ...
The formation of disc galaxies in high-resolution moving
... resolution changes and require ‘retuning’ of the free parameters of the model to obtain the same or a similar result when the resolution is changed – if at all possible. The differences can be as extreme as those reported in Okamoto et al. (2005), where a galaxy’s morphology simulated at different r ...
... resolution changes and require ‘retuning’ of the free parameters of the model to obtain the same or a similar result when the resolution is changed – if at all possible. The differences can be as extreme as those reported in Okamoto et al. (2005), where a galaxy’s morphology simulated at different r ...
Processing of Star Catalog and Star Image
... (sub-blocks) by planes that are parallel to the equatorial plane. Each spherical zone has the same span of declination [2]. And guide stars in GSC can be directly retrieved by using a declination value. The problem with this method lies in the extremely uneven distribution of each sub-block. The num ...
... (sub-blocks) by planes that are parallel to the equatorial plane. Each spherical zone has the same span of declination [2]. And guide stars in GSC can be directly retrieved by using a declination value. The problem with this method lies in the extremely uneven distribution of each sub-block. The num ...
book_text4
... around the World. Such observations are highly complementary to those made by Hubble since they can exploit the collecting power of much larger telescopes and can be used very effectively to feed such light-hungry instruments as spectrographs. This higher resolution is achieved over a small patch of ...
... around the World. Such observations are highly complementary to those made by Hubble since they can exploit the collecting power of much larger telescopes and can be used very effectively to feed such light-hungry instruments as spectrographs. This higher resolution is achieved over a small patch of ...
Turbulence-driven Polar Winds from T Tauri Stars Energized by
... • It is highly likely that somewhere in the outer solar atmosphere the fluctuations become turbulent and cascade from large to small scales: ...
... • It is highly likely that somewhere in the outer solar atmosphere the fluctuations become turbulent and cascade from large to small scales: ...
Galactic Stellar and Substellar Initial Mass Function Invited Review Gilles Chabrier
... early star formation conditions. The disk IMF for single objects has a characteristic mass around mc ∼ 0.08 M, and a variance in logarithmic mass j ∼ 0.7 , whereas the IMF for multiple systems has mc ∼ 0.2 M, and j ∼ 0.6. The extension of the single MF into the brown dwarf regime is in good agreemen ...
... early star formation conditions. The disk IMF for single objects has a characteristic mass around mc ∼ 0.08 M, and a variance in logarithmic mass j ∼ 0.7 , whereas the IMF for multiple systems has mc ∼ 0.2 M, and j ∼ 0.6. The extension of the single MF into the brown dwarf regime is in good agreemen ...
Luminosity, Flux and Magnitudes Outline
... shorter wavelengths as the temperature increases (Wien’s law). ...
... shorter wavelengths as the temperature increases (Wien’s law). ...
The low-mass dispersed population around the Lupus clouds
... strong CaII absorption. The CaII lines in absorption disappear at mid-M types, but other surface gravity indicators discussed in the text clearly show that the bottom four stars are giants as well. ...
... strong CaII absorption. The CaII lines in absorption disappear at mid-M types, but other surface gravity indicators discussed in the text clearly show that the bottom four stars are giants as well. ...
