A cold detached dust envelope around an oxygen-rich Mira
... case (Hashimoto 1994, 1995). (4) Or, some circumstellar mechanisms other than dust grains may produce the infrared excess. For example, strong line emission from circumstellar molecules such as H2 O may cause the reddening. In any case, there must be some physical conditions which are unknown in the ...
... case (Hashimoto 1994, 1995). (4) Or, some circumstellar mechanisms other than dust grains may produce the infrared excess. For example, strong line emission from circumstellar molecules such as H2 O may cause the reddening. In any case, there must be some physical conditions which are unknown in the ...
All About Elements
... in the universe. Only Hydrogen is more abundant! These two elements were copiously formed during the creation of the universe. In the early stages of the universe, helium and hydrogen nuclei were actually formed. No atoms were formed until about 300,000 years after the Big Bang took place, when the ...
... in the universe. Only Hydrogen is more abundant! These two elements were copiously formed during the creation of the universe. In the early stages of the universe, helium and hydrogen nuclei were actually formed. No atoms were formed until about 300,000 years after the Big Bang took place, when the ...
Early-type stars in the core of the young open cluster Westerlund 2
... is dominated by strong and broad H Balmer lines. Weak absorption lines of He λλ 4388, 4471, Mg λ 4481 and Si λ 4552 are also seen. The He λ 4471/Mg λ 4481 intensity ratio indicates a spectral type B8-A0. The appearance of some weak metallic lines favours an A0 classification, whilst ...
... is dominated by strong and broad H Balmer lines. Weak absorption lines of He λλ 4388, 4471, Mg λ 4481 and Si λ 4552 are also seen. The He λ 4471/Mg λ 4481 intensity ratio indicates a spectral type B8-A0. The appearance of some weak metallic lines favours an A0 classification, whilst ...
The spectroscopic Hertzsprung
... these stars remain almost constant during this evolution, it will thus be difficult to distinguish whether an observed star is on the redward or on the blueward part of the track. While it remains hidden in the HR diagram, the sHR diagram reveals nicely that the mass loss drives these stars towards ...
... these stars remain almost constant during this evolution, it will thus be difficult to distinguish whether an observed star is on the redward or on the blueward part of the track. While it remains hidden in the HR diagram, the sHR diagram reveals nicely that the mass loss drives these stars towards ...
Stars & Galaxies - newmanlib.ibri.org
... Lifespan of a G Star • When it uses up the H in its core, it expands to form a red giant, burning H in an outer shell & He in the core. • When the He is gone, the star collapses to form a white dwarf. • The dwarf gradually cools till it ceases to shine, becoming a black dwarf. ...
... Lifespan of a G Star • When it uses up the H in its core, it expands to form a red giant, burning H in an outer shell & He in the core. • When the He is gone, the star collapses to form a white dwarf. • The dwarf gradually cools till it ceases to shine, becoming a black dwarf. ...
ALMA - ESO
... Herschel is best suited for surveys, ALMA a followup instrument ALMA has a small Field Of View (FOV), but high angular resolution and sensitivity Higher angular resolution to image the sources measured by Herschel Follow up to sources discovered with PACS or SPIRE in longer wavelength dust emission ...
... Herschel is best suited for surveys, ALMA a followup instrument ALMA has a small Field Of View (FOV), but high angular resolution and sensitivity Higher angular resolution to image the sources measured by Herschel Follow up to sources discovered with PACS or SPIRE in longer wavelength dust emission ...
GALAXIES 626
... Kinematics and structure of the thick disk rotational lag ~ 30 km/s near the sun and increases by about 30 km s-1 kpc-1 with height above the plane velocity dispersion in (U,V,W) = (46, 50, 35) km/s radial scale length = 3.5 to 4.5 kpc : uncertain scale height from star counts = 800 to 1200 pc (thi ...
... Kinematics and structure of the thick disk rotational lag ~ 30 km/s near the sun and increases by about 30 km s-1 kpc-1 with height above the plane velocity dispersion in (U,V,W) = (46, 50, 35) km/s radial scale length = 3.5 to 4.5 kpc : uncertain scale height from star counts = 800 to 1200 pc (thi ...
A Comet-Hunter`s Legacy -
... their hottest, brightest stars -- stars that are burning their fuel so quickly that they are nearly at the end of their Main Sequence lives -- are much brighter than the hottest, brightest stars in other globular clusters, and can't be much more than half a ...
... their hottest, brightest stars -- stars that are burning their fuel so quickly that they are nearly at the end of their Main Sequence lives -- are much brighter than the hottest, brightest stars in other globular clusters, and can't be much more than half a ...
2. The X-ray-Radio correlation for bulgeless galaxies
... Fig. 21: The VLA-COSMOS Large Project Survey as obtained with the NRAO's VLA. A section of the survey as been zoomed to allow for a better visualization of the sources...............................................................45 Fig. 22: Flux distribution for the radio-detected sources as captur ...
... Fig. 21: The VLA-COSMOS Large Project Survey as obtained with the NRAO's VLA. A section of the survey as been zoomed to allow for a better visualization of the sources...............................................................45 Fig. 22: Flux distribution for the radio-detected sources as captur ...
IAC_L2_thindisk
... the disk, e.g. via Jeans equation. Is there more matter in the disk that we can account for from census of visible objects ? The tracer sample must be in equilibrium so the stars need to be older than a few Gyr. The last few estimates have used K dwarfs and K giants - probably OK but they do include ...
... the disk, e.g. via Jeans equation. Is there more matter in the disk that we can account for from census of visible objects ? The tracer sample must be in equilibrium so the stars need to be older than a few Gyr. The last few estimates have used K dwarfs and K giants - probably OK but they do include ...
Stellar Remnants White Dwarfs Type Ia Supernovae Neutron Stars
... © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
... © 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley ...
AR2012 - Vatican Observatory
... binoculars equipped with solar filters. In addition, the Vatican Observatory’s Coronado Solar Telescope, attached to the large Visual refractor telescope on the Papal Palace roof, was connected to a new CCD imaging camera and computer network, recently provided to the Observatory from the Governator ...
... binoculars equipped with solar filters. In addition, the Vatican Observatory’s Coronado Solar Telescope, attached to the large Visual refractor telescope on the Papal Palace roof, was connected to a new CCD imaging camera and computer network, recently provided to the Observatory from the Governator ...
Evolution of stars
... e. combines four hydrogen nuclei to form one helium nucleus, which produces energy. What causes the outward pressure that balances the inward pull of gravity in a star? a. The outward flow of energy. b. The opacity of the gas. c. The temperature of the gas d. The density of the gas e. c and d The fr ...
... e. combines four hydrogen nuclei to form one helium nucleus, which produces energy. What causes the outward pressure that balances the inward pull of gravity in a star? a. The outward flow of energy. b. The opacity of the gas. c. The temperature of the gas d. The density of the gas e. c and d The fr ...
A Digital Spectral Classification Atlas
... spectra are presented in a rectified intensity versus wavelength format, in which the spectral continuum has been normalized to unity. The 3.6Å resolution spectra, for the most part, are presented in a flux versus wavelength format; this format provides additional information on ...
... spectra are presented in a rectified intensity versus wavelength format, in which the spectral continuum has been normalized to unity. The 3.6Å resolution spectra, for the most part, are presented in a flux versus wavelength format; this format provides additional information on ...
Mn, Cu, and Zn abundances in barium stars and their correlations
... intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ≥ 10 M stars (see Raiteri et al. 1993; Matteucci et al. 1993; Mishenina et al. 2002, and references therein). Even though their positions in the periodic table are contiguous, their be ...
... intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ≥ 10 M stars (see Raiteri et al. 1993; Matteucci et al. 1993; Mishenina et al. 2002, and references therein). Even though their positions in the periodic table are contiguous, their be ...
LIGO I - Indico
... GWs aren’t just a new band, they’re a new spectrum, with very different and complementary properties to EM waves. • Vibrations of space-time, not in space-time • Emitted by coherent motion of huge masses moving at near light-speed; not vibrations of electrons in atoms • Can’t be absorbed, scattered, ...
... GWs aren’t just a new band, they’re a new spectrum, with very different and complementary properties to EM waves. • Vibrations of space-time, not in space-time • Emitted by coherent motion of huge masses moving at near light-speed; not vibrations of electrons in atoms • Can’t be absorbed, scattered, ...
The Evolution of Isotope Ratios in the Milky Way Galaxy
... metals are produced. This assumption may not be valid but does not affect the average chemical evolution of galaxies. Super AGB stars — The fate of stars with initial masses between about 8 − 10M⊙ is uncertain. The upper limit of AGB stars, Mu,1 , is defined as the minimum mass for carbon ignition, ...
... metals are produced. This assumption may not be valid but does not affect the average chemical evolution of galaxies. Super AGB stars — The fate of stars with initial masses between about 8 − 10M⊙ is uncertain. The upper limit of AGB stars, Mu,1 , is defined as the minimum mass for carbon ignition, ...
GRB EXPERIMENT
... • Note that the definition does not specify the magnetic field strength • To explain SGRs and AXPs, however, B must be greater than the quantum critical value 4.4 x 1013 G, where the energy between electron Landau levels equals their rest mass • Some AXPs and SGRs require B~1015 Gauss, so these magn ...
... • Note that the definition does not specify the magnetic field strength • To explain SGRs and AXPs, however, B must be greater than the quantum critical value 4.4 x 1013 G, where the energy between electron Landau levels equals their rest mass • Some AXPs and SGRs require B~1015 Gauss, so these magn ...
Galaxies - hwchemistry
... neutron stars. – Astronomers don’t see the X rays these objects would emit. – There is 10 to 100 times more dark matter than visible matter. – That many black holes would produce X rays that would be easy to detect. ...
... neutron stars. – Astronomers don’t see the X rays these objects would emit. – There is 10 to 100 times more dark matter than visible matter. – That many black holes would produce X rays that would be easy to detect. ...
Evidence for the Tidal Destruction of Hot Jupiters by Subgiant Stars
... Figure 2. Galactic U V W kinematics of subgiant stars that host exoplanets discovered with the radial-velocity technique. In each panel, we plot the U V W space motions of the subgiant sample as blue points and the density of points in a control sample selected from the Hipparcos catalog as the back ...
... Figure 2. Galactic U V W kinematics of subgiant stars that host exoplanets discovered with the radial-velocity technique. In each panel, we plot the U V W space motions of the subgiant sample as blue points and the density of points in a control sample selected from the Hipparcos catalog as the back ...
Review: How does a star`s mass determine its life story?
... • size R ~ thousands of kilometers • mass M ~ mass of stars • density absurdly high: – white dwarf matter is roughly a million times more dense than water atomic density ...
... • size R ~ thousands of kilometers • mass M ~ mass of stars • density absurdly high: – white dwarf matter is roughly a million times more dense than water atomic density ...