Orion the Hunter
... Hunter. Its brightest stars form one of the best known celestial shapes, which is visible even from cities. The plane of the Milky Way clips the northeast corner of the constellation and manifests itself as a featureless, hazy band through the neighboring constellations of Gemini and Monoceros. Or ...
... Hunter. Its brightest stars form one of the best known celestial shapes, which is visible even from cities. The plane of the Milky Way clips the northeast corner of the constellation and manifests itself as a featureless, hazy band through the neighboring constellations of Gemini and Monoceros. Or ...
Epsilon Aurigae: a rare stellar eclipse - Project VS
... from the inside. The previous eclipse took place back in 1982-1984. The recent was in 2009-2011, when a new generation of telescopes had been prepared on this stellar enigma in an effort to unlock its mystery. This was only the seventh documented eclipse in history (2010, 1983, 1956, 1930, 1902, 187 ...
... from the inside. The previous eclipse took place back in 1982-1984. The recent was in 2009-2011, when a new generation of telescopes had been prepared on this stellar enigma in an effort to unlock its mystery. This was only the seventh documented eclipse in history (2010, 1983, 1956, 1930, 1902, 187 ...
THE MONTHLY SKY GUIDE, SIXTH EDITION
... Most bright stars, and several not-so-bright ones, have strangesounding names. Other stars are known merely by letters and numbers. These designations arose in various ways, as follows. A number of star names date back to Greek and Roman times. For example, the name of the brightest star in the sky, ...
... Most bright stars, and several not-so-bright ones, have strangesounding names. Other stars are known merely by letters and numbers. These designations arose in various ways, as follows. A number of star names date back to Greek and Roman times. For example, the name of the brightest star in the sky, ...
Zapartas_deMink_Izzard_AA_2017
... Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova ra ...
... Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova ra ...
The science case for - Astrophysics
... How typical is our Solar System? What are the planetary environments around other stars? ...
... How typical is our Solar System? What are the planetary environments around other stars? ...
The roAp star α Circinus as seen by BRITE
... larger, mostly due to problems with the BAb star tracker and as a result of the spectral type, which produces a smaller count rate for the blue BRITEs compared to the red BRITEs. The rotation light curves are obviously different in the two colours. While one maximum at approximately phase φ = 0.8 app ...
... larger, mostly due to problems with the BAb star tracker and as a result of the spectral type, which produces a smaller count rate for the blue BRITEs compared to the red BRITEs. The rotation light curves are obviously different in the two colours. While one maximum at approximately phase φ = 0.8 app ...
White dwarfs from GAIA: The 7th dimension
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
... • The white dwarf luminosity function of Gaia is a sensitive probe of the averaged star formation rate • Due to their very short main-sequence lifetimes the shape of the SFR can be reconstructed from the luminosity function of massive white dwarfs • To achieve these goals, we need R~5000 spectroscop ...
Laboratory for AO at UCSC
... The observable wavefronts in multi-guide star wavefront sensors are the integrals along a 3-D volumetric atmosphere along different lines-of-sight. A tomographic algorithm14,15 can be used to directly compute the phase in metapupils at various heights through the atmosphere from these integrated wav ...
... The observable wavefronts in multi-guide star wavefront sensors are the integrals along a 3-D volumetric atmosphere along different lines-of-sight. A tomographic algorithm14,15 can be used to directly compute the phase in metapupils at various heights through the atmosphere from these integrated wav ...
Chemical analysis of 24 dusty (pre-) main
... (Canary Islands, Spain). The second observational run, concerning mostly southern-hemisphere objects, was performed by dr. Gwendolyn Meeus from January 26 till January 28, 1999 at the ESO site La Silla (Chile). These data were collected using the 1.5m telescope and the FEROS instrument. The waveleng ...
... (Canary Islands, Spain). The second observational run, concerning mostly southern-hemisphere objects, was performed by dr. Gwendolyn Meeus from January 26 till January 28, 1999 at the ESO site La Silla (Chile). These data were collected using the 1.5m telescope and the FEROS instrument. The waveleng ...
The Ages of Stars
... create a true cohort based on mass, composition, and age. At present, comparisons of the Sun to other stars often rely on the very stellar properties (such as activity, rotation, or lithium abundance) that one is trying to understand; the process is self-referential. • To fully understand the Galaxy ...
... create a true cohort based on mass, composition, and age. At present, comparisons of the Sun to other stars often rely on the very stellar properties (such as activity, rotation, or lithium abundance) that one is trying to understand; the process is self-referential. • To fully understand the Galaxy ...
PPT presentation
... observations of mass loss rates and/or location of the Mira variables tells you which stars are now dying. Mass loss rates are sensitive to a combination of R, L, and M such that low metallicity stars, smaller at a given L, M, reach higher L before dying. The generation of dust and oxygen- or carbo ...
... observations of mass loss rates and/or location of the Mira variables tells you which stars are now dying. Mass loss rates are sensitive to a combination of R, L, and M such that low metallicity stars, smaller at a given L, M, reach higher L before dying. The generation of dust and oxygen- or carbo ...
The spectroscopic Hertzsprung
... stars that have a luminosity larger than the luminosity of a single star of comparable mass and evolutionary state. Kippenhahn & Weigert (1990) showed that main sequence stars are expected to obey the relation L ∼ M α µβ , where µ is the average mean molecular weight and β > 1. An overluminosity is ...
... stars that have a luminosity larger than the luminosity of a single star of comparable mass and evolutionary state. Kippenhahn & Weigert (1990) showed that main sequence stars are expected to obey the relation L ∼ M α µβ , where µ is the average mean molecular weight and β > 1. An overluminosity is ...
![Module 4.1 - The Scale of the Universe [slide 1] We now turn to](http://s1.studyres.com/store/data/002846843_1-9e0ec9d1a2abbbab3c0d406694bfc4e2-300x300.png)
Module 4.1 - The Scale of the Universe [slide 1] We now turn to
... Since all of them were roughly the same distance, apparent magnitude would correlate with period and then they understood that comparing that with nearby Cepheids they can find out how far the Magellanic Couds are. Cepheids are important because they are bright and so we can see them far away, we c ...
... Since all of them were roughly the same distance, apparent magnitude would correlate with period and then they understood that comparing that with nearby Cepheids they can find out how far the Magellanic Couds are. Cepheids are important because they are bright and so we can see them far away, we c ...
a changing cosmos - Whittier Union High School District
... a volume approximately 10 light years in diameter and is still expanding at the very high velocity of about 1,800 km/sec. A supernova is an unimaginably powerful explosive event. It occurs when a very large star, over eight times the Sun's mass, has burned most of its nuclear fuel. When such a star' ...
... a volume approximately 10 light years in diameter and is still expanding at the very high velocity of about 1,800 km/sec. A supernova is an unimaginably powerful explosive event. It occurs when a very large star, over eight times the Sun's mass, has burned most of its nuclear fuel. When such a star' ...
10. Atmospheres of Planets and of Exoplanets - ETH E
... Layers of the Atmosphere of Venus The Atmosphere of Venus is much denser and hotter than that of the Earth . The Temperature at the surface is 467 0C, while there, the pressure is 93 bar! The Atmosphere of Venus contains opaque clouds of sulfuric acid (H2SO4); this Atmosphere makes observations from ...
... Layers of the Atmosphere of Venus The Atmosphere of Venus is much denser and hotter than that of the Earth . The Temperature at the surface is 467 0C, while there, the pressure is 93 bar! The Atmosphere of Venus contains opaque clouds of sulfuric acid (H2SO4); this Atmosphere makes observations from ...
The cosmological significance of high
... and probably nearby (d = 27 kpc) HVC whose location in the Galactic plane has hampered previous investigations of its stellar content. The H I mass of the cloud is 2.0 × 107 (d/27 kpc)2 M⊙ , making Complex H one of the most massive HVCs if its distance is more than ∼ 20 kpc. Virtually all similar H ...
... and probably nearby (d = 27 kpc) HVC whose location in the Galactic plane has hampered previous investigations of its stellar content. The H I mass of the cloud is 2.0 × 107 (d/27 kpc)2 M⊙ , making Complex H one of the most massive HVCs if its distance is more than ∼ 20 kpc. Virtually all similar H ...
Lectures 19-20 The Milky Way Galaxy
... the dust. This is helpful because there are large number of K and M giant stars (T ~ 4000 K) in the central part of the galaxy, and these are brightest in at 2-micron. Note that the nearest star to the Sun is ~1 pc away. The density of stars is much higher in the Galactic Center ! ...
... the dust. This is helpful because there are large number of K and M giant stars (T ~ 4000 K) in the central part of the galaxy, and these are brightest in at 2-micron. Note that the nearest star to the Sun is ~1 pc away. The density of stars is much higher in the Galactic Center ! ...
Historic mass loss from the RS Ophiuchi system
... Stars with an initial mass between ∼ 1 and ∼ 40 M¯ become hydrogen/heliumshell-burning Asymptotic Giant Branch (AGB) stars or core-helium-burning red supergiants (RSG). These phases are characterised by cool, molecular atmospheres giving rise to M spectral types (S or C for some chemically peculiar ...
... Stars with an initial mass between ∼ 1 and ∼ 40 M¯ become hydrogen/heliumshell-burning Asymptotic Giant Branch (AGB) stars or core-helium-burning red supergiants (RSG). These phases are characterised by cool, molecular atmospheres giving rise to M spectral types (S or C for some chemically peculiar ...
Camelopardalis-Better-Know-A-Constellation
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
flare swg usa
... Fitting SEDS: The long-λ fluxes from cool dust have ambiguous SED fits, while higher spatial resolution, near-IR fluxes from clustered sources are often very much fainter. FLARE can reach ~8 mag deeper than IRAC surveys at 3.5 μm, enabling the measurement of the NIR SEDs of young (<104 yr old) ...
... Fitting SEDS: The long-λ fluxes from cool dust have ambiguous SED fits, while higher spatial resolution, near-IR fluxes from clustered sources are often very much fainter. FLARE can reach ~8 mag deeper than IRAC surveys at 3.5 μm, enabling the measurement of the NIR SEDs of young (<104 yr old) ...