
Bez nadpisu
... to the luminosity of the system than afterward, when it is exhausted. The heights of the maxima in the pre-outburst state are different because we view the region where the stream and the outer parts of the disk interact from different angles. On the other hand, the depths of the minima are differen ...
... to the luminosity of the system than afterward, when it is exhausted. The heights of the maxima in the pre-outburst state are different because we view the region where the stream and the outer parts of the disk interact from different angles. On the other hand, the depths of the minima are differen ...
MASSIVE CLOSE BINARIES
... by a WR-type stellar wind mass loss. The effect on massive star evolution of present day WR-type mass loss rates (Equation 2) has been studied by Vanbeveren et al. (1998 a, b, c). ...
... by a WR-type stellar wind mass loss. The effect on massive star evolution of present day WR-type mass loss rates (Equation 2) has been studied by Vanbeveren et al. (1998 a, b, c). ...
neutron star
... galaxies are richer in heavy elements than the Sun, with the highest abundances ever seen in the early Universe. Heavy elements that enrich mature galaxies in the local Universe were made in past generations of stars. So these young galaxies have experienced a prodigious rate of star formation and c ...
... galaxies are richer in heavy elements than the Sun, with the highest abundances ever seen in the early Universe. Heavy elements that enrich mature galaxies in the local Universe were made in past generations of stars. So these young galaxies have experienced a prodigious rate of star formation and c ...
Supernovae and Gamma-Ray Bursts (draft)
... photons, e.g., from the radioactive decay of 56 Ni. If the He layer is shielded from this radioactive source, it is possible in principle to hide significant amounts of He. However, the most recent estimates (Hachinger et al. 2012) suggest that at most 0.2 M⊙ can be hidden. ...
... photons, e.g., from the radioactive decay of 56 Ni. If the He layer is shielded from this radioactive source, it is possible in principle to hide significant amounts of He. However, the most recent estimates (Hachinger et al. 2012) suggest that at most 0.2 M⊙ can be hidden. ...
Impact of atmospheric refraction: How deeply can we probe exo
... Misra et al. 2014) modeling the spectrum of the Earth’s atmosphere viewed as a transiting exoplanet. However, most models predicting, or fitting, the spectral dependence of planetary transits have not fully included a fundamental phenomenon of the atmosphere on radiation: refraction. As light rays t ...
... Misra et al. 2014) modeling the spectrum of the Earth’s atmosphere viewed as a transiting exoplanet. However, most models predicting, or fitting, the spectral dependence of planetary transits have not fully included a fundamental phenomenon of the atmosphere on radiation: refraction. As light rays t ...
Starburst Galaxies Encyclopedia of Astronomy & Astrophysics eaa.iop.org T Heckman
... Perhaps the most commonly used technique to estimate t is to calculate the gas-depletion time: the mass of interstellar gas in the starburst divided by the present rate of star formation. This is then a rough estimate of how much longer the starburst can be sustained before running out of gas. Gas- ...
... Perhaps the most commonly used technique to estimate t is to calculate the gas-depletion time: the mass of interstellar gas in the starburst divided by the present rate of star formation. This is then a rough estimate of how much longer the starburst can be sustained before running out of gas. Gas- ...
NAMES IN ESTONIAN FOLK ASTRONOMY – FROM `BIRD`S WAY
... porary astronomy there is indeed a snake in the Milky Way, in addition to the birds – in the constellation Serpens Cauda – Tail of the Snake. The Snake is borne by the nearby Ophiuchus constellation. As the North pole shifted, the Milky Way began to lean. This is a possible source for the stories an ...
... porary astronomy there is indeed a snake in the Milky Way, in addition to the birds – in the constellation Serpens Cauda – Tail of the Snake. The Snake is borne by the nearby Ophiuchus constellation. As the North pole shifted, the Milky Way began to lean. This is a possible source for the stories an ...
The Extragalactic Group of MPE and USM
... • Advantage of photo z: no color selection bias, fainter luminosities, larger sample (~10000 galaxies in FDF and GOODS S sub-sample) • FORS Deep Field (IAB=26.8): 98% of all galaxies with dz/(1+z)<0.03; GOODS S (KAB=25.4): dz/(1+z)<0.055 • Deep I-selection misses only a small fraction of deep K sele ...
... • Advantage of photo z: no color selection bias, fainter luminosities, larger sample (~10000 galaxies in FDF and GOODS S sub-sample) • FORS Deep Field (IAB=26.8): 98% of all galaxies with dz/(1+z)<0.03; GOODS S (KAB=25.4): dz/(1+z)<0.055 • Deep I-selection misses only a small fraction of deep K sele ...
Educator`s Guide
... They go as far back in time as the beginning of recorded history. For instance, the ancient Egyptians saw him as Osirus, the god of the Afterlife. Pyramids built 2500 BC possessed burial chambers with viewing shafts that aligned with Orion’s belt. 4000 years ago ancient Jews saw him as the biblical ...
... They go as far back in time as the beginning of recorded history. For instance, the ancient Egyptians saw him as Osirus, the god of the Afterlife. Pyramids built 2500 BC possessed burial chambers with viewing shafts that aligned with Orion’s belt. 4000 years ago ancient Jews saw him as the biblical ...
Rotation Periods and Relative Ages of Solar-Type Stars
... Pcalc are a function of chromospheric activity level as well as B - V spectral type. The formula for the calculation of rotation periods was derived from Noyes’ algorithm for determining Rossby number from mean stellar activity. A more detailed description is given by Noyes et al. (1984). These calc ...
... Pcalc are a function of chromospheric activity level as well as B - V spectral type. The formula for the calculation of rotation periods was derived from Noyes’ algorithm for determining Rossby number from mean stellar activity. A more detailed description is given by Noyes et al. (1984). These calc ...
Legends Night Sky Orion
... Legends of the Night Sky: Orion Educator’s Guide The constellation Draco, the dragon: - Winds between the Big and Little Dippers. - Generally takes up all of the remaining bright stars between those two constellations. - Draco’s head hangs down near Cepheus. - Draco is probably the toughest circump ...
... Legends of the Night Sky: Orion Educator’s Guide The constellation Draco, the dragon: - Winds between the Big and Little Dippers. - Generally takes up all of the remaining bright stars between those two constellations. - Draco’s head hangs down near Cepheus. - Draco is probably the toughest circump ...
P7 Further Physics
... Astronomers often use the “parsec” to describe galactic distances. A parsec is roughly 3¼ light years. Angles involved in parallax measurements are often very small and are measured in seconds of an arc (arcseconds). A second of an arc is 1/60th of a minute of an arc, which is 1/60th of a degree. In ...
... Astronomers often use the “parsec” to describe galactic distances. A parsec is roughly 3¼ light years. Angles involved in parallax measurements are often very small and are measured in seconds of an arc (arcseconds). A second of an arc is 1/60th of a minute of an arc, which is 1/60th of a degree. In ...
Radiative Precession of an Isolated Neutron Star
... swings. Davis & Goldstein (1970) showed that α tends towards zero on the braking time-scale if the star is a rigid sphere or a fluid body in hydrostatic equilibrium — an unrealistic scenario which leaves all except the youngest pulsars as aligned rotators, contrary to observation. Goldreich (1970) o ...
... swings. Davis & Goldstein (1970) showed that α tends towards zero on the braking time-scale if the star is a rigid sphere or a fluid body in hydrostatic equilibrium — an unrealistic scenario which leaves all except the youngest pulsars as aligned rotators, contrary to observation. Goldreich (1970) o ...
Stellar Metamorphosis as Alternative to Nebular Hypothesis
... Mainstream has this process backwards and is exceedingly clueless because their definitions are unnecessarily complex and arbitrary. [28] 3. There is no physical mechanism in the solar nebula model to explain the angular momentum loss of the Sun.[5] If the nebular model were correct and all the mate ...
... Mainstream has this process backwards and is exceedingly clueless because their definitions are unnecessarily complex and arbitrary. [28] 3. There is no physical mechanism in the solar nebula model to explain the angular momentum loss of the Sun.[5] If the nebular model were correct and all the mate ...
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... “mean” value for what is found in the literature (using Vizier; Ochsenbein et al., 2000)1. The carbon star TW Hor is an exception in this sample. We include it because it was observed in the same UVES run as most of the other sample stars. According to the spectral type designations, the stars W Cet ...
... “mean” value for what is found in the literature (using Vizier; Ochsenbein et al., 2000)1. The carbon star TW Hor is an exception in this sample. We include it because it was observed in the same UVES run as most of the other sample stars. According to the spectral type designations, the stars W Cet ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... to determine rest-frame absolute magnitudes (Vega) and Kcorrections. As input, we use the MAG− AUTO photometry from the g′ BV r′ R imaging and assumed minimum photometric uncertainties in each bandpass of 0.05 mag. The photometry has been corrected for foreground Galactic extinction using the Schleg ...
... to determine rest-frame absolute magnitudes (Vega) and Kcorrections. As input, we use the MAG− AUTO photometry from the g′ BV r′ R imaging and assumed minimum photometric uncertainties in each bandpass of 0.05 mag. The photometry has been corrected for foreground Galactic extinction using the Schleg ...
Galaxy Spiral Arms
... while revolving with the galaxy as a whole. We all believe that the Pleiades Cluster stays together due to mutual gravitation between the component stars and gases. We can make some decent estimates of characteristics of this very large, tapering and somewhat cone-shaped, open cluster that we all ca ...
... while revolving with the galaxy as a whole. We all believe that the Pleiades Cluster stays together due to mutual gravitation between the component stars and gases. We can make some decent estimates of characteristics of this very large, tapering and somewhat cone-shaped, open cluster that we all ca ...
Rotational Doppler beaming in eclipsing binaries
... In general the detectability is a combination of source flux, eclipse duration, instrument stability and intrinsic amplitude. Source flux can be optimized using a bigger telescope, eclipse duration is unfortunately a given for an individual source, instrument stability is in the design of the instru ...
... In general the detectability is a combination of source flux, eclipse duration, instrument stability and intrinsic amplitude. Source flux can be optimized using a bigger telescope, eclipse duration is unfortunately a given for an individual source, instrument stability is in the design of the instru ...
A spectroscopic investigation of the O
... Moreover, the distribution of the orbital parameters provides observational clues to the way that O-type stars form and to the interactions during their evolution. Aims. Our objective is to constrain the multiplicity of a sample of O-type stars belonging to poorly investigated OB associations in the ...
... Moreover, the distribution of the orbital parameters provides observational clues to the way that O-type stars form and to the interactions during their evolution. Aims. Our objective is to constrain the multiplicity of a sample of O-type stars belonging to poorly investigated OB associations in the ...
Module1: Scale of the Universe
... Ask&your&students&to&discuss&some&possible&difBiculties&of&measuring&cosmic& distances&using¶llax.&Ensure&they&mention&the&following&points:& Parallax&shifts&are&always&small.&& Parallax&shift&is&even&smaller&than&the&apparent&size&of&the&star.&In&additional,& starlight&is&refracted&by&Earth's&a ...
... Ask&your&students&to&discuss&some&possible&difBiculties&of&measuring&cosmic& distances&using¶llax.&Ensure&they&mention&the&following&points:& Parallax&shifts&are&always&small.&& Parallax&shift&is&even&smaller&than&the&apparent&size&of&the&star.&In&additional,& starlight&is&refracted&by&Earth's&a ...
IAU GA, Prague, Aug 2006 - Spanish Virtual Observatory
... • Building a census of substellar objects implies the discovery of a statistically significant number of them through queries that combine attributes available from different archives. • This is an approach out of the scope of the "classical" methodology but that perfectly fits into the Virtual Obse ...
... • Building a census of substellar objects implies the discovery of a statistically significant number of them through queries that combine attributes available from different archives. • This is an approach out of the scope of the "classical" methodology but that perfectly fits into the Virtual Obse ...
404.06 Stephen Drake
... Total summed flare energy in soft X-ray band >~7 x 1034 erg/s (but observations stopped after half a day when Lx was still 10 x normal level) ...
... Total summed flare energy in soft X-ray band >~7 x 1034 erg/s (but observations stopped after half a day when Lx was still 10 x normal level) ...
A Spectroscopic Survey of a Sample of Active M Dwarfs.
... interested in seeing whether other indications of youth are present. It has long been known that single M dwarfs decline in activity with age. The discovery of the TW Hydrae Association (Kastner et al. 1997; Webb et al. 1999) shows that very young stars can be found in the immediate solar neighbourh ...
... interested in seeing whether other indications of youth are present. It has long been known that single M dwarfs decline in activity with age. The discovery of the TW Hydrae Association (Kastner et al. 1997; Webb et al. 1999) shows that very young stars can be found in the immediate solar neighbourh ...
Perseus (constellation)

Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.