Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... times brighter than stars like the Sun, their total luminosity will approximately equal that of 2 × 1010 of these. Thus, during the star formation activity the galaxy increases its luminosity by ∼ 20%. Its colors also become bluer, because the radiation emitted by massive stars is very rich of light ...
... times brighter than stars like the Sun, their total luminosity will approximately equal that of 2 × 1010 of these. Thus, during the star formation activity the galaxy increases its luminosity by ∼ 20%. Its colors also become bluer, because the radiation emitted by massive stars is very rich of light ...
Conference Abstract Booklet here.
... of an RCB star: the merger of a CO/He WD binary and a final helium-shell flash. RCB stars show periodic or semi-periodic light and radial velocity fluctuations due to both radial and non-radial pulsations. A number of RCB stars are now being studied with K2. A correlation between pulsation phase and ...
... of an RCB star: the merger of a CO/He WD binary and a final helium-shell flash. RCB stars show periodic or semi-periodic light and radial velocity fluctuations due to both radial and non-radial pulsations. A number of RCB stars are now being studied with K2. A correlation between pulsation phase and ...
The Chemical Composition of Carbon-Rich, Very Metal
... put forward to account for the moderately metal-poor classical CH stars ([Fe/H]∼ −1.5). These are usually explained by a model involving mass transfer from a carbon-enhanced asymptotic giant branch (AGB) star (one that has since evolved to the white dwarf stage and cannot now be seen) to its lower-m ...
... put forward to account for the moderately metal-poor classical CH stars ([Fe/H]∼ −1.5). These are usually explained by a model involving mass transfer from a carbon-enhanced asymptotic giant branch (AGB) star (one that has since evolved to the white dwarf stage and cannot now be seen) to its lower-m ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
3-1
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
... B. 0.6 + 0.008 + 0.0007 Standard form: 0.6087 Word form: six thousand eighty-seven tenthousandths Course 1 ...
Teil 2
... suggests that the flip-flop phenomenon is caused by changing the relative strengths of the spot groups at the two active longitudes without actual spot movement on the stellar surface. Inversions of light-curves result in maps of spot filling factor. The second figure shows the phases of the maximum ...
... suggests that the flip-flop phenomenon is caused by changing the relative strengths of the spot groups at the two active longitudes without actual spot movement on the stellar surface. Inversions of light-curves result in maps of spot filling factor. The second figure shows the phases of the maximum ...
A trip to the end of the universe and the twin “paradox”
... defined by local measurements of reflected light signals. The interesting information that both twins can interchange in our example are their individual proper times. They will not be able to determine the time dilation from this proper time because the information carrying the proper time of the o ...
... defined by local measurements of reflected light signals. The interesting information that both twins can interchange in our example are their individual proper times. They will not be able to determine the time dilation from this proper time because the information carrying the proper time of the o ...
- ANU Repository
... distribution and period distribution of planets. Unlike previous approaches, MIMC analyses planets as discrete values or distributions of values that can include non-trivial priors on parameters. Silburt et al. (2015) pointed out that because of detection bias, errors in radii of small planets will ...
... distribution and period distribution of planets. Unlike previous approaches, MIMC analyses planets as discrete values or distributions of values that can include non-trivial priors on parameters. Silburt et al. (2015) pointed out that because of detection bias, errors in radii of small planets will ...
targets - siamois
... - less noise at low frequency - measurement of modes up to degree l= 3 - observation of bright stars very precise inversion and modelling ...
... - less noise at low frequency - measurement of modes up to degree l= 3 - observation of bright stars very precise inversion and modelling ...
Observations of Jets and Outflows from Young Stars
... 500 km s−1 . Internal shocks form where faster ejecta overrun slower material. The very fastest shocks can sometimes be detected in X-rays. These primary flows often contain molecules such as H2 , CO, and SiO when launched from young Class 0/I sources; they tend to be dominated by HI and low-ionizat ...
... 500 km s−1 . Internal shocks form where faster ejecta overrun slower material. The very fastest shocks can sometimes be detected in X-rays. These primary flows often contain molecules such as H2 , CO, and SiO when launched from young Class 0/I sources; they tend to be dominated by HI and low-ionizat ...
HWWS 2010 - Monash University
... … and even some new flavours • Rotating radio transients (RRATs); “intermittent” radio pulsars • Soft Gamma-ray Repeaters (SGRs); isolated neutron stars that show (occasionally violent) gamma-ray outbursts & pulsations • Anomalous X-ray pulsars (AXPs); isolated neutron stars with long pulse periods ...
... … and even some new flavours • Rotating radio transients (RRATs); “intermittent” radio pulsars • Soft Gamma-ray Repeaters (SGRs); isolated neutron stars that show (occasionally violent) gamma-ray outbursts & pulsations • Anomalous X-ray pulsars (AXPs); isolated neutron stars with long pulse periods ...
Is there a Supermassive Black Hole at the Center of the Milky Way?
... picture of these “radio galaxies.” The radio waves did not come from the galaxy itself, but from two giant “lobes” symmetrically placed about, but well separated from, the parent galaxy (see Fig. 1). These lobes can be among the largest structures in the Universe, hundreds of times the size of the p ...
... picture of these “radio galaxies.” The radio waves did not come from the galaxy itself, but from two giant “lobes” symmetrically placed about, but well separated from, the parent galaxy (see Fig. 1). These lobes can be among the largest structures in the Universe, hundreds of times the size of the p ...
1. INTRODUCTION - Institut für Theoretische Astrophysik
... We calculate time-dependent models of acoustically heated chromospheres for main-sequence stars between spectral type F0 V and M0 V and for two giants of spectral type K0 III and K5 III assuming monochromatic waves. The hydrodynamic equations are solved together with the radiative transfer and stati ...
... We calculate time-dependent models of acoustically heated chromospheres for main-sequence stars between spectral type F0 V and M0 V and for two giants of spectral type K0 III and K5 III assuming monochromatic waves. The hydrodynamic equations are solved together with the radiative transfer and stati ...
Mn, Cu, and Zn abundances in barium stars and their correlations
... a variety of nucleosynthetic processes, including explosive nucleosynthesis in SN II and SN Ia, the main component of the s-process, thought to occur in the He-burning shells of low to intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ...
... a variety of nucleosynthetic processes, including explosive nucleosynthesis in SN II and SN Ia, the main component of the s-process, thought to occur in the He-burning shells of low to intermediate mass AGB stars, and the weak component of the s-process, thought to be sited at He-burning cores of M ...
The Paranatellonta in ancient Greek astrological literature
... not add anything else to what has been said about it in Sphaera. It is obvious that the stone on which everything else rests is the dating of Antiochus, which in turn is uncertain and on which, as we shall see in its own place, scholars are in complete disagreement. Even our Teucer's birth place is ...
... not add anything else to what has been said about it in Sphaera. It is obvious that the stone on which everything else rests is the dating of Antiochus, which in turn is uncertain and on which, as we shall see in its own place, scholars are in complete disagreement. Even our Teucer's birth place is ...
AGN surveys to study galaxy evolution along cosmic times
... of galaxies. We also know that they are deeply connected, as shown by the so-called Magorrian relation (Magorrian et al. 1998). We want to know the full cosmic history of energy generation by stars (star formation) and AGNs (black hole accretion). These energy production rates correspond to built up ...
... of galaxies. We also know that they are deeply connected, as shown by the so-called Magorrian relation (Magorrian et al. 1998). We want to know the full cosmic history of energy generation by stars (star formation) and AGNs (black hole accretion). These energy production rates correspond to built up ...
Magnitude-range brightness variations of overactive K giants
... IL Hya and up to 54% in XX Tri over the course of our observations. We emphasize that for IL Hya this is just about half of the total luminosity variation that can be explained by the photospheric temperature (spots/faculae) changes, while for XX Tri it is even about one third. The long-term, 0.m 6 ...
... IL Hya and up to 54% in XX Tri over the course of our observations. We emphasize that for IL Hya this is just about half of the total luminosity variation that can be explained by the photospheric temperature (spots/faculae) changes, while for XX Tri it is even about one third. The long-term, 0.m 6 ...
21 -26 August University of Exeter
... by cloud-cloud collisions. Future large radio observations with finer spatial resolution and higher sensitivity can observe giant molecular clouds with much lower mass than before, which may put unique constraints on the giant molecular cloud formation/dispersal timescales in different environment o ...
... by cloud-cloud collisions. Future large radio observations with finer spatial resolution and higher sensitivity can observe giant molecular clouds with much lower mass than before, which may put unique constraints on the giant molecular cloud formation/dispersal timescales in different environment o ...
Hubble Space Telescope Imaging of Post
... The F606W filter corresponds to the rest-frame B of the sample and probes rest-frame wavelengths near the peak output for ∼ 100 Myr stellar populations enhancing the stellar/AGN contrast. At HSTs resolution (∼0.0500 ) and an average redshift of hzi ∼ 0.319, an galaxy with a 500 diameter corresponds ...
... The F606W filter corresponds to the rest-frame B of the sample and probes rest-frame wavelengths near the peak output for ∼ 100 Myr stellar populations enhancing the stellar/AGN contrast. At HSTs resolution (∼0.0500 ) and an average redshift of hzi ∼ 0.319, an galaxy with a 500 diameter corresponds ...
The Astronomers of Nabta Playa
... vernal equinox heliacal (i.e., rising together with the sun on the first day of spring) position on the horizon. The other aligned with a reference star, in this case Vega, thus fixing the first star’s rising at a specific date in history. In archaeoastronomy single megalithic alignments with stars ...
... vernal equinox heliacal (i.e., rising together with the sun on the first day of spring) position on the horizon. The other aligned with a reference star, in this case Vega, thus fixing the first star’s rising at a specific date in history. In archaeoastronomy single megalithic alignments with stars ...
Fluorine abundances in dwarf stars of the solar neighbourhood⋆
... Cloud and in the globular cluster ω Cen. They found that the abundance ratio of F/O declines as the oxygen abundance decreases. They therefore suggested that the observed low values of F/O exclude AGB synthesis as the dominant source of fluorine in their targeted stellar populations. In particular, ...
... Cloud and in the globular cluster ω Cen. They found that the abundance ratio of F/O declines as the oxygen abundance decreases. They therefore suggested that the observed low values of F/O exclude AGB synthesis as the dominant source of fluorine in their targeted stellar populations. In particular, ...
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.