PPT presentation
... constant; in some places there are no PNs and all you detect are the contaminants. This is frustrating but it teaches us that the distribution of the ICPNs is far from relaxed in Virgo. ...
... constant; in some places there are no PNs and all you detect are the contaminants. This is frustrating but it teaches us that the distribution of the ICPNs is far from relaxed in Virgo. ...
Astronomy Astrophysics NGC 7419 as a template for red supergiant clusters &
... spectroscopy around the Hα line for most of the candidate Be stars, confirming their nature. A second peculiarity of NGC 7419 is the presence of five red supergiants (RSGs) as confirmed radial velocity members of the cluster (Beauchamp et al. 1994). Until recently, this was the highest number of RSG ...
... spectroscopy around the Hα line for most of the candidate Be stars, confirming their nature. A second peculiarity of NGC 7419 is the presence of five red supergiants (RSGs) as confirmed radial velocity members of the cluster (Beauchamp et al. 1994). Until recently, this was the highest number of RSG ...
Cassiopeia Kelly Pearce
... that the hundreds or even thousands of objects within it formed at the same time, from the same nebulae (Gater & Vamplew, 2010, p.88). There is one object within the NGC 457 that is not a part of the open cluster and is actually a red giant that is approximately 6,700 light-years closer than the rem ...
... that the hundreds or even thousands of objects within it formed at the same time, from the same nebulae (Gater & Vamplew, 2010, p.88). There is one object within the NGC 457 that is not a part of the open cluster and is actually a red giant that is approximately 6,700 light-years closer than the rem ...
- MNASSA Page
... is relatively easily to see, and gives the impression of riding along on top of this glow. The magnitude 12.2 star on the southern end of the nebula is a distracting factor drawing the eye away. Nebulosity very much interweaves the lovely star NGC 2032, the larger and brighter, north- grouping NGC 2 ...
... is relatively easily to see, and gives the impression of riding along on top of this glow. The magnitude 12.2 star on the southern end of the nebula is a distracting factor drawing the eye away. Nebulosity very much interweaves the lovely star NGC 2032, the larger and brighter, north- grouping NGC 2 ...
Statistical analysis of stellar evolution
... one-dimensional curve. Sophisticated Markov chain Monte Carlo (MCMC) methods are required to explore these distributions. Our strategy involves dynamically transforming the parameters with the aim of reducing correlations. We use initial ...
... one-dimensional curve. Sophisticated Markov chain Monte Carlo (MCMC) methods are required to explore these distributions. Our strategy involves dynamically transforming the parameters with the aim of reducing correlations. We use initial ...
Open clusters in the Third Galactic Quadrant III. Alleged binary
... content may become evident in some clusters from the reddening estimation. Therefore, we applied the same metal content set of isochronous lines (Girardi et al. 2000) until the best MS match is achieved in the CMD. The method is exemplified with the cluster Haffner 10 (see Sect. 4.1.1) where a simult ...
... content may become evident in some clusters from the reddening estimation. Therefore, we applied the same metal content set of isochronous lines (Girardi et al. 2000) until the best MS match is achieved in the CMD. The method is exemplified with the cluster Haffner 10 (see Sect. 4.1.1) where a simult ...
Slide 1
... their electrons overlap. This happens for stars with cores up to 3 times heavier than the sun. This is the case with neutron stars. When a big core dies, gravity crushes down, but it crushes even harder than electron degeneracy pressure. As the electrons overlap, they merge with the protons to turn ...
... their electrons overlap. This happens for stars with cores up to 3 times heavier than the sun. This is the case with neutron stars. When a big core dies, gravity crushes down, but it crushes even harder than electron degeneracy pressure. As the electrons overlap, they merge with the protons to turn ...
Stars - Emera Astronomy Center
... two brightest stars mark opposite ends of the constellation. Regulus, the heart of the lion, is at Leo's western edge. And the second-brightest star, Denebola, marks Leo's tail at the constellation's eastern end. Look for it above and to the left of the full Moon this evening, and to the lower left ...
... two brightest stars mark opposite ends of the constellation. Regulus, the heart of the lion, is at Leo's western edge. And the second-brightest star, Denebola, marks Leo's tail at the constellation's eastern end. Look for it above and to the left of the full Moon this evening, and to the lower left ...
On the nature and detectability of Type Ib/c supernova progenitors
... YWL21) end their lives while they are filling their Rochelobes during Case ABB or BB mass transfer (i.e., mass transfer from the He star during/after the carbon-oxygen core contraction phase; see Yoon et al. 2010 for more details). For comparison, the evolutionary track of a single, pure helium star ...
... YWL21) end their lives while they are filling their Rochelobes during Case ABB or BB mass transfer (i.e., mass transfer from the He star during/after the carbon-oxygen core contraction phase; see Yoon et al. 2010 for more details). For comparison, the evolutionary track of a single, pure helium star ...
Main-Sequence Stars and the Sun
... wanted to describe it in astronomical nomenclature, we would call it a G2V star. Its spectral class is G2, and its luminosity class is V. Be careful not to confuse type V main-sequence stars with white dwarfs, which are much smaller. White dwarfs will be discussed in Chapter 9. ...
... wanted to describe it in astronomical nomenclature, we would call it a G2V star. Its spectral class is G2, and its luminosity class is V. Be careful not to confuse type V main-sequence stars with white dwarfs, which are much smaller. White dwarfs will be discussed in Chapter 9. ...
Distance determination for RAVE stars using stellar models
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
... spirals, and finally dwarf galaxies. The power spectrum is used to measure the power of density perturbations on a certain scale. The current cosmological model predicts a HarrisonZel’dovich spectrum (P (k) ∝ k, where k is the wavenumber). This power spectrum predicts more power on small scale, so t ...
Lecture 14
... • Parallax precision p ~ 10-5 arcsec for 1 billion stars – 100x better parallaxes – 10,000x more stars – Stars that are ~100 times fainter than Hipparcos ...
... • Parallax precision p ~ 10-5 arcsec for 1 billion stars – 100x better parallaxes – 10,000x more stars – Stars that are ~100 times fainter than Hipparcos ...
October 2016 BRAS Newsletter - The Baton Rouge Astronomical
... ‘The burst of the century’ “This was the burst of the century!” exclaimed James A. Wren, an engineer at Los Alamos National Laboratory and coauthor of one of the papers. Indeed, GRB 130427A (as it is now called) was the most powerful gamma-ray burst and the secondbrightest optical flash measured in ...
... ‘The burst of the century’ “This was the burst of the century!” exclaimed James A. Wren, an engineer at Los Alamos National Laboratory and coauthor of one of the papers. Indeed, GRB 130427A (as it is now called) was the most powerful gamma-ray burst and the secondbrightest optical flash measured in ...
Chapter 16--Properties of Stars
... mysterious points of light in the sky. We now know that all stars form in great clouds of gas and dust. Each star begins its life with roughly the same chemical composition: About three-quarters of the star’s mass at birth is hydrogen, and about one-quarter is helium, with no more than about 2% cons ...
... mysterious points of light in the sky. We now know that all stars form in great clouds of gas and dust. Each star begins its life with roughly the same chemical composition: About three-quarters of the star’s mass at birth is hydrogen, and about one-quarter is helium, with no more than about 2% cons ...
Auriga (constellation)
Auriga is one of the 48 constellations listed by the 2nd-century astronomer Ptolemy and remains one of the 88 modern constellations. Located north of the celestial equator, its name is the Latin word for ""charioteer"", associating it with various mythological charioteers, including Erichthonius and Myrtilus. Auriga is most prominent during winter evenings in the Northern Hemisphere, along with the five other constellations that have stars in the Winter Hexagon asterism. Because of its northern declination, Auriga is only visible in its entirety as far as 34° south; for observers farther south it lies partially or fully below the horizon. A large constellation, with an area of 657 square degrees, it is half the size of the largest constellation, Hydra.Its brightest star, Capella, is an unusual multiple star system among the brightest stars in the night sky. Beta Aurigae is an interesting variable star in the constellation; Epsilon Aurigae, a nearby eclipsing binary with an unusually long period, has been studied intensively. Because of its position near the winter Milky Way, Auriga has many bright open clusters in its borders, including M36, M37, and M38, popular targets for amateur astronomers. In addition, it has one prominent nebula, the Flaming Star Nebula, associated with the variable star AE Aurigae.In Chinese mythology, Auriga's stars were incorporated into several constellations, including the celestial emperors' chariots, made up of the modern constellation's brightest stars. Auriga is home to the radiant for the Aurigids, Zeta Aurigids, Delta Aurigids, and the hypothesized Iota Aurigids.