1 edition of Abundance spread within globular clusters found in the catalog.
Abundance spread within globular clusters
|Statement||edited by G. Cayrel de Strobel, M. Spite and T. Lloyd Evans.|
CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): Summary. Galactic globular cluster stars exhibit abundance patterns which are not shared by their field counterparts. It is clear from recent spectroscopic observations of GC turnoff stars that these abundance anomalies were already present in the gas from which the observed stars formed. Context: M 75 is a relatively young Globular Cluster (GC) found at 15 kpc from the Galactic centre at the transition region between the inner and outer Milky.
Milky Way. These are globular clusters within the halo of the Milky Way galaxy. The diameter is in minutes of arc as seen from Earth. For reference, the J epoch celestial coordinates of the Galactic Center are R.A. 17 h 45 m s, Dec. −29° 00′ ″. A high proportion of globular clusters are located in the Ophiuchus and Sagittarius constellations, both of which lie in the. Italian researchers have investigated the chemical composition of NGC , a massive globular cluster in the Milky Way galaxy. Their analysis, .
Globular clusters are roughly spherical, densely packed groups of stars found around galaxies. Most globular clusters probably formed at the same time as their host galaxies. Therefore they provide a unique fossil record of the conditions during the formation and early evolution of by: Globular clusters are extremely luminous objects. Their mean luminosity is the equivalent of approximat most luminous are 50 times brighter. The brightest stars are the red giants, bright red stars with an absolute magnitude of −2, about times the Sun’s brightness, or luminosity. In relatively few globular clusters have stars as intrinsically faint as the Sun been.
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Account the measurement errors, the intrinsic abundance dispersion is σ int[Fe/H] = dex. Among the Galactic globular clusters, the abundance dispersion in NGC is only exceeded by ω Cen, which is regarded as the remnant of a disrupted dwarf galaxy, and M 54, which is the nuclear star cluster of the Sagittarius dwarf by: 9.
At a Galactocentric distance of 27 kpc, Palomar 13 is an old globular cluster (GC) belonging to the outer halo. We present a chemical abundance analysis of this remote system from high-resolution spectra obtained with the Keck/HIRES spectrograph. The properties of abundance inhomogeneities in globular clusters are discussed.
Some of the most pronounced star-to-star variations are seen in the strengths of the molecular bands of CN and CH, with stars having enhanced CN bands being very : G. Smith. But we have known for more than twenty years 1 that the surface abundances, which are what we observe, of elements such as C, N and O can vary substantially from red giant to red giant within an individual globular cluster.
Indeed it has become clear that “abundance anomalies” of this type are common in the galactic globular cluster by: 5.
Among the Galactic globular clusters, the abundance dispersion in NGC is only exceeded by omega Cen, which is regarded as the remnant of a disrupted dwarf galaxy, and M 54, which is the nuclear star cluster of the Sagittarius dwarf by: 9.
Abstract Abundance variations within globular clusters (GCs), and of GC stars with respect to field stars, are important diagnostics of a variety of physical phenomena, related to the evolution of individual stars, mass transfer in binary systems, and chemical evolution in high density environments.
The broad astrophysical implications of GCs as building blocks of our knowledge of the Universe make a full Cited by: Abundances of C, N, and O are determined in four bright red giants that span the known abundance range for light (Na and Al) and s-process (Zr and La) elements in the globular cluster NGC The abundance sum C+N+O exhibits a range of dex, a factor of 4, in contrast to other clusters in which no significant C+N+O spread is found.
The stars' composition in globular clusters is known to a good accuracy, but many clusters present a spread in metallicity and helium content [13, 14,, which in principle could.
There is now clear evidence the metallicities of globular clusters are not simple tracers of the elemental abundances in their protocluster clouds; some of the heavy elements were formed subsequently within the cluster itself.
It is also manifestly clear that star formation is a clumpy process. We present a brief overview of a theoretical model for how self-enrichment by supernova ejecta Author: Jeremy Bailin. Among the Galactic globular clusters, the abundance dispersion in NGC is only exceeded by ω Cen, which is regarded as the remnant of a disrupted dwarf galaxy, and M54, which is the nuclear star cluster of the Sagittarius dwarfCited by: 9.
Nothing but, three meetings on globular clusters have been organized; one meeting (CM37/3) was chaired by T. Loyd Evans and was devoted to “The abundance spread within globular clusters”. Another meeting (JCM7), directed by Pierre Demarque gave us an overview of: “Stars clusters in the Magellanic Clouds”.Author: Derek McNally.
CiteSeerX - Document Details (Isaac Councill, Lee Giles, Pradeep Teregowda): We numerically investigate abundance properties of the Galactic globular clusters (GCs) by adopting a new “external pollution ” scenario.
In this framework, GCs are assumed to originate in forming low-mass dwarfs embedded in dark matter subhalos at very high redshifts (z) and thus be chemically influenced by field.
Occasionally, a globular cluster is known simply as a globular. Globular clusters are found in the halo of a galaxy and contain considerably more stars, and are much older than the less dense open clusters, which are found in the disk of a galaxy. chemical evolution within globular clus-ters. The evidence is much clearer for the most massive clusters.
Many au-thors have proposed that (at least the most massive) globular clusters may be closely related to the nuclei of dwarf galaxies. I review recent results on the chemical inhomogeneities in globular clusters and discuss the perspectives.
ω Centauri is the only globular star cluster in the Galactic halo known to have multiple stellar populations with a significant spread in iron abundance and age.
But now Terzan 5, a globular. Yet some of the abundance trends that we find defy a simple allocation of 47 Tuc to the thick disk; for instance, the high [Al/Fe] ratio in the globular cluster are at odds with the significant enrichment by SNe Ia in the disk as reported (e.g., by Prochaska et al.
; Feltzing et al.) and at this stage we refrain from over-interpreting any Cited by: *Globular clusters are bigger (radius of 40 - ly) and denser, with older stars that are much more strongly bound together.
Contains from a few hundred thousand to several million stars. Globular clusters are metal-poor and are located away from the Milky way, "halo". Start studying Ch. Learn vocabulary, terms, and more with flashcards, games, and other study tools.
Search. Browse. What do globular clusters tell us about our Galaxy and our place within it. the gas in the Galaxy was spread over an irregular, extended region of space spanninglight years.
The most massive globular cluster in the Milky Way, ω Centauri, is thought to be the remaining core of a disrupted dwarf galaxy 1,2, as expected within Cited by: Several globular clusters (GCs) in the Galaxy are observed to show internal abundance spreads in r -process elements (e.g., Eu).
We propose a new scenario that explains the origin of these GCs (e.g., M5 and M15). In this scenario, stars with no/little abundance variations. Structure and Dynamics of Globular Clusters Volume: 50 Year: View this Volume on ADS eISBN: Electronic access to books and articles is now available to purchase.
Volume eAccess: $ Printed and eAccess: Variable, see Astroshop Globular Cluster Color Profiles at High Resolution - a Case Study of. Abstract Abundance variations within globular clusters (GCs), and of GC stars with respect to field stars, are important diagnostics of a variety of physical phenomena, related to the evolution of individual stars, mass transfer in binary systems, and chemical evolution in high density environments.
The broad astrophysical implications of GCs as building blocks of our knowledge of the .Abstract Abundance variations within globular clusters (GCs), and of GC stars with respect to field stars, are important diagnostics of a variety of physical phenomena, related to the evolution of.