2 edition of Rutherfurd photographs of the stellar clusters h and x Persei ... found in the catalog.
Rutherfurd photographs of the stellar clusters h and x Persei ...
Anne Sewell Young
in New York
Written in English
|LC Classifications||QB4 .C72 no. 24|
|The Physical Object|
|Pagination||iv, -76 p.|
|Number of Pages||76|
|LC Control Number||07034606|
Page 1 of 2 - Double Cluster in Perseus - posted in Deep Sky Observing: Rising in the North Eastern skies and at 11PM (EDT) it was high enough to enjoy with my 90mm F/11 refractor at 25X (about a degree FOV). This is a small scope, binocular object. Eclipsing binaries in open clusters - I. V Per and V Per in h Persei We derive absolute dimensions for two early-type main-sequence detachedeclipsing binaries in the young open cluster h Persei (NGC ). VPersei has a spectral type of B7 V and a period of d. V Perseiis A2 V and has a period of d.
Now known as h and chi Persei, or NGC (above right) and NGC , the clusters themselves are separated by only a few hundred light-years and contain stars much younger and hotter than the Sun. In addition to being physically close together, the clusters' ages based on their individual stars are similar - evidence that both clusters were. STARS and STARS OF THE WEEK Star Count: Created by Jim Kaler, Prof. Emeritus of Astronomy, University of Illinois Learn about stellar spectra in STARS AND THEIR SPECTRA: An Introduction to the Spectral Sequence, Second Ed., with two new chapters and new illustrations, Cambridge University Press (UK or North America), From the Sun to the .
a Persei cluster (age ",50 Myr) are rapidly rotating (vsini ~ km s-l),while another significant fraction are very slow rotators (v sini:5 10 km S-l). The spin down time scale for the rapidly rotating G stars appears to be between the age of the a Persei cluster and that of the Pleiades (age ",70 Myr), where most of the G. The Alpha Persei Cluster, also known as Melo is a bright stellar association in Perseus constellation. To the naked eye, the cluster consists of several blue stars of spectral type B, along with the most massive member, the yellow supergiant Alpha Persei itself. Brightest members include Alpha, Delta, Epsilon, Psi, 29, 30, 34 and 48 Persei.
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Adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86AAuthor: Anne Sewell Young. Additional Physical Format: Online version: Young, Anne Sewell, b.
Rutherfurd photographs of the stellar clusters h and x Persei. New York, Rutherfurd photographs of the stellar clusters h and x Persei By Anne Sewell Young.
Abstract. Mode of access: Internet Topics: Stars. Publisher: New York, Year: OAI identifier: oai::MIU Provided by: University of Michigan Author: Anne Sewell Young.
Discover Book Depository's huge selection of Anne Young books online. Free delivery worldwide on over 20 million titles. Rutherfurd Photographs of the Stellar Clusters H and X Persei. Anne Sewell Young. 19 Nov Hardback. US$ Rutherfurd Photographs of the Stellar Clusters H and X Persei.
Anne Sewell Young. 21 Feb h Persei and 2h22m5s.8, 57 8 43 for χ Persei. These positions are comparable to the cluster centers determined by Bragg & Kenyon (), which we will adopt in this paper: h Persei center = 2h18m56s.4, 57 8 25, χ Persei center = 2h22m4s.3, 57 8 Because the clusters are separated by ≈27 arcmin, the total.
Thus, within our deg 2 field there are probably cluster members for h Persei, for χ Persei, and for the low-density halo, yielding a total of 12, stars in h and χ Persei.
If lower-mass halo stars associated with the halo cover 1 deg 2 on the sky, consistent with our spectroscopic membership results for higher-mass stars. The two star clusters making up the Double Cluster are called NGC (h Persei) and NGC (Chi Persei).
The position of h Persei’s is Right Ascension: 2h 19m; Declination: 57 o 9′ north. The lengths of time one can expect the stars to remain on the main sequence are shown at the right of Fig. 3, The stars in galactic clusters belong to Population I those In M67 can be described as old Population I, while those in clusters such as NGC and h +-X Persei have been formed very recently and are extreme Population I.
This volume presents recent results of the studies of star-forming regions and the interstellar medium, stellar atmospheres and magnetism, activity of stars, multiple stellar systems and exoplanets, and stars after the nuclear burning stage.
Methods and instruments of present-day stellar astrophysics are also discussed. An illustration of an open book. Books. An illustration of two cells of a film strip. An illustration of two photographs. Images. An illustration of a heart shape Donate. An illustration of text ellipses.
More. An icon used to represent a menu that can be toggled by interacting with this icon. About Full text of "Star Clusters".
We derive absolute dimensions for two early-type main-sequence detached eclipsing binaries in the young open cluster h Persei (NGC ). V Persei has a spectral type of B7 V and a period of d. Stellar evolution as evidenced by members of open clusters near the turn-off from the main sequence.- Stroemgren photometry of F-type stars in M67 and NGC Statistical analysis of the red giant distributions of old open clusters.- X-ray survey of the Pleiades: dependence of X-ray luminosity on stellar age A special study now in progress at Harvard, of the environs of the Large Magellanic Cloud adds several new globular clusters to the list; some of them may not be outlying members of the Cloud, and two or three are not N.G.C.
or I.C. objects. In A Np () Lampland and Tombaugh report that N.G.C. is a typical globular cluster. Sometimes, two clusters born at the same time will form a binary cluster.
The best known example in the Milky Way is the Double Cluster of NGC and NGC (sometimes mistakenly called h and χ Persei; h refers to a neighboring star and χ to both clusters), but at least 10 more double clusters are known to exist. . massive stellar clusters, with a universal IMF. Formation of a bound stellar cluster from the super-shell expanding out of the gaseous cloud has been dis-cussed by Brown et al.
(, ). In their concept stars are formed when the supershell has swept out the entire cloud and expanded beyond its original boundary. The Pleiades, Praesepe, and the Hyades are open clusters; examples of globular clusters are the cluster M3 in the constellation Canes Venatici and the cluster M13 in Hercules.
In our galaxy open clusters are concentrated in the plane of symmetry of the Milky Way (the galactic plane) and possess a small velocity relative to the sun (20 km/sec on.
In the northern sky, stellar prominences have been detected in the G dwarf AP (located in the open cluster α Persei, Barnes et al. ), in RE. The Online Books Page. Rutherford Photographs of the Stellar Clusters h or x Persei Anne Sewell Young (January 2, – Aug ) was an American astronomer.
She was an astronomy professor at Mount Holyoke College for 37 years. imaging and allow us to see clusters closer to the epoch of their for-mation (e.g. Figure 1 shows the infrared H-band image of Mon R2, Carpenter et al.see also Plate 1). Figure 1. The Mon R2 cluster imaged in the near-infrared H-band (from Carpenter et al.
The ﬁeld of view is ∼ × arcmin2. Abstract. Observations of the stellar cluster in the central 10 pc of the Galaxy are reviewed. The stellar density law derived from the observed light distribution and the effects on this density law of variable extinction, the possibility of a varying mass-to-light ratio, and the current debate as to the core radius of the cluster are all important for establishing the true mass distribution.The Double Cluster (also known as Caldwell 14) is the common name for the open clusters NGC and NGC (often designated h Persei and χ Persei, respectively), which are close together in the constellation visible with the naked eye, NGC and NGC lie at a distance of light years.The two open clusters, known individually as Chi (χ) Persei (NGCat left) and h Persei (NGCright), formed 11 million and 12 million years .