תוכן
תמונות
הוסף תמונה שלך
DSS Images Other Images
מאמרים קשורים
Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| On the origin of binaries with twin components
The existence of a statistically significant excess of dwarf binarieswith mass ratios from 0.95 to 1, as first noted by Lucy & Ricco (?),is confirmed by modern data. Excess of such binaries, called twins, isfound only for periods shorter than 40 days, and in the 2-30 days periodrange they constitute 10-20% of the total binary population. Twins musthave been formed by a special mechanism. It cannot be a mass transfer incontact pre-main-sequence binaries, fission is also unlikely. As shownby Bate (2000), accretion onto a close binary shifts mass ratio towards1, so twins may originate from binaries that became close while stillsurrounded by massive envelopes. Many twins are members ofhigher-multiplicity systems and/or clusters, which probably explains anearly formation of a close binary by stellar dynamics.
| The Tokyo PMC catalog 90-93: Catalog of positions of 6649 stars observed in 1990 through 1993 with Tokyo photoelectric meridian circle
The sixth annual catalog of the Tokyo Photoelectric Meridian Circle(PMC) is presented for 6649 stars which were observed at least two timesin January 1990 through March 1993. The mean positions of the starsobserved are given in the catalog at the corresponding mean epochs ofobservations of individual stars. The coordinates of the catalog arebased on the FK5 system, and referred to the equinox and equator ofJ2000.0. The mean local deviations of the observed positions from theFK5 catalog positions are constructed for the basic FK5 stars to comparewith those of the Tokyo PMC Catalog 89 and preliminary Hipparcos resultsof H30.
| BVRI photometry of spectroscopic binaries
Not Available
| ICCD Speckle Observations of Binary Stars.XV.An Investigation of Lunar Occultation Systems
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1996AJ....112.2260M&db_key=AST
| Spectroscopic binary orbits from photoelectric radial velocities. A synopsis of papers 1-100
Not Available
| Spectroscopic binary orbits from photoelectric radial velocities. Paper 97: HD 98439
Not Available
| Derivation of angular diameters of stars from lunar occultations
A description is presented of the results obtained in the photoelectricobservations of occultations involving four stars. The considered starsinclude Eta Gem (ZC 946), Mu Gem (ZC 976), 187 B. Gem (ZC 1161), and 31Leo (ZC 1486). The theoretical principles of the studies are considered,taking into account point source occultations, the stellar diameter andthe influence of telescope aperture, and spectral effects. Observationaldata concerning the considered stars are presented in a table and anumber of graphs. It is pointed out that Mu Gem is a triple system.However, on account of their distances and their weakness the companionscannot affect the observed intensity curve. A combination of the deriveddiameter with the trigonometric parallax reported by Jenkins (1963)provides for the linear diameter of Mu Gem the result of 91 plus orminus 28 solar diameters.
| Some thoughts on multiple stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977RMxAA...3...13E&db_key=AST
| Photoelectric measurements of lunar occultation. VI. Further observational results.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1973AJ.....78..482D&db_key=AST
| The Kreinin-Murri Method for Absolute Determination of Equatorial-Star Declinations.
Not Available
|
הכנס מאמר חדש
לינקים קשורים
הכנס לינק חדש
משמש של הקבוצה הבאה
|
תצפית ומידע אסטרומטרי
| קבוצת-כוכבים: | אריה |
| התרוממות ימנית: | 11h19m32.93s |
| סירוב: | -00°11'17.8" |
| גודל גלוי: | 7.912 |
| מרחק: | 68.634 פארסק |
| תנועה נכונה: | 70 |
| תנועה נכונה: | -151.1 |
| B-T magnitude: | 8.569 |
| V-T magnitude: | 7.967 |
קטלוגים וכינוים:
|
