VRI Light Curves of SS 433: Photometry and Model
We present the results of VRI CCD photometric observations of SS 433 andVRI light-curve modelings for SS 433. Observations were carried out inthe fall of 1995 using the 51-cm relfector at Osaka Kyoiku University.Three cycles of the binary phase were covered. The mean magnitudes andcolors during the observational periods were V = 14.0, R = 11.1, I =10.5; V - R = 2.88, V - I = 3.50, R - I = 0.62. On October 17 and 18 astrong flare was observed. Theoretical light curves were also calculatedusing a model in which SS 433 consists of a geometrically thick torusaround a compact star and a companion star filling the Roche lobe. Inthe torus picture VRI light curves were first calculated; forappropriate parameters VRI model light curves well reproduce theobservational profiles. In addition, the extinction was first derivedfrom the magnitude difference between the obervation and the model;AV ~ 6--7, AR ~ 3--4, and AI ~ 3. These values are in goodagreement with those of a previous observation.
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On the sytematic accuracy of the equatorial UBVRI standard stars
The considerable systematic difference in B-V between northern andsouthern measurements of the equatorial UBVRI standard stars arestudied. It is found that the northern data (Landolt 1983) are muchcloser to the original UBV system than the southern ones. The situationis less clear in the case of V and U-B.
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Photometry of Stars in the Field of V345 and V553 Aquilae
Not Available
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Photometry of Stars in the Field of the Mira EL Lyrae
Not Available
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Photometry of Stars in the Field of the Mira XY Aquilae
Not Available
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Photometry of Stars in the Field of the Mira YZ Draconis
Not Available
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Photometry of Stars in the Field of AV Cygni and DV Cygni
Not Available
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UBV(RI)c photometry of equatorial standard stars - A direct comparison between the northern and southern systems
UBV(RI)c photometry of 212 stars from Landolt's list of equatorialstandards is presented. The observations are tied to the system definedby Cousin's E-region standards. A comparison of the present results withLandolt's reveals reasonably good agreement for (V-R)c and (V-I)c, butmarked systematic differences for (B-V) and (U-B). The UBV systems ofCousins and Landolt are evidently not the same and both probably differfrom Johnson's original system.
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UBVRI Photometry of FKSZ Stars - Part One
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1987A&AS...70..369C&db_key=AST
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Application of the infrared flux method to globular cluster stars. The M 3 giant branch
A first attempt is presented to apply the Infrared Flux Method (IFM) todetermine the physical parameters of globular cluster stars on the basisof a new U, B, V, R, I, J, H, and K photometry for a set of red giantsin M 3. It is concluded that the IFM is useful for this application, asit provides a good determination of T(eff) and theta from reasonablephotometry. Linear radius can also be determined if the moduli distanceis known. The (V-K) index seems to be a good T(eff) indicator if theRidgway et al. (1980) calibration for field stars is used, even formetal-deficient stars, at least in the 3900-4600 K range.
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UBV Photometry of Equatorial Stars
Not Available
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Standardization of Broadband Photometry of Equatorial Standards
Not Available
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UBVRI photometric standard stars around the celestial equator
It is pointed out that accurate, internally consistent, and readilyaccessible standard star photometric sequences are necessary for thecalibration of the intensity and color data which astronomers obtain atthe telescope. The photometric results provided in connection with thepresent study represent the first part of an effort which is concernedwith the presentation of UBVRI photoelectric photometric standard starsin the magnitude range from 7 to 17 over as broad a range in color aspossible. All of the photometric observations were made with a 31034type photomultiplier used in a pulse counting mode. Some 15 to 25standard stars chosen from Cousins' lists (1973, 1976) in the E-regionswere observed with an 0.4-m telescope each night along with the programstars. UBVRI standard stars were observed periodically throughout thenight. Observations with a 0.9-m telescope were also conducted. TheUBVRI photoelectric observations take into account 223 stars.
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A UBVRI equatorial extinction star network
An equatorial-extinction star network, based on 1503 observations of 37stars, is presented. These results together with those of Crawford etal. (1971) provide a well-determined UBVRI extinction network.Identification charts are included.
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Distances to eclipsing binaries. III - Masses, radii, and absolute magnitudes of 96 stars
Distances to, and absolute magnitudes of, 96 components of eclipsingbinaries with well-determined absolute dimensions have been computedusing V-R photometry. The calculations take into account interstellarreddening, which is estimated from existing UBV and uvby-betaphotometry, as well as photometric proximity effects. The resultingabsolute magnitudes, dimensions, and masses are compared with zero-agemain sequences predicted by theory. Theory is in good agreement with theobserved data for stars more massive than the sun if a composition (X,Y, Z) = (0.66 + or - 0.03, 0.303 + or - 0.03, 0.037 + or - 0.005) ischosen. The corresponding helium-to-hydrogen number ratio is 0.115 + or- 0.02, in agreement with previous estimates.
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A UBV equatorial-extinction star network
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1971PASP...83..652C&db_key=AST
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