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Speckle Interferometry of New and Problem HIPPARCOS Binaries
The ESA Hipparcos satellite made measurements of over 12,000 doublestars and discovered 3406 new systems. In addition to these, 4706entries in the Hipparcos Catalogue correspond to double star solutionsthat did not provide the classical parameters of separation and positionangle (rho,theta) but were the so-called problem stars, flagged ``G,''``O,'' ``V,'' or ``X'' (field H59 of the main catalog). An additionalsubset of 6981 entries were treated as single objects but classified byHipparcos as ``suspected nonsingle'' (flag ``S'' in field H61), thusyielding a total of 11,687 ``problem stars.'' Of the many ground-basedtechniques for the study of double stars, probably the one with thegreatest potential for exploration of these new and problem Hipparcosbinaries is speckle interferometry. Results are presented from aninspection of 848 new and problem Hipparcos binaries, using botharchival and new speckle observations obtained with the USNO and CHARAspeckle cameras.
| Mesures de vitesses radiales. VIII. Accompagnement AU sol DU programme d'observation DU satellite HIPPARCOS
We publish 1879 radial velocities of stars distributed in 105 fields of4^{\circ} \times 4^{\circ}. We continue the PPO series \cite[(Fehrenbachet al. 1987;]{Feh87} \cite[Duflot et al. 1990, 1992 and 1995),]{Du90}using the Fehrenbach objective prism method. Table 1 only available inelectronic form at CDS via to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| The infrared temporal evolution of FG Sagittae
We present near- and mid-infrared photometry of the post-AGB star FG Sgeobtained at two distinct epochs separated by a period of 10 yr.Observations of FG Sge taken in 1983 suggest that the 1 to 12 micronenergy distribution was produced at that time by a stellar photosphere,with a blackbody temperature of about 5600 K. In late August of 1992, FGSge exhibited a marked decline (about 3 mag in V) in its visible lightcurve. At the same time the 1 to 18.0 micron IR energy distribution hasevolved to become approximately a 1000 K blackbody. We propose that thislight decline partially is due to the ejection and condensation of adust shell. We esti mate the amount of dust condensed during thisepisode to be about 3.3 x 10 exp 9 solar masses with a covering factor(total visual depth) of about 0.3.
| An Einstein Observatory SAO-based catalog of B-type stars
About 4000 X-ray images obtained with the Einstein Observatory are usedto measure the 0.16-4.0 keV emission from 1545 B-type SAO stars fallingin the about 10 percent of the sky surveyed with the IPC. Seventy-fourdetected X-ray sources with B-type stars are identified, and it isestimated that no more than 15 can be misidentified. Upper limits to theX-ray emission of the remaining stars are presented. In addition tosummarizing the X-ray measurements and giving other relevant opticaldata, the present extensive catalog discusses the reduction process andanalyzes selection effects associated with both SAO catalog completenessand IPC target selection procedures. It is concluded that X-rayemission, at the level of Lx not less than 10 exp 30 ergs/s, is quitecommon in B stars of early spectral types (B0-B3), regardless ofluminosity class, but that emission, at the same level, becomes lesscommon, or nonexistent, in later B-type stars.
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Pozíciós és asztrometriai adatok
| Csillagkép: | Nyíl |
| Rektaszcenzió: | 20h10m45.15s |
| Deklináció: | +20°29'12.7" |
| Vizuális fényesség: | 7.447 |
| Távolság: | 1333.333 parszek |
| RA sajátmozgás: | 1.1 |
| Dec sajátmozgás: | -7.3 |
| B-T magnitude: | 7.357 |
| V-T magnitude: | 7.44 |
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