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Empirical temperature calibrations for early-type stars
Three temperature calibrations of suitable photometric quantities havebeen derived for O and B stars. A sample of 120 stars with reliableT(eff.) determinations has been used for establishing each calibration.The different calibrations have been critically discussed and compared.Temperature determinations for 1009 program stars have been obtainedwith an accuracy of the order of 10 percent.
| Starlight polarization in the direction of two H I complexes
Upper limits to the gas/dust ratio in the direction of two complexes arederived based on 21-cm line observations and starlight polarizationmeasurements. Elongated H I structures parallel to the galactic magneticfield suggest that the gas and dust comprise a common cloud or cloudsystem. Dust producing the starlight polarization is mixed with the H Igas, aiding in estimating the distance for the two H I complexes.Distances of 100 pc for the filament at low velocities and of 200 pc foran intermediate-velocity cloud complex (IVC) are established frompolarimetric data, and possible origins for the filaments and IVC aresuggested.
| H-beta photometry of southern early-type stars
H-beta photoelectric photometry is presented for 209 southern hemisphereearly-type stars from the HD catalog with galactic latitudes /b/ greaterthan 6 deg. Four-color photometry exists for all these stars and MKtypes for most of them. Absolute magnitudes have been estimated for allbut the emission-line stars and distances from the sun and the galacticplane determined.
| Four colour photometry of southern early-type stars.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978MNRAS.182..629K&db_key=AST
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Pozíciós és asztrometriai adatok
| Csillagkép: | Hajógerinc |
| Rektaszcenzió: | 09h07m39.61s |
| Deklináció: | -68°45'17.3" |
| Vizuális fényesség: | 7.527 |
| Távolság: | 476.19 parszek |
| RA sajátmozgás: | -7.4 |
| Dec sajátmozgás: | 8.4 |
| B-T magnitude: | 7.417 |
| V-T magnitude: | 7.518 |
Katalógusok és elnevezések:
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