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Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available

UBV Photoelectric Times of Minima of the Eclipsing Variable TV Cassiopeiae
Not Available

Radial velocities. Measurements of 2800 B2-F5 stars for HIPPARCOS
Radial velocities have been determined for a sample of 2930 B2-F5 stars,95% observed by the Hipparcos satellite in the north hemisphere and 80%without reliable radial velocity up to now. Observations were obtainedat the Observatoire de Haute Provence with a dispersion of 80Ä,mm(-1) with the aim of studying stellar and galactic dynamics.Radial velocities have been measured by correlation with templates ofthe same spectral class. The mean obtained precision is 3.0 km s(-1)with three observations. A new MK spectral classification is estimatedfor all stars. Based on observations made at the Haute ProvenceObservatory, France and on data from The Hipparcos Catalogue, ESA.Tables 4, 5 and 6 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr or viahttp://cdsweb.u-strasbg.fr/Abstract.htm

A spectral survey of early-type stars in the region of Cassiopeia using an objective prism
Not Available

Radial velocity measurements. I - Ground-based observations of the program stars for the HIPPARCOS satellite
The radial velocities of 272 stars brighter than m(pg) = 8.5 aredetermined by digital microphotometric measurement of plates obtainedwith dispersion 80 A/mm using the Marly slit spectrograph on the 120-cmtelescope of the Observatoire de Haute Provence. The objects wereselected as probable members of the input catalog for the ESA Hipparcosastrometric satellite. The measurement techniques and data-reductionprocedures are described in detail, and the results are presented inextensive tables and graphs and briefly characterized.

TV Cassiopeiae in the Utrecht photometric system
Four UPS light curves of TV Cas are presented. An instantaneous periodanalysis of these curves and previously published data reveals erraticrelative period changes of over 10E-6 a year. The secondary minimumappears to be at phase 0.502. Light curve analysis indicates that thecool component fills its Roche lobe and is of spectral type G5-G9IV.Roche lobe overflow is not sufficient to explain the observed seculardecrease of the period. Other mechanisms may be found in thechromospheric activity of the cool component. This activity is suggestedby the observed small variations in the light curves with acharacteristic period of about a year.

V377 Cassiopeiae = BD +58 28 = HD 1479 zeigt keine Veränderlichkeit.
Not Available

Period study and UBV light curves of TV Cassiopeiae
Abstract image available at:http://adsabs.harvard.edu/abs/1977AJ.....82..740G

Photoelectric Photometry of TV CAS
Not Available

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Membre dels grups següents:

Dades d'Observació i Astrometria

Constel·lació:Cassiopeia
Ascensió Recta:00h15m48.61s
Declinació:+59°26'24.9"
Magnitud Aparent:7.894
Distancia:239.808 parsecs
Moviment propi RA:7.6
Moviment propi Dec:-5.1
B-T magnitude:7.948
V-T magnitude:7.899

Catàlegs i designacions:
Noms Propis   (Edit)
HD 1989HD 1128
TYCHO-2 2000TYC 3665-1211-1
USNO-A2.0USNO-A2 1425-00374713
HIPHIP 1259
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