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HD 5361

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Photoelectric photometry of the RRs variable GP And Medium-to-high-time-resolution photoelectric observations of the RRsvariable GP And are discussed. It is found that the fundamentalpulsation with period P1 0.07868270d is superposed by the followingtypes of disturbances: (1) variability of the mean brightness (no perioddetected); (2) variability of amplitude (possible period P2 0.64d); (3)superposition of an 18-minute wave (possibly only near minimum and withphase fluctuations); and (4) variability of the shape of the light curvein individual cycles.
Orbital elements and dimensions of the eclipsing binary AI Phe Spectroscopic observations of the 9th magnitude eclipsing binary AI Pheare reported and discussed in conjunction with the recent photometricdata by Reipurth (1978). The spectroscopic orbital elements have beendetermined from 18 double-lined spectra as following: V0equals -5.95 km/s, Kp equals 49.9 km/s, Ks equals47.8 km/s, e equals 0.19. The spectral types of components are estimatedto be G2V and G5V. The primary and secondary components of AI Phe arefound to have masses of 1.1 and 1.15 solar mass, and radii 1.7 and 2.1solar radii, respectively.
Colors, luminosities, and motions of the nearer G-type stars Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1964AJ.....69..570E&db_key=AST
Spectral and Luminosity Classifications and Measurements of the Strength of Cyanogen Absorption for Late-Type Stars from Objective-Prism Spectra. Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1961ApJ...134..809Y&db_key=AST

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Takýmyýldýz:	Zincirli Prenses
Sað Açýklýk:	00^h55^m41.78^s
Yükselim:	+23Â°09'22.2"
Görünürdeki Parlaklýk:	8.037
Uzaklýk:	217.391 parsek
özdevim Sað Açýklýk:	-1
özdevim Yükselim:	3.8
B-T magnitude:	9.384
V-T magnitude:	8.149

Kataloglar ve belirtme:

Özgün isimleri	(Edit)
HD 1989	HD 5361
TYCHO-2 2000	TYC 1739-2137-1
USNO-A2.0	USNO-A2 1125-00327180
HIP	HIP 4344

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