Period change in GS Gru

Details Period change in GS Gru Period change in GS Gru

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995dssn....8....3r&link_type=abstract

Delta Scuti Star Newsletter, Issue 8, p. 3-5.

Astronomy and Astrophysics

Astronomy

Scientific paper

RS Gru is a high amplitude Delta Scuti type star with dV~= 0.56m and P=0.1470d. Four new times of light maxima were obtained for this star from simultaneous uvby observations carried out in the year 1988 at European Southern Observatory in Chile. In total, twenty-two times of light maxima (from 1952 to 1988, collected from Hoffmeister 1956, Veröff. Sternw. Sonneberg 3, 1; Kinman 1961, Roy. Obs. Bull. 37, 151; Oosterhoff and Walraven 1966, Bull. Astron. Inst. Netherl. 18, 387; McNamara and Feltz 1976, PASP 88, 510; Dean et al. 1977, Mem. R. Astron. Soc. 83, 69; Balona and Martin 1978, MNRAS 184, 1 and us) were used to derive the ephemeris of the light curve of RS Gru by means of the classical O-C method. The least squares fit of a linear ephemeris leads the the following elements: T0=2447464.7136d(+- 0.0010) and P0=0.147011134d (+- 0.000000021). The residuals O-C, in days, with respect to this linear ephemeris are shown in the Figure 1. From this figure it appears that a quadratic fit as T max=T1+P1*E+A*E*E with the following coefficients: T1=2447464.7101d(+- 0.0004) P1=0.147010864d(+- 0.000000022) A=-3.14d(+- 0.24)E-12 fit the data much better than the linear ephemeris. This means that the pulsation period of RS Gru is decreasing at a rate of dP/Pdt= -10.6(+- 0.8)E-8/y.

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