Peremennye Zvezdy

Article in PDF
"Peremennye Zvezdy",
vol. 6, N 9 (2006)

ASAS 062726+0111.6: a new Double-mode Cepheid

S. V. Antipin
Sternberg Astronomical Institute and Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia

ISSN 2221–0474

Received:   16.03.2006;   accepted:   16.03.2006
(E-mail for contact:

Star Name: ASAS 062726+0111.6, HD 288719, BD+01 1350, TYC 0133 01103 1
Coordinates (J2000): 06 27 25.25, +01 11 32.5
Variability type: CEP(B);   Limits, System: 10.11-10.37 (V);   Spectrum: G0
Period: (see Remarks) d;   Epoch(max): JD (see Remarks)

According to ASAS-3 data (Pojmanski et al., 2005), HD 288719, listed in the ASAS catalog of variable stars as a fundamental mode Cepheid, is actually a double-mode Cepheid. The phased light curves plotted for the following elements:

HJD(max)=2453753.684+2.26571xE (fundamental mode) and

HJD(max)=2453724.711+1.61404xE (first overtone mode),

are given in the Figure. The period ratio P1/P0=0.712 is typical for beat Cepheids. ROTSE-I observations (NSVS 12488333, NSVS 12496743; Wozniak et al., 2004) are in agreement with the suggested classification and periods. However, I did not use the NSVS data for analysis and period determination because of the short interval and small number of good observations.

Pojmanski, G., Pilecki, B., Szczygiel, D., 2005, Acta Astronomica, 55, 275
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W. et al., 2004, Astron. J., 127, 2436

Light Curve
ASAS 062726+0111.6: a new Double-mode Cepheid
The phased light curves. Top panels: ASAS-3 data folded with the fundamental-mode and the first overtone periods. Bottom panels: the same curves after prewhitening the other oscillation; additionally, the frequency connected with the interaction mode (1/P1+1/P0, P=0.94254 d) has been whitened.

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