B and V photometry and analysis of the eclipsing binary RZ Cas

Riazi, N.; Bagheri, Mahdi; Faghihi, F.

doi:10.1007/bf00658232

Cited by 7 publications

(5 citation statements)

References 6 publications

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“…1973 means winter 1973-1974). Sources are: (1) Chambliss (1976); (2) unpublished data collected at AAO; (3) Nakamura et al (1991); (4) Riazi, Bagheri & Faghihi (1994); (5) Hegedus et al (1996).…”

Section: Pulsational Behaviour Over Timementioning

confidence: 99%

Sct-type pulsations in eclipsing binary systems: RZ Cas

Rodríguez

García²,

Mkrtichian

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present the results of a three‐continent multisite photometric campaign carried out on the Algol‐type eclipsing binary system RZ Cas, in which the primary component has recently been discovered to be a δ Sct‐type pulsator. The present observations include, for the first time, complete simultaneous Strömgren uvby light curves together with a few Crawford Hβ data collected around the orbital phase of the first quadrature. The new observations confirm the pulsational behaviour of the primary component. A detailed photometric analysis, based on these observations, is presented for both binarity and pulsation. The results indicate a semidetached system where the secondary fills its Roche lobe. The appearance of the light curves reveals the presence of the mass stream from the secondary component and a hotspot where this stream impacts on the surface of the primary star. There are also some indications of chromospheric activity in the secondary. On the other hand, the pulsational behaviour out‐of‐primary eclipse can be well described with only one frequency at 64.1935 cd−1 similar to the main peak found by Ohshima et al. The existence of multiperiodicity is not confirmed in our data. Concerning the mode identification, our results indicate non‐radial pulsation in a high radial order (n= 6), with l= 2, |m|= 1, 2 as the most suitable. However, additional effects must be taken into account in the predictions. Moreover, the pulsation amplitude in the u band is larger than in b and v, which is unusual among the δ Sct‐type variables. This can be explained as due to pulsation in a high n value and close to the blue edge of the δ Sct region. On the other hand, the early data of Ohshima et al. have also been analysed and similar results are found concerning the frequency content and pulsational amplitude. Finally, a revision of all the photometric out‐of‐primary‐eclipse data sets available in the literature is made together with some additional unpublished data leading to interesting findings relative to changes taking place in the pulsation amplitudes and frequencies from season to season. Furthermore, multiperiodicity is probably present in some epochs.

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Section: Pulsational Behaviour Over Timementioning

confidence: 99%

Sct-type pulsations in eclipsing binary systems: RZ Cas

Rodríguez

García²,

Mkrtichian

et al. 2004

Monthly Notices of the Royal Astronomical Society

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“…RZ Cas is also a radio source and an X-ray source. See Riazi et al (1994) and Maxted et al (1994) and references therein. CC Cas is the massive O-type binary system with a period P = 3.366 days.…”

mentioning

confidence: 99%

Velocity curve analysis of the spectroscopic binary stars by the non-linear least squares

Karami

Teimoorinia

2007

Astrophys Space Sci

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1 etermining the orbital elements of the binary stars help us to obtain the necessary information such as the mass and the radius of stars which play the important roles during the evolutions of the stellar structures. Analyzing both the light and the radial velocity curves deducing from the photometric and the spectroscopic observations, respectively, yields to derive the orbital parameters. One of the usual methods to analyze the velocity curve is the method of Lehmann-Filhés (Smart 1990). Here we introduce a new method to derive these parameters by the nonlinear regression of the radial velocity-acceleration curves. We test our method for the three double-line spectroscopic binary systems RZ Cas, CC Cas and V1130 Tau which have the following properties.The Algol system RZ Cas is the semi-detached eclipsing binary stars with a period P = 1.195 days. There is a mass transfer between the two components. Some evidences existed for periodicity in the period changes due to apsidal motion. RZ Cas is also a radio source and an X-ray source. See Riazi et al. (1994) and Maxted et al. (1994) and references therein. CC Cas is the massive O-type binary system with a period P = 3.366 days. This system is a detached binary with the two components within the main sequence band. It is an actively interacting system. The system shows a mass loss rate 3 × 10 −7 m ⊙ yr −1 due to the stellar winds. Such mass loss from the system yields to a change in the orbital period by the rate of less than 3 × 10 −6 days per century ). V1130 Tau is a very

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“…Photometric light curves for RZ Cas have been provided by, amongst others, Huffer & Kopal (1951), Huffer (1955), Chambliss (1976), Riazi, Bagheri & Faghihi (1994), Maxted et al (1994), Narusawa, Nakamura & Yamasaki (1994) and Varricatt et al (1998). Some authors have reported a flat primary minimum, indicating eclipse totality (Hegedüs 1989; Nakamura, Narusawa & Kamada 1991; Narusawa et al 1994), but Varricatt et al (1998) have recently confirmed that the eclipse is partial and the orbital inclination is .…”

Section: Rz Cassiopeiaementioning

confidence: 99%

VLA and MERLIN observations of RZ Cassiopeiae

Gunn

Brady

2003

Monthly Notices of the Royal Astronomical Society

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We present radio interferometric observations of the Algol‐type binary system RZ Cassiopeiae made with the VLA and MERLIN arrays at 6 cm over an incomplete orbital cycle of the system (1.195 d). We detected RZ Cas with both instruments. The images were unresolved in both cases, with angular extents comparable to the synthesized beams. The peak flux density in the VLA image was 1.14 mJy beam−1 and in the MERLIN image it was 0.93 mJy beam−1. The derived brightness temperatures are 4.02 × 108 and 4.35 × 108 K and the effective electron energies are 0.347 and 0.346 MeV for the MERLIN and VLA data respectively. The radio light curve shows an interesting modulation centred close to the primary eclipse which seems to correlate with ASCA SIS observations of the system. The results can be interpreted as an emitting region on the outer hemisphere of the cool component aligned along the centroid axis of the binary system.

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B and V photometry and analysis of the eclipsing binary RZ Cas

Cited by 7 publications

References 6 publications

Sct-type pulsations in eclipsing binary systems: RZ Cas

Sct-type pulsations in eclipsing binary systems: RZ Cas

Velocity curve analysis of the spectroscopic binary stars by the non-linear least squares

VLA and MERLIN observations of RZ Cassiopeiae

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