WR Örten çifti CQ cephei'nin fotoelektrik ışık ölçümü
Başlık çevirisi mevcut değil.
- Tez No: 28813
- Danışmanlar: PROF. DR. ÖMÜR GÜLMEN
- Tez Türü: Doktora
- Konular: Astronomi ve Uzay Bilimleri, Astronomy and Space Sciences
- Anahtar Kelimeler: Belirtilmemiş.
- Yıl: 1993
- Dil: Türkçe
- Üniversite: Ege Üniversitesi
- Enstitü: Fen Bilimleri Enstitüsü
- Ana Bilim Dalı: Astronomi ve Uzay Bilimleri Ana Bilim Dalı
- Bilim Dalı: Belirtilmemiş.
- Sayfa Sayısı: 100
Özet
ÖZET CQ Cephei (HD 214419 =BD +56°2818), donemi -1.64 gün olan bir örten değişen dizgesidir. Bir bileşeni bir WN7 yıldızı diğeri ise muhtemelen büyük bir erken tür yıldızdır. Bu örten değişen yıldız Ege Üniversitesi Rasathanesinde fotoelektrik olarak 1991 yılında 19, 1992 yılında ise 11 gece gözlenmiştir. Gözlemler 48 cm lik Cassegrain teleskopla yapılmıştır. Gözlemlerde soğultulmamış EMİ 9781 A fotokatlandıncı tüp ve UBV standard düzeneğine çok yakın olan B,V süzgeçleri kullanılmıştır. Mukayese olarak BD + 56° 2815 ve denet olarak ise BD + 56° 2813 yıldızları seçilmiştir. Gözlem süresi boyunca mukayese yıldızının parlaklığının sabit olduğu bulunmuştur. Her bir renkte toplam 1511 er gözlem noktası elde edilmiştir. Mukayese - değişen olacak şekilde düzenlenen fark parlaklıkların tümü atmosferin sönükleştirme etkisinden kurtarılmıştır ve düzeltilmiş parlaklıklar Çizelge 2.1.1 de verilmiştir. Mukayese, denet ve değişen yıldızların parlaklıkları, standard UBV sistemine dönüştürülmüştür ve Çizelge 2.1.3 ve 2.3.2 de verilmiştir. Gözlemler sırasında yedi baş ve üç yan minimum zamanı elde edilmiştir. Bu baş minimum zamanlarıyla literatürden bulunabilen fotografik ve fotoelektrik minimum zamanlarını birleştirerek, en küçük kareler yöntemiyle aşağıda verilen kuadratik ışık öğeleri hesaplanmıştır: HeI.Min.I J.D. = 24324568.694 + 18.6412481xE - 9.29xl
Özet (Çeviri)
SUMMARY CQ Cephei(HD 214419=BD+56° 2818) is an eclipsing binary system with a period of ~1.64 day. One Component is a WN7 star and the other is probably a massive early type star. This eclipsing binary was observed photoelectrically at Ege University Observatory on 19 nights in 1991 and 12 nights in 1992. The observations were made with the 48 cm Cassegrain reflector. An unrefrigerated EMI 9781A photomultiplier tube and B,V filters which are very close to the standard UBV system were used. BD +56°2815 was selected as comparison and BD 56+° 2813 as check star. The comparison star was found as constant in brightnes during the period of observations. A total of 1511 observational points were obtained in each colour. All the differential magnitudes( in the sense variable minus comparison) were corrected for the atmospheric extinction and the corrected magnitudes were given Table 2.1.1. The magnitudes of comparison, check and variable stars were transferred to standard UBV system and given in Table 2.1.3 and 2.3.2. During the observations 7 primary and 3 secondary times of minima were obtained. Combining these times of primary minima with other photogrophic and photoelectric ones which can be found from the literature, the new quadratic light elements were calculated by the least-squares method as follow: HeI.Min.1 J.D. = 24324568.694 + 18.641248UE - 9.29x10 ^xE2 (2.2.2) ±2 ±2 ±36 The period of system is decreasing with amount of 0.036+0.01 second per year. The light and colour curves are given in Figure 2.3.1. The phases in Table 2.1.1 and Figure 2.3.1 were calculated with following linear light elements: Hel Min J.D= 244485248.423+ 18.64 12299xE (2.2.3) These light elements were obtained from quadratic light elements and may be used in near future. The synthetic light curve technique of Wilson and Devinney(1971) was applied to the system CQ Cephei. The modern version of method devoloped by Wilson(private comm.,1984) was used for our solutions. 73For the solution, 935 observational points in the phases from 0.0 to 0.57 were combined into 29 normal points in V colour. The temperature of WR Component was taken from Conti(1976), Leep(1986), Willis ve WiIson(1979) as equal to 45000 K. The limb-darkening coefficents were taken from Al Naimiy(1977), the gravity darkening exponents from von Zeipel(1924). The bolometric albedos were set to 1.0 for radiative atmospheres. At first, the light curve in V were tried to solve. Then simultaneous solutions were made by combining the V light curve with the radial velocity curve of NTV X 4058 A given by Leung et.al. (1983). The q-search procedure was applied to find the mass ratio of the system. But all the weighted sum of the squared residuals [ W(O-C)2] were found almost the same. The results of the q-search procedure are given in Table 3.2.1 and 3.2.2. According to Massey(1981 ), the mass of WR component should be in the limits of ~2STHq and ~50 Wl0; therefore the mass ratio of the system must be between 0.7 to 1. Then q=0.7 was taken as input value, added to adjustable parameters and final solutions were made with Mode 3. The convergent solutions were obtained with the free parameters by iterating until the corrections on the parameters became smaller than the corresponding probable errors. The mass ratio was found as 0.79±0.01 from solutions of V light curves and 0.81±0.01 from the simultaneous solution of V light and Leung's radial velocity curves. The result are given in Table 3.2.3. The theoretical light and radial velocity curves are shown in Fig 3.2.4(a,b). These curves are fitted the observations well. According to our results, the system CQ Cephei is a contact binary which has a WR component. IUE spectra of CQ Cephei system were also investigated. 40 SWP and 38 LWR spectra taken by IUE were obtained from WILSPA. These spectra have flux numbers versus wavelengths. Firstly, the wavelenghts on the magnetic tapes were corrected by using the equation (2.4.2) for the motions of earth and IUE. Then the flux numbers were transferred to absolute fluxes by using the equation (2.4.3) and corrected for interstellar absorbtion with (2.4.6). Some samples of spectra which have been corrected for radial velocity and interstellar absorbtion are shown in Fig. 3.1.1(a,b,c,d). The average fluxes in different wavelength regions were calculated to investigate the correlation between the energy distribution and certain orbital phase. The light curves derived from the continuous spectra are 74shown in Fig. 3.1.2(a,b) for the wavelengths 1300, 1600, 1850, 2450, 2650 and 3000 A. In general, bigger the amplitudes smaller the wavelenghts. The phase dependence of the total fluxes for the wavelenght region of each 100 A are shown in Fig. 3.1.3(a,b). In the region XX 1200-1300 and 1300-1400 A the depths of secondary minimum are bigger than that of primary. At the other hand, the phase dependence of total fluxes calculated from the wider regions of the spectrum (XX 1200-1900, 1300-1900, 1400-1900, 1500-1900 etc.) are shown in Fig. 3.1.4. In the first two regions the secondary minimum are deeper than that of primary; while in the others, primary minima are deeper than the secondary. Therefore, it can be said that CQ Cep has an flux excess in the ultraviolet. Stickland et.al. (1984) have also stated that the the system CQ Cep has an abnormal flux distribution at the wavelengths smaller than 1800 A. The samples of light curves which have been obtained from the spectra taken with LWR camera are shown in Fig 3.1.5(a,b). In these curves, there are no anomalies. The inclination of the ascending and descending branches are similar to that of B,V light curves. In the secondary maximum more lights come from the system. This situation is also seen in B,V curves. 75
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