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| 1 | Effect of thermal treatment,ionic strength,and pH on the short-term and long-term coalescence stability of lactoglobulin emulsions显示文摘 | Slavka T Nikolai D D Doroteya S | 2006 | Langmuir2006，22，： | 1 |
| 2 | Degree of tumor regression after preoperative chemo-radiotherapy in locally advanced rectal cancer—Preliminary results显示文摘 | Iglika Mihaylova Vesselina Parvanova Chanita Velikova Galia Kurteva Doroteya Ivanova | 2011 | Reports of Practical Oncology & Radiotherapy2011，，6： | 1 |
| 3 | Observations and light curve solutions of the W UMa binaries V796 Cep,V797 Cep,CSS J015341.9+381641 and NSVS 3853195显示文摘Photometric observations in Sloan g′and i′bands of four W UMa binaries, V796 Cep,V797 Cep, CSS J015341.9+381641 and NSVS 3853195, are presented. Our observations showed that CSS J015404.1+382805 and NSVS 3853195 are the same star. We determined the initial epochs T_0 of all targets and found improved values for the period of NSVS 3853195. The light curve solutions of our data revealed that the components of each target are almost the same in terms of mass, temperature,radius and luminosity. The stellar components are G and K spectral types and undergo partial eclipses.All systems have barely-overcontact configurations and can be classified as H subtype W UMa binaries.We established that the relation between the luminosity ratio l_2/l_1 and mass ratio q of our targets is approximately l_2/l_1 = q^(1.5). | Diana Petrova Kjurkchieva Velimir Angelov Popov Sunay Ibryamov Ibryamov Doroteya Lyubenova Vasileva Nikola Ivanov Petrov | 2017 | Research in Astronomy and Astrophysics2017，17，5： | 0 |
| 4 | Observations and light curve solutions of a selection of middle-contact W UMa binaries显示文摘Photometric observations in Sloan g′and i′ bands of W UMa binaries NSVS 4340949,T-Dra0–00959,GSC 03950–00707,NSVS 4665041,NSVS 4803568,MM Peg,MM Com and NSVS4751449 are presented.The light curve solutions revealed that the components of each target are of G and K spectral types.The binaries of the sample have middle-contact configurations whose fillout factors are within the range 0.2–0.4.The only exception is NSVS 4751449 which is in deeper contact(fillout factor of 0.55).It precisely obeys the relation between mass ratio and fillout factor for deep,low mass ratio overcontact binaries.One of the eclipses of almost all targets(except MM Peg)is an occultation and their photometric mass ratios and solutions could be accepted with confidence.We found that the target components have almost equal temperatures but differ considerably in size and mass.The components of the partially-eclipsed MM Peg have close parameters.Our solutions reveal that NSVS 4340949,T-Dra0–00959,NSVS 4803568 and MM Com are of W subtype while GSC 03950–00707,NSVS 4665041,MM Peg and NSVS 4751449 are of A subtype.This subclassification is well-determined for all totallyeclipsed binaries.The targets confirm the trends in which W-subtype systems have smaller periods and lower temperatures than A subtype binaries. | Diana Petrova Kjurkchieva Velimir Angelov Popov Doroteya Lyubenova Vasileva Nikola Ivanov Petrov | 2018 | Research in Astronomy and Astrophysics2018，18，4： | 0 |
| 5 | Photometric observations and light curve solutions of the W UMa stars NSVS 2244206,NSVS 908513,CSS J004004.7+385531 and VSX J062624.4+570907显示文摘Photometric observations in Sloan g' and i' bands of four W UMa stars,NSVS 2244206,NSVS908513,CSS J004004.7+385531 and VSX J062624.4+570907,are presented.The light curve solutions reveal that all targets have overcontact configurations with fillout factors within 0.15-0.26.Their components are G-K spectral types and are almost in thermal contact.They are also relatively close in size and luminosity:the radius ratios r_2/r_1 are within 0.75-0.90;the luminosity ratios l_2/l_1 are within 0.53-0.63.The results of the light curve solution of CSS J004004.7+385531 imply the weak limb-darkening effect of its primary component and possible presence of additional absorbing features in the system. | Diana Petrova Kiurkchieva Velimir Angelov Popov Doroteya Lyubenova Vasileva Nikola Ivanov Petrov | 2016 | Research in Astronomy and Astrophysics2016，16，9： | 0 |
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