目的探讨H3.3G34W、p63及SATB2在骨巨细胞瘤(giant cell tumor of bone,GCTB)中的表达情况及其联合应用对GCTB的诊断作用和价值。方法收集西安交通大学附属红会医院病理科2020年至2022年诊断的54例GCTB、83例非骨巨细胞瘤(non-giant cel...目的探讨H3.3G34W、p63及SATB2在骨巨细胞瘤(giant cell tumor of bone,GCTB)中的表达情况及其联合应用对GCTB的诊断作用和价值。方法收集西安交通大学附属红会医院病理科2020年至2022年诊断的54例GCTB、83例非骨巨细胞瘤(non-giant cell tumor of bone,NGCTB)(包含14例动脉瘤样骨囊肿、16例软骨母细胞瘤和53例非骨化性纤维瘤)患者的样本和病历资料,采用免疫组织化学EliVision法检测H3.3G34W、p63及SATB2的表达情况。通过χ^(2)检验判断H3.3G34W、p63及SATB2的阳性率在各组间是否存在统计学差异;通过Logistic回归分析建立包括H3.3G34W、p63及SATB2的联合诊断模型,通过受试者工作特征(ROC)曲线分析评价模型的诊断价值。结果H3.3G34W、p63及SATB2在GCTB组中阳性率分别为81.5%、90.7%、92.6%;在NGCTB组中阳性率分别为2.4%、28.9%、62.7%。与NGCTB组相比,GCTB组患者年龄显著较大[(41.222±14.849)vs.(16.566±9.439);P<0.001],女性比男性患病率更高(51.9%vs.48.1%,P<0.001)。与NGCTB组相比,GCTB组中H3.3G34W(81.5%vs.2.4%,P<0.001);p63(90.7%vs.28.9%,P<0.001)和SATB2(92.6%vs.62.7%,P<0.001)的阳性率更高。单因素Logistic回归分析构建单因素预测模型,同时行ROC曲线分析,表明年龄(AUC=92.9%,P<0.001)、性别(AUC=64.5%,P=0.004)、H3.3G34W阳性率(AUC=89.5%,P<0.001)、p63阳性率(AUC=80.9%,P<0.001)、SATB2阳性率(AUC=65.0%,P=0.003)是GCTB诊断的独立预测因素。进一步的多因素Logistic回归分析构建混合预测模型,并行ROC曲线分析,发现混合模型展现出比单因素模型更好的预测价值(AUC=98.4%,P<0.001)。结论H3.3G34W、p63及SATB2是有效诊断GCTB的分子标记物,且三者联合应用更能提高GCTB的诊断预测效能。展开更多
目的探究在Halcyon直线加速器上使用调强适形放射治疗(IMRT)和容积旋转调强放射治疗(VMAT)进行乳腺癌保乳术后放射治疗的临床应用。方法选择乳腺癌保乳术后放射治疗患者25例,年龄36~61岁,平均年龄50.9岁;左侧乳腺癌15例,右侧乳腺癌10例...目的探究在Halcyon直线加速器上使用调强适形放射治疗(IMRT)和容积旋转调强放射治疗(VMAT)进行乳腺癌保乳术后放射治疗的临床应用。方法选择乳腺癌保乳术后放射治疗患者25例,年龄36~61岁,平均年龄50.9岁;左侧乳腺癌15例,右侧乳腺癌10例;肿瘤分期均为T1~T2、N0、M0。计划设计均在Eclipse计划系统上,每例患者分别采用IMRT和VMAT进行计划设计。对两类计划的主要剂量学参数、剂量分布、γ通过率和照射时间进行比较。结果所有计划均可临床使用,两组计划靶区D_(95%)、平均剂量D_(mean)差异较小(P>0.05),靶区均匀性指数(HI)(IMRT组0.06±0.01 vs VMAT组0.06±0.01),差异无统计学意义(P>0.05),适形性指数(CI)(IMRT组0.85±0.03 vs VMAT组0.92±0.02),差异有统计学意义(P<0.05)。IMRT组患侧肺V_(5)、V_(20)和平均剂量,心脏平均剂量,健侧肺V_(5)均低于VMAT组,差异具有统计学意义[患侧肺V_(5)(41.36±2.04)%vs(47.58±2.42)%、患侧肺V_(20)(15.04±2.90)%vs(16.35±1.97)%、患侧肺平均剂量(886.32±79.41)cGy vs(993.49±50.14)cGy、心脏平均剂量(209.23±98.12)cGy vs(277.60±83.18)cGy、健侧肺V_(5)(2.10±1.35)%vs(14.06±8.62)%。P<0.05]。VMAT组γ通过率优于IMRT组,差异有统计学意义[3 mm/3%(99.72±0.20)%vs(99.38±0.37)%;2 mm/2%(97.22±1.05)%vs(96.99±0.91)%。P<0.05]。IMRT组照射时间(2.08±0.27)min,VMAT组照射时间(0.87±0.04)min,VMAT组节省超过55%照射时间,差异有统计学意义(P<0.05)。结论使用Halcyon直线加速器进行保乳术后放射治疗,IMRT计划和VMAT计划均能满足临床治疗需求,采用VMAT技术会提高靶区的剂量分布,明显提高计划执行效率。展开更多
The growth plate(GP)is a crucial tissue involved in skeleton development via endochondral ossification(EO).The bone organoid is a potential research model capable of simulating the physiological function,spatial struc...The growth plate(GP)is a crucial tissue involved in skeleton development via endochondral ossification(EO).The bone organoid is a potential research model capable of simulating the physiological function,spatial structure,and intercellular communication of native GPs.However,mimicking the EO process remains a key challenge for bone organoid research.To simulate this orderly mineralization process,we designed an in vitro sh Ca_(v)3.3 ATDC5-loaded gelatin methacryloyl(Gel MA)hydrogel model and evaluated its bioprintability for future organoid construction.In this paper,we report the first demonstration that the T-type voltage-dependent calcium channel(T-VDCC)subtype Ca_(v)3.3 is dominantly expressed in chondrocytes and is negatively correlated with the hypertrophic differentiation of chondrocytes during the EO process.Furthermore,Ca_(v)3.3 knockdown chondrocytes loaded with the Gel MA hydrogel successfully captured the EO process and provide a bioink capable of constructing layered and orderly mineralized GP organoids in the future.The results of this study could therefore provide a potential target for regulating the EO process and a novel strategy for simulating it in bone organoids.展开更多
We conducted the first light curve study of the binary star EL Tuc within the Binary Systems of South and North project's framework.The photometric observations were made using standard multiband BVR_cI_c filters ...We conducted the first light curve study of the binary star EL Tuc within the Binary Systems of South and North project's framework.The photometric observations were made using standard multiband BVR_cI_c filters at an observatory in Argentina.We presented a new ephemeris for EL Tuc and a linear fit to the O–C diagram,utilizing our extracted times of minima and additional literature.We employed the PHysics Of Eclipsing BinariEs Python code and the Markov chain Monte Carlo approach for the system's light curve analysis.The target system's light curve solution required a cold starspot on the hotter component.We conclude that EL Tuc is a total contact binary system with a low mass ratio of q=0.172±0.002,an orbital inclination of i=83°.74±0°.40,and a fillout factor of f=53.7%±1.6%.We used the P-a relationship and the Gaia Data Release 3 parallax method to determine the absolute parameters of EL Tuc to compare the precision of our results.This system was classified as W-type based on the mass and effective temperature of the companion stars.The positions of the systems were depicted on the M-L,M-R,T-M,and q-Lratiodiagrams.The relationship between the spectroscopic and photometric mass ratios of binaries was discussed.展开更多
1) The observation by Allais of the precession of pendulums from 1954 to 1960 highlighted regularities of astral origin an in-depth analysis of which showed that, apparently, no classical phenomenon can explain them. ...1) The observation by Allais of the precession of pendulums from 1954 to 1960 highlighted regularities of astral origin an in-depth analysis of which showed that, apparently, no classical phenomenon can explain them. These regularities were diurnal waves whose periods are characteristic of astral influence (the main ones being 24 h and 24 h 50 min), annual and semi-annual components, and a multi-annual component of approximately 6 years, an influence of Jupiter being a very good candidate to explain it. 2) Allais had experimentally established that all these astral influences were expressed globally on the pendulum by an action tending to call back its plane of oscillation towards a direction variable in time, and which ovalized its trajectory. In 2019 the observation of 2 pendulums in Horodnic (Romania), thanks to the use of an automatic alidade, made it possible to identify the main mechanism that, very probably, acted on the pendulum to achieve this result. This perturbation model, called “linear anisotropy”, is characterized by its “coefficient of anisotropy” η, and by the azimuth of its “direction of anisotropy”. The composition of 2 linear anisotropies is always a linear anisotropy. 3) In the search for the phenomena which could be at the origin of all what precedes, the fact that they must create an ovalization immediately eliminates some of them. 4) We have calculated the values of η corresponding to the 24 h and 24 h 50 min waves both for the observations in Horodnic and the Allais observations. The order of magnitude (some 10−7) is effectively the same in both cases. 5) Mathematically, the regularities discovered may result of a new force field but also, as Allais proposes, from the creation, under the astral influences, of a local anisotropy of the medium in which the pendulum oscillates. In the first case the length of the pendulum is involved, in the second one not. The data available do not make it possible to decide. 6) The joint exploitation, in mechanics and optics, of Allais observations and of observations by other experimenters provides additional information: a) Allais, and after him several other scientists, discovered also marked anomalies in the precession of pendulums during certain eclipses, and maybe certain other syzygies. For the few eclipses for which both something was observed and sufficient data were available (one of them being a lunar eclipse for which nothing had been published until now), it was always the above perturbation model which acted on the pendulum, but sometimes with quite exceptional magnitude. b) There are quite possible links with optics. During the observation campaign of August 1958, which had implemented both two pendulums and an optical device, all the 24 h 50 min waves were almost in phase. In the precession of the Allais pendulum, in Miller’s interferometric observations in Mont Wilson, and in Esclangon’s observations in Strasbourg, a same peculiarity is found: the extrema of the annual influence are at the equinoxes, not at the solstices.展开更多
The light curve analyses and orbital period variations for two contact binary stars,LS Del and V997 Cyg,are presented in this work which was conducted in the frame of the Binary Systems of South and North project Grou...The light curve analyses and orbital period variations for two contact binary stars,LS Del and V997 Cyg,are presented in this work which was conducted in the frame of the Binary Systems of South and North project Ground-based photometric observations were performed at two observatories in France.We used the Transiting Exoplanet Survey Satellite(TESS)data for extracting times of minima and light curve analysis of the targe systems.The O-C diagram for both systems displays a parabolic trend.LS Del and V997 Cyg’s orbital periods are increasing at rates of dP/dt=7.20×10^(-08)days yr^(-1)and dP/dt=2.54×10^(-08)days yr^(-1),respectively Therefore,it can be concluded that mass is being transferred from the less massive star to the more massive component with a rate of dM/dt=-1.96×10^(-7)M_(⊙)yr^(-1)for the LS Del system,and dM/dt=-3.83×10^(-7)M_(⊙)yr-1for V997 Cyg.The parameters of a third possible object in the system are also considered.The PHysics Of Eclipsing BinariEs Python code was used to analyze the light curves.The light curve solutions needed a cold starspot due to the asymmetry in the LS Del system’s light curve maxima.The mass ratio fill-out factor,and star temperature all indicate that both systems are contact binary types in this investigation.Two methods were applied to estimate the absolute parameters of the systems:one method relied on the parallax of Gaia DR3,and the other used a P-M relationship.The positions of the systems are also depicted on the M-L,M-R q-L_(ratio),and logM_(tot)-logJ_(0)diagrams.We recommend that further observations and investigations be done on the existence of a fourth body in this system.展开更多
V0405 Dra is a W UMa-type binary star.Based on the TESS data,we have conducted an orbital period study and performed a light curve analysis for the system.The orbital period study reveals that the O-C curve for V0405 ...V0405 Dra is a W UMa-type binary star.Based on the TESS data,we have conducted an orbital period study and performed a light curve analysis for the system.The orbital period study reveals that the O-C curve for V0405 Dra exhibits secular decrease at an extremely high rate of d P/dt=-2.71×10^(-6)day year^(-1),along with periodic variations characterized by an amplitude of A_(3)=0.0032 day and a period of P_(3)=1.413 years.The orbital periodic change is possibly due to the light-travel time effect resulting from an additional third body in the system,for which we estimate a minimum mass of M_(3)=0.77M_(⊙).By employing the 2013 version of the Wilson-Devinney(W-D)method to synthesize a light curve,we derived photometric solutions indicating that V0405 Dra is a new deep(f=68.7%)and low-mass ratio(q=0.175)contact binary.The fast decrease in its orbital period is likely caused by mass transfer from the more massive primary star to the less massive secondary star,or due to angular momentum loss.With further mass transfer and loss of angular momentum,the binary will gradually evolve into a tighter contact configuration,eventually leading to a merger into a single star,following the evolutionary paths suggested for such deep and low mass ratio contact binaries.展开更多
In this paper,new light curves(LCs) of contact eclipsing binary(CEB) systems LX Lyn and V0853 Aur are presented and analyzed by using the 2015 version of the Wilson-Devinney(W-D) code.In order to explain their asymmet...In this paper,new light curves(LCs) of contact eclipsing binary(CEB) systems LX Lyn and V0853 Aur are presented and analyzed by using the 2015 version of the Wilson-Devinney(W-D) code.In order to explain their asymmetric LCs,cool starspots on the components were employed.It is suggested that their fill-out degrees are f=12.0%(LX Lyn) and f=26.3%(V0853 Aur).At the same time,we found that LX Lyn is a W-type eclipsing binary(EB) with an orbital inclination of i=84°.88 and a mass ratio of q=2.31.V0853 Aur is also a W-type CEB with a mass ratio of q=2.77 and an orbital inclination of i= 79°.26.Based on all available times of light minimum,their orbital period changes are studied by using the O-C method.The O-C diagram of LX Lyn reveals a cyclic oscillation with a period of about 14.84 yr and an amplitude of 0.0019 days,which can be explained by the light-travel time effect(LTTE) due to the presence of a third body with a minimum mass of0.06M_⊙.For V0853 Aur,it is discovered that the O-C diagram of the system also shows a cyclic oscillation with a period of 9.64 yr and an amplitude of 0.03365 days.The cyclic oscillation of V0853 Aur can be attributed to the LTTE by means of a third body with a mass no less than 3.77M_⊙.The third body may play an important role in the formation and evolution of these systems.展开更多
文摘目的探讨H3.3G34W、p63及SATB2在骨巨细胞瘤(giant cell tumor of bone,GCTB)中的表达情况及其联合应用对GCTB的诊断作用和价值。方法收集西安交通大学附属红会医院病理科2020年至2022年诊断的54例GCTB、83例非骨巨细胞瘤(non-giant cell tumor of bone,NGCTB)(包含14例动脉瘤样骨囊肿、16例软骨母细胞瘤和53例非骨化性纤维瘤)患者的样本和病历资料,采用免疫组织化学EliVision法检测H3.3G34W、p63及SATB2的表达情况。通过χ^(2)检验判断H3.3G34W、p63及SATB2的阳性率在各组间是否存在统计学差异;通过Logistic回归分析建立包括H3.3G34W、p63及SATB2的联合诊断模型,通过受试者工作特征(ROC)曲线分析评价模型的诊断价值。结果H3.3G34W、p63及SATB2在GCTB组中阳性率分别为81.5%、90.7%、92.6%;在NGCTB组中阳性率分别为2.4%、28.9%、62.7%。与NGCTB组相比,GCTB组患者年龄显著较大[(41.222±14.849)vs.(16.566±9.439);P<0.001],女性比男性患病率更高(51.9%vs.48.1%,P<0.001)。与NGCTB组相比,GCTB组中H3.3G34W(81.5%vs.2.4%,P<0.001);p63(90.7%vs.28.9%,P<0.001)和SATB2(92.6%vs.62.7%,P<0.001)的阳性率更高。单因素Logistic回归分析构建单因素预测模型,同时行ROC曲线分析,表明年龄(AUC=92.9%,P<0.001)、性别(AUC=64.5%,P=0.004)、H3.3G34W阳性率(AUC=89.5%,P<0.001)、p63阳性率(AUC=80.9%,P<0.001)、SATB2阳性率(AUC=65.0%,P=0.003)是GCTB诊断的独立预测因素。进一步的多因素Logistic回归分析构建混合预测模型,并行ROC曲线分析,发现混合模型展现出比单因素模型更好的预测价值(AUC=98.4%,P<0.001)。结论H3.3G34W、p63及SATB2是有效诊断GCTB的分子标记物,且三者联合应用更能提高GCTB的诊断预测效能。
文摘目的探究在Halcyon直线加速器上使用调强适形放射治疗(IMRT)和容积旋转调强放射治疗(VMAT)进行乳腺癌保乳术后放射治疗的临床应用。方法选择乳腺癌保乳术后放射治疗患者25例,年龄36~61岁,平均年龄50.9岁;左侧乳腺癌15例,右侧乳腺癌10例;肿瘤分期均为T1~T2、N0、M0。计划设计均在Eclipse计划系统上,每例患者分别采用IMRT和VMAT进行计划设计。对两类计划的主要剂量学参数、剂量分布、γ通过率和照射时间进行比较。结果所有计划均可临床使用,两组计划靶区D_(95%)、平均剂量D_(mean)差异较小(P>0.05),靶区均匀性指数(HI)(IMRT组0.06±0.01 vs VMAT组0.06±0.01),差异无统计学意义(P>0.05),适形性指数(CI)(IMRT组0.85±0.03 vs VMAT组0.92±0.02),差异有统计学意义(P<0.05)。IMRT组患侧肺V_(5)、V_(20)和平均剂量,心脏平均剂量,健侧肺V_(5)均低于VMAT组,差异具有统计学意义[患侧肺V_(5)(41.36±2.04)%vs(47.58±2.42)%、患侧肺V_(20)(15.04±2.90)%vs(16.35±1.97)%、患侧肺平均剂量(886.32±79.41)cGy vs(993.49±50.14)cGy、心脏平均剂量(209.23±98.12)cGy vs(277.60±83.18)cGy、健侧肺V_(5)(2.10±1.35)%vs(14.06±8.62)%。P<0.05]。VMAT组γ通过率优于IMRT组,差异有统计学意义[3 mm/3%(99.72±0.20)%vs(99.38±0.37)%;2 mm/2%(97.22±1.05)%vs(96.99±0.91)%。P<0.05]。IMRT组照射时间(2.08±0.27)min,VMAT组照射时间(0.87±0.04)min,VMAT组节省超过55%照射时间,差异有统计学意义(P<0.05)。结论使用Halcyon直线加速器进行保乳术后放射治疗,IMRT计划和VMAT计划均能满足临床治疗需求,采用VMAT技术会提高靶区的剂量分布,明显提高计划执行效率。
基金supported by the National Natural Science Foundation of China(No.31800784)the Chongqing Key Laboratory of Precision Medicine in Joint Surgery(No.425Z2138)+2 种基金the Chongqing Excellent Scientist Project(No.425Z2W21)the Chongqing Natural Science Foundation General Project(No.cstc2021jcyjmsxm X0135)the Chongqing Postdoctoral Research Project Special Fund(No.2021XM3033)。
文摘The growth plate(GP)is a crucial tissue involved in skeleton development via endochondral ossification(EO).The bone organoid is a potential research model capable of simulating the physiological function,spatial structure,and intercellular communication of native GPs.However,mimicking the EO process remains a key challenge for bone organoid research.To simulate this orderly mineralization process,we designed an in vitro sh Ca_(v)3.3 ATDC5-loaded gelatin methacryloyl(Gel MA)hydrogel model and evaluated its bioprintability for future organoid construction.In this paper,we report the first demonstration that the T-type voltage-dependent calcium channel(T-VDCC)subtype Ca_(v)3.3 is dominantly expressed in chondrocytes and is negatively correlated with the hypertrophic differentiation of chondrocytes during the EO process.Furthermore,Ca_(v)3.3 knockdown chondrocytes loaded with the Gel MA hydrogel successfully captured the EO process and provide a bioink capable of constructing layered and orderly mineralized GP organoids in the future.The results of this study could therefore provide a potential target for regulating the EO process and a novel strategy for simulating it in bone organoids.
文摘We conducted the first light curve study of the binary star EL Tuc within the Binary Systems of South and North project's framework.The photometric observations were made using standard multiband BVR_cI_c filters at an observatory in Argentina.We presented a new ephemeris for EL Tuc and a linear fit to the O–C diagram,utilizing our extracted times of minima and additional literature.We employed the PHysics Of Eclipsing BinariEs Python code and the Markov chain Monte Carlo approach for the system's light curve analysis.The target system's light curve solution required a cold starspot on the hotter component.We conclude that EL Tuc is a total contact binary system with a low mass ratio of q=0.172±0.002,an orbital inclination of i=83°.74±0°.40,and a fillout factor of f=53.7%±1.6%.We used the P-a relationship and the Gaia Data Release 3 parallax method to determine the absolute parameters of EL Tuc to compare the precision of our results.This system was classified as W-type based on the mass and effective temperature of the companion stars.The positions of the systems were depicted on the M-L,M-R,T-M,and q-Lratiodiagrams.The relationship between the spectroscopic and photometric mass ratios of binaries was discussed.
文摘1) The observation by Allais of the precession of pendulums from 1954 to 1960 highlighted regularities of astral origin an in-depth analysis of which showed that, apparently, no classical phenomenon can explain them. These regularities were diurnal waves whose periods are characteristic of astral influence (the main ones being 24 h and 24 h 50 min), annual and semi-annual components, and a multi-annual component of approximately 6 years, an influence of Jupiter being a very good candidate to explain it. 2) Allais had experimentally established that all these astral influences were expressed globally on the pendulum by an action tending to call back its plane of oscillation towards a direction variable in time, and which ovalized its trajectory. In 2019 the observation of 2 pendulums in Horodnic (Romania), thanks to the use of an automatic alidade, made it possible to identify the main mechanism that, very probably, acted on the pendulum to achieve this result. This perturbation model, called “linear anisotropy”, is characterized by its “coefficient of anisotropy” η, and by the azimuth of its “direction of anisotropy”. The composition of 2 linear anisotropies is always a linear anisotropy. 3) In the search for the phenomena which could be at the origin of all what precedes, the fact that they must create an ovalization immediately eliminates some of them. 4) We have calculated the values of η corresponding to the 24 h and 24 h 50 min waves both for the observations in Horodnic and the Allais observations. The order of magnitude (some 10−7) is effectively the same in both cases. 5) Mathematically, the regularities discovered may result of a new force field but also, as Allais proposes, from the creation, under the astral influences, of a local anisotropy of the medium in which the pendulum oscillates. In the first case the length of the pendulum is involved, in the second one not. The data available do not make it possible to decide. 6) The joint exploitation, in mechanics and optics, of Allais observations and of observations by other experimenters provides additional information: a) Allais, and after him several other scientists, discovered also marked anomalies in the precession of pendulums during certain eclipses, and maybe certain other syzygies. For the few eclipses for which both something was observed and sufficient data were available (one of them being a lunar eclipse for which nothing had been published until now), it was always the above perturbation model which acted on the pendulum, but sometimes with quite exceptional magnitude. b) There are quite possible links with optics. During the observation campaign of August 1958, which had implemented both two pendulums and an optical device, all the 24 h 50 min waves were almost in phase. In the precession of the Allais pendulum, in Miller’s interferometric observations in Mont Wilson, and in Esclangon’s observations in Strasbourg, a same peculiarity is found: the extrema of the annual influence are at the equinoxes, not at the solstices.
基金project was supported by the Scientific Research Projects Coordination Unit of Erciyes University(project number FBA-2022-11737)the TESS mission is provided by the NASA Explorer Program。
文摘The light curve analyses and orbital period variations for two contact binary stars,LS Del and V997 Cyg,are presented in this work which was conducted in the frame of the Binary Systems of South and North project Ground-based photometric observations were performed at two observatories in France.We used the Transiting Exoplanet Survey Satellite(TESS)data for extracting times of minima and light curve analysis of the targe systems.The O-C diagram for both systems displays a parabolic trend.LS Del and V997 Cyg’s orbital periods are increasing at rates of dP/dt=7.20×10^(-08)days yr^(-1)and dP/dt=2.54×10^(-08)days yr^(-1),respectively Therefore,it can be concluded that mass is being transferred from the less massive star to the more massive component with a rate of dM/dt=-1.96×10^(-7)M_(⊙)yr^(-1)for the LS Del system,and dM/dt=-3.83×10^(-7)M_(⊙)yr-1for V997 Cyg.The parameters of a third possible object in the system are also considered.The PHysics Of Eclipsing BinariEs Python code was used to analyze the light curves.The light curve solutions needed a cold starspot due to the asymmetry in the LS Del system’s light curve maxima.The mass ratio fill-out factor,and star temperature all indicate that both systems are contact binary types in this investigation.Two methods were applied to estimate the absolute parameters of the systems:one method relied on the parallax of Gaia DR3,and the other used a P-M relationship.The positions of the systems are also depicted on the M-L,M-R q-L_(ratio),and logM_(tot)-logJ_(0)diagrams.We recommend that further observations and investigations be done on the existence of a fourth body in this system.
基金supported by the Joint Research Fund in Astronomy(grant No.U1631108)under a cooperative agreement between the National Natural Science Foundation of China(NSFC)the Chinese Academy of Sciences(CAS)the Chinese National Natural Science Foundation of China(NSFC,grant No.12103030)。
文摘V0405 Dra is a W UMa-type binary star.Based on the TESS data,we have conducted an orbital period study and performed a light curve analysis for the system.The orbital period study reveals that the O-C curve for V0405 Dra exhibits secular decrease at an extremely high rate of d P/dt=-2.71×10^(-6)day year^(-1),along with periodic variations characterized by an amplitude of A_(3)=0.0032 day and a period of P_(3)=1.413 years.The orbital periodic change is possibly due to the light-travel time effect resulting from an additional third body in the system,for which we estimate a minimum mass of M_(3)=0.77M_(⊙).By employing the 2013 version of the Wilson-Devinney(W-D)method to synthesize a light curve,we derived photometric solutions indicating that V0405 Dra is a new deep(f=68.7%)and low-mass ratio(q=0.175)contact binary.The fast decrease in its orbital period is likely caused by mass transfer from the more massive primary star to the less massive secondary star,or due to angular momentum loss.With further mass transfer and loss of angular momentum,the binary will gradually evolve into a tighter contact configuration,eventually leading to a merger into a single star,following the evolutionary paths suggested for such deep and low mass ratio contact binaries.
基金partly supported by the Joint Research Fund in Astronomy (grant Nos. U1931101, 42364001) under cooperative agreement between the National Natural Science Foundation of China (NSFC) and Chinese Academy of Sciences (CAS)the National Natural Science Foundation of China (NSFC, Grant No. 11933008)+3 种基金the Guizhou Provincial Science and Technology Foundation (grant Nos.[2020]1Y017, ZK[2022]322)the Foundation of Education Bureau of Guizhou Province,China (grant No. KY (2020) 003)partially supported by the Open Project Program of the CAS Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciencesthe TESS team for its support。
文摘In this paper,new light curves(LCs) of contact eclipsing binary(CEB) systems LX Lyn and V0853 Aur are presented and analyzed by using the 2015 version of the Wilson-Devinney(W-D) code.In order to explain their asymmetric LCs,cool starspots on the components were employed.It is suggested that their fill-out degrees are f=12.0%(LX Lyn) and f=26.3%(V0853 Aur).At the same time,we found that LX Lyn is a W-type eclipsing binary(EB) with an orbital inclination of i=84°.88 and a mass ratio of q=2.31.V0853 Aur is also a W-type CEB with a mass ratio of q=2.77 and an orbital inclination of i= 79°.26.Based on all available times of light minimum,their orbital period changes are studied by using the O-C method.The O-C diagram of LX Lyn reveals a cyclic oscillation with a period of about 14.84 yr and an amplitude of 0.0019 days,which can be explained by the light-travel time effect(LTTE) due to the presence of a third body with a minimum mass of0.06M_⊙.For V0853 Aur,it is discovered that the O-C diagram of the system also shows a cyclic oscillation with a period of 9.64 yr and an amplitude of 0.03365 days.The cyclic oscillation of V0853 Aur can be attributed to the LTTE by means of a third body with a mass no less than 3.77M_⊙.The third body may play an important role in the formation and evolution of these systems.