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Absolute parameters and observed flares in the M-type detached eclipsing binary 2MASS J04100497+2931023

Research in Astronomy and Astrophysics 2021年第5期21卷 130-138页

作者： Gang Meng Li-Yun Zhang Qing-Feng Pi Liu Long Xianming L.Han misra prabhakar College of Physics&Guizhou Provincial Key Laboratory of Public Big Data Guizhou UniversityGuiyang 550025China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650011China College of Medicine Guizhou University of Traditional Chinese MedicineGuiyang 550025China Department of Astronomy Beijing Normal UniversityBeijing 100875China Dept.of Physics and Astronomy Butler UniversityIndianapolisIN 46208USA Department of Physics&Astronomy Howard UniversityWashington DC 20059USA

The eclipsing binary 2 MASS J04100497+2931023(J04100497+2931023) is classified its spectral type of M0±2 V on basis of a low-resolution spectral survey by the Large Sky Area Multi-Object Fiber Spectroscopic Telescope(LAMOST). The low-resolution spectra exhibit strong single-peak emission in the Hα line. We obtained the radial velocities of this binary by means of the Cross-Correlation Function method from the LAMOST medium-resolution spectra. Both components of J04100497+2931023 indicate strong emissions in the Hα line. We performed follow-up photometric observations of J04100497+2931023 using the Xinglong 85 cm telescope of National Astronomical Observatories, Chinese Academy of Sciences. We obtained its full light curve in V RI filters. We first determined their absolute parameters from simultaneously radial velocity and light curves by the Wilson-Devinney program. From our new light curves, we detected three flares for the first time, including one convective flare. The amplitudes,durations, energies, and spectral indices of three flares were also determined. J04100497+2931023 was monitored for approximately 29 h, which indicates that the flare rate is 0.1 flare per hour. We conclude that J04100497+2931023 is a low-mass detached eclipsing binary with strong magnetic activity.

关键词： binaries:eclipsing stars:flare star:low-mass stars:J04100497+2931023

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Properties of Flare Events on M Stars from LAMOST Spectral Survey Based on Kepler and TESS Light Curves

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Research in Astronomy and Astrophysics 2023年第5期23卷 1-18页

作者： Gang Meng Li-Yun Zhang Tianhao Su Zilu Yang Xianming LHan prabhakar misra Liu Long Qingfeng Pi Zhongzhong Zhu Linyan Jiang College of Physics&Guizhou Provincial Key Laboratory of Public Big Data Guizhou UniversityGuiyang 550025China Department of Astronomy Beijing Normal UniversityBeijing 100875China Dept.of Physics and Astronomy Butler UniversityIndianapolisIN 46208USA Department of Physics&Astronomy Howard University WashingtonDC 20059USA College of Medicine Guizhou University of Traditional Chinese MedicineGuiyang 550025China Guiyang Institute of Information Science and Technology Guiyang 550025China

A catalog of M stars has been published from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope data release 7(LAMOST DR7).We cross-matched the LAMOST M catalog with Kepler,Kepler 2(K2)and Transiting Exoplanet Survey Satellite(TESS)*** obtained the light curves from the Kepler and TESS *** detected 20,047 flare events from 4053 M stars and calculated their durations,amplitudes,and *** analyzed the distribution of the flare durations and *** distributions of flare duration for Kepler,K2 and TESS peak are at 3–3.5 hr,4–6 hr and 1–1.5 hr,*** may be the result of the different cadences for the three data *** highest regions of the flare energies of Kepler,K2 and TESS are 32–32.5,32–32.5 and31–31.5 erg in Log format,respectively.A linear relationship between flare duration and energy emerges from our *** ratio of flare duration to total observational time is approximately 0.2%–0.3%for the Kepler,K2 and TESS *** occurrence rate of a star with a flare event increases from the M0 to M4 *** also determined the spatial distribution of the flare rate of M stars in the Milky *** seems that the flare rate decreases as the vertical height *** power index of the flare energies is in the region of 1.53–2.32,which is similar to previous result for solar type star(2.0).Further,we examined the relationship between the flare amplitude and chromospheric *** flare activity increases rapidly with the increase in the HαEW at the lower values(less approximately 2?)and it increases slowly at the higher values.

关键词： stars activity-stars flare-stars low-mass

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Collisional Rate Parameters For The 1S4 Energy Level Of Neon 638.3nm And 650.7nm Transitions From The Analyses Of The Time-Dependent Optogalvanic Signals

Collisional Rate Parameters For The 1S4 Energy Level Of Neon...

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第十五届全国原子与分子物理学术会议

作者： Haridass Chandran prabhakar misra Department of Physical Sciences Belfry School Department of Physics&Astronomy Howard University

The time-dependent optogalvanic signals can be represented by a series of exponential functions:

关键词： Optogalvanic Effect(OGE) Monte Carlo Least Squares Fitting Collisional rates

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用印度松节油生产松油的工艺改革

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香料香精化妆品 1981年第Z1期 53-54页

作者： misra Siddiqui Sen 汪雅芬

根据印度松节油和含水硫酸在丙酮介质中发生水合作用的气相色谱数据,确定了印度松节油生产松油(提自 Pinus longifolia)的参数。印度松节油约含20～30%α—蒎烯,10%β—蒎烯,55%δ~3—蒈烯和3～10%长叶烯。一个含有30%α—蒎烯,10%β—... 详细信息

根据印度松节油和含水硫酸在丙酮介质中发生水合作用的气相色谱数据,确定了印度松节油生产松油(提自 Pinus longifolia)的参数。印度松节油约含20～30%α—蒎烯,10%β—蒎烯,55%δ~3—蒈烯和3～10%长叶烯。一个含有30%α—蒎烯,10%β—蒎烯,55%δ~3—蒈烯和5%长叶烯的印度松节油样品已经转化成质量良好的松油。松油的得率是80%,内含有60～65%的醇,以α—松油醇计。此松油具有愉快的香气,可用于调香。松油在世界上用途广泛,许多国家利用生产松油醇的馏份或副产品来生产松油,这些松油醇工业一般以α—蒎烯含量高的松节油(欧州松节油)为起始原料。松油是无色至淡琥珀色液体,有松树香气,是一种除臭剂或消毒剂。它广泛地用于兽医用喷雾剂、油漆、低档香精以及肥皂和洗涤剂加香。其主要成份是叔醇,α—松油醇。还有较少量的仲醇。prabhakar,Nigam,Handa 和 Kelkar 等人对不同地区的印度松节油进行了分析。发现这些油中α—蒎烯含量不高。Nigam 和他的同事在早些时候已通过均化作用把松节油转化成松油。均化是通过丙酮把油和硫酸(40%)溶在一起而进行的。本篇报道改善实验条件和减少丙酮用量,提高丙酮回收率,提高松油得率的新参数。

关键词：松节油硫酸萜类化合物硫化合物松油松油醇南亚印度

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