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TWO-DIMENSIONAL REAL-TIME VELOCITY FIELD ON SOLAR PROMINENCE

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Chinese Science Bulletin 1988年第24期33卷 2046-2049页

作者：张洪起艾国祥韩峰孔繁熙刘克宁曹鸿岩 Beijing Observatory Academia Sinica Beijing Observatory Academia Sinica a visiting astronomer fromrmqi Astronomical StationAcademia Silica.

The study of the prominence velocity field is important for understanding the formation and evolution. People have found the macroscopic flow of cool material moving along the prominence. Engvold reported the downward... 详细信息

关键词： solar prominence solar limb Dopplergram

Relativistic Corrections to the Maxwellian Distribution for Astrophysical and Fusion Plasmas

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Journal of Applied Mathematics and Physics 2023年第8期11卷 2414-2428页

作者： Amaury de Kertanguy Retired astronomer Paris France

We present calculations and improvement inspired by the work of Lorenzo Zaninetti, published in 2020, it concerns a problem whose origin dates back 1911 with so called Maxwell-Jüttner distribution these lies on the Lorentz factor , with . This work uses powerful modern software for a reconstruction of Zaninetti work, which computes with special functions, these are included in the Mathematica software, as by instance Bessel and Meijer G-functions ready to manipulate. A progress is made, it is possible to perform an integral that is not computed in Zaninetti paper. This author connects the correct relativistic probability law: the Maxwell-Jüttner to the synchrotron emissivity with a magnetic B field, this work generalize these results, using the linear Stark effect and deals with an electric field E.

关键词： Maxwell-Jüttner Distribution Relativity Modification to Maxwell Law Lorentz Factor Linear Stark Effect Plasma Physics

Modification of Constants in the Schrödinger Equation Giving Access to Neutrino Behavior

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Journal of Applied Mathematics and Physics 2024年第11期12卷 3860-3868页

作者： Amaury de Kertanguy Retired astronomer Paris France

The paper deals with a study of the Schrödinger equation with an original approach. Recalling the well-known relation: p→iℏΔr. It considers this equation for which the kinetic factor is EKin=p22M=−ℏ22MΔr2. Making the kinetic factor EKin=−Δr2can be obtained if one defines a mass M=ℏ22, very small and close to the accepted mass of a neutrino νe. The Schrödinger equation reduces to: −Δr2ϕ(r)=Eϕ(r). The energy E is that given by Dirac (1927), (c being the light velocity), with his remark that two solutions exist E=±p2c2+M2c4. The body of this paper shows all solutions obtained when solving the simplified Schrödinger equation.

关键词： Schrödinger Equation Planck Constant Particle Physics Neutrino Physics

DISTRIBUTION OF QSOs AROUND NGC 1097

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Science China Mathematics 1983年第4期 418-427页

作者：何香涛,R.D.WOLSTENCROFT visiting astronomer from the Department of Astronomy Beijing Normal University China Royal Observatory Blackford Hill Edinburgh Scotland Institute of Astronomy University of Hawaii 2680 Woodlawn Drive Honolulu Hawaii 96822 U.S.A.

The UK 1.2 m Shmidt telescope was used to obtain two objective-prism plates and one direct plate of the area around NGC 1097, centred on 2h44.m2. --30°29′.0 （1950.0） 37 quasar candidates are found within a 9 square degree region. Adding 6 QSOs found before, the total number of QSOs found in this area is *** have analysed the distribution of the QSOs around NGC 1097. The preliminary results are as follows: （ⅰ） The surface density of QSOs is very high near NGC 1097 and decreases with distance, from 15.2 to 2.0 per square degree. The average density is about 4.8 per square degree, （ⅱ） There is an obvious correlation between the jets and the QSOs. （ⅲ） It is difficult to explain the distribution of the QSOs by accidental probability or other reasons. This is a good evidence to suggest that the redshifts are non-cosmological.

关键词： NGC QS DISTRIBUTION OF QSOs AROUND NGC 1097

Absolute parameters of young stars:PU Pup

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Research in Astronomy and Astrophysics 2021年第10期21卷 151-163页

作者： Ahmet Erdem Derya Surgit Timothy S.Banks Burcu Ozkardes Edwin Budding Canakkale Onsekiz Mart University Astrophysics Research Center and Ulupinar ObservatoryTR-17100CanakkaleTurkey Department of Physics Faculty of Arts and SciencesCanakkale Onsekiz Mart UniversityTerzioglu KampusuTR-17100CanakkaleTurkey Department of Space Sciences and Technologies Faculty of Arts and SciencesCanakkale Onsekiz Mart UniversityTerzioglu KampusuTR-17100CanakkaleTurkey Data Science Nielsen200 W JacksonChicagoIL 60606USA Physics&Astronomy Harper College1200 W Algonquin RdPalatineIL 60067USA visiting astronomer Mt.John ObservatoryUniversity of CanterburyPrivate Bag 4800Christchurch 8140NZ Carter Observatory Wellington 6012New Zealand School of Chemical&Physical Sciences Victoria University of WellingtonWellington 6012New Zealand Variable Stars South RASNZPO Box 3181WellingtonNew Zealand

We present combined photometric and spectroscopic analyses of the southern binary star PU ***-resolution spectra of this system were taken at the University of Canterbury *** Observatory in the years 2008 and again in *** find the light contribution of the secondary component to be only 2%of the total light of the system in optical wavelengths,resulting in a single-lined spectroscopic *** TESS data revealed grazing eclipses within the light minima,though the tidal distortion,examined also from Hipparcos data,remains the predominating light curve *** model shows PU Pup to have the more massive primary relatively close to filling its Roche *** Pup is thus approaching the rare‘fast phase’of interactive(Case B)*** adopted absolute parameters are as follows:M_(1)=4.10(±0.20)M_(⊙),M_(2)=0.65(±0.05)M_(⊙),R_(1)=6.60(±0.30)R_(⊙),R_(2)=0.90(±0.10)R_(⊙);T_(1)=11500(±500)K,T_(2)=5000(±350)K;photometric distance=186(±20)pc,age=170(±20)*** less-massive secondary component is found to be significantly oversized and overluminous compared to standard main sequence *** discuss this discrepancy referring to heating from the reflection effect.

关键词： (stars:)binaries(including multiple):close stars:early-type stars:individual(PU Pup) Galaxy:stellar content

Magnetar giant flare originating from GRB 200415A:transient GeV emission, time-resolved E_(p)-L_(iso) correlation and implications

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Research in Astronomy and Astrophysics 2021年第9期21卷 224-230页

作者： Vikas Chand Jagdish C.Joshi Rahul Gupta Yu-Han Yang Dimple Vidushi Sharma Jun Yang Manoneeta Chakraborty Jin-Hang Zou Lang Shao Yi-Si Yang Bin-Bin Zhang Shashi Bhushan Pandey Ankush Banerjee Eman Moneer School of Astronomy and Space Science Nanjing UniversityNanjing 210093China Key Laboratory of Modern Astronomy and Astrophysics(Nanjing University) Ministry of EducationNanjing 210093China Aryabhatta Research Institute of Observational Sciences(ARIES) Manora PeakNainital-263002India Department of Physics Deen Dayal Upadhyaya Gorakhpur UniversityGorakhpur 273009India Inter University Centre for Astronomy and Astrophysics PuneIndia DAASE Indian Institute of Technology IndoreKhandwa RoadSimrolIndore 453552India College of Physics Hebei Normal UniversityShijiazhuang 050024China Department of Physics and Astronomy University of NevadaLas VegasNV 89154USA Princess Nourah Bint Abdurhamn University Department of PhysicsKSA Riyadh 84428 Airport RoadKSA11671 Private astronomer

Giant flares(GFs)are unusual bursts from soft gamma-ray repeaters(SGRs)that release an enormous amount of energy in a fraction of a *** afterglow emission of these SGR-GFs or GF candidates is a highly beneficial means of discerning their composition,relativistic speed and emission *** 200415A is a recent GF candidate observed in a direction coincident with the nearby Sculptor galaxy at 3.5 *** this work,we searched for transient gamma-ray emission in past observations by Fermi-LAT in the direction of GRB *** observations confirm that GRB 200415A is observed as a transient GeV source only once.A pure pair-plasma fireball cannot provide the required energy for the interpretation of GeV afterglow emission and a baryonic poor outflow is additionally needed to explain the afterglow emission.A baryonic rich outflow is also viable,as it can explain the variability and observed quasi-thermal spectrum of the prompt emission if dissipation is happening below the photosphere via internal *** the peak energy(Ep)of the time-resolved prompt emission spectra and their fluxes(Fp),we found a correlation between Ep and Fp or isotropic luminosity Liso for GRB *** supports the intrinsic nature of Ep-Liso correlation found in SGRs-GFs,hence favoring a baryonic poor *** results also indicate a different mechanism at work during the initial spike,and that the evolution of the prompt emission spectral properties in this outflow would be intrinsically due to the injection process.

关键词： gamma-rays:general stars:magnetars stars:flares methods:data analysis