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arXiv 2023年

作者： Hussenot-Desenonges, T. Wouters, T. Guessoum, N. Abdi, I. Abulwfa, A. Adami, C. Fernández, J.F. Agüí Ahumada, T. Aivazyan, V. Akl, D. Anand, S. Andrade, C.M. Antier, S. Ata, S.A. D’Avanzo, P. Azzam, Y.A. Baransky, A. Basa, S. Blazek, M. Bendjoya, P. Beradze, S. Boumis, P. Bremer, M. Brivio, R. Buat, V. Bulla, M. Burkhonov, O. Burns, E. Cenko, S.B. Coughlin, M.W. Corradi, W. Daigne, F. Dietrich, T. Dornic, D. Ducoin, J.-G. Duverne, P.-A. Elhosseiny, E.G. Elnagahy, F.I. El-Sadek, M.A. Ferro, M. Le Floc’h, E. Freeberg, M. Fynbo, J.P.U. Götz, D. Gurbanov, E. Hamed, G.M. Hasanov, E. Healy, B.F. Heintz, K.E. Hello, P. Inasaridze, R. Iskandar, A. Ismailov, N. Izzo, L. Jhawar, S. du Laz, T. Jegou Kamel, T.M. Karpov, S. Klotz, A. Koulouridis, E. Kuin, N.P. Kochiashvili, N. Leonini, S. Lu, K.-X. Malesani, D.B. Mašek, M. Mao, J. Melandri, A. Mihov, B.M. Natsvlishvili, R. Navarete, F. Nedora, V. Nicolas, J. Odeh, M. Palmerio, J. Pang, P.T.H. De Pasquale, M. Peng, H.W. Pormente, S. Peloton, J. Pradier, T. Pyshna, O. Rajabov, Y. Rakotondrainibe, N.A. Rivet, J.-P. Rousselot, L. Saccardi, A. Sasaki, N. Schneider, B. Serrau, M. Shokry, A. Slavcheva-Mihova, L. Simon, A. Sokoliuk, O. Srinivasaragavan, G. Strausbaugh, R. Takey, A. Tanvir, N.R. Thöne, C.C. Tillayev, Y. Tosta e Melo, I. Turpin, D. de Ugarte Postigo, A. Vasylenko, V. Vergani, S.D. Vidadi, Z. Xu, D. Wang, L.T. Wang, X.F. Winters, J.M. Zhang, X.-L. Zhu, Z. IJCLab Univ Paris-Saclay CNRS IN2P3 Orsay France Nikhef Science Park 105 Amsterdam1098 XG Netherlands Utrecht University Princetonplein 1 Utrecht3584 CC Netherlands Physics Department American University of Sharjah Sharjah United Arab Emirates 1 El-marsad St. Helwan Cairo11421 Egypt Aix Marseille Univ CNRS CNES LAM Marseille France Instituto de Astrofísica de Andalucía Glorieta de la Astronomía s/n Granada18008 Spain Cahill Center for Astrophysics California Institute of Technology PasadenaCA91125 United States E. Kharadze Georgian National Astrophysical Observatory Mt. Kanobili Abastumani Adigeni0301 Georgia Samtskhe-Javakheti State University Rustaveli Str. 113 Akhaltsikhe0080 Georgia School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Observatoire de la Côte d’Azur Université Côte d’Azur Boulevard de l’Observatoire Nice06304 France INAF–Osservatorio Astronomico di Brera Via E. Bianchi 46 LC Merate23807 Italy Astronomical Observatory Taras Shevchenko National University of Kyiv Observatorna Str. 3 Kyiv04053 Ukraine CEICO Institute of Physics The Czech Academy of Sciences Na Slovance 1999/2 PrahaCZ-182 21 Czech Republic Centro Astronómico Hispano en Andalucía Observatorio de Calar Alto Sierra de los Filabres Gérgal Almería04550 Spain Laboratoire J.-L. Lagrange Université de Nice Sophia-Antipolis CNRS Observatoire de la Côte d’Azur Nice06304 France National Observatory of Athens Institute for Astronomy Astrophysics Space Applications and Remote Sensing Greece Institut de Radioastronomie Millimétrique France Università degli Studi dell’Insubria Dipartimento di Scienza e Alta Tecnologia Via Valleggio 11 Como22100 Italy Department of Physics and Earth Science University of Ferrara via Saragat 1 FerraraI-44122 Italy INFN Sezione di Ferrara via Saragat 1 FerraraI-44122 Italy INAF Osservatorio Astronomico d’Abruzzo via Mentore Maggini snc TeramoI-64100 Italy Ulugh Beg Astrono

GRB 230812B is a bright and relatively nearby (z = 0.36) long gamma-ray burst (GRB) that has generated significant interest in the community and has thus been observed over the entire electromagnetic spectrum. We report over 80 observations in X-ray, ultraviolet, optical, infrared, and sub-millimeter bands from the GRANDMA (Global Rapid Advanced Network for Multi-messenger Addicts) network of observatories and from observational partners. Adding complementary data from the literature, we then derive essential physical parameters associated with the ejecta and external properties (i.e. the geometry and environment) of the GRB and compare with other analyses of this event. We spectroscopically confirm the presence of an associated supernova, SN2023pel, and we derive a photospheric expansion velocity of v ∼ 17×103 km s-1. We analyze the photometric data first using empirical fits of the flux and then with full Bayesian Inference. We again strongly establish the presence of a supernova in the data, with a maximum (pseudo-)bolometric luminosity of 5.75×1042 erg/s, at 15.76+0.81-1.21 days (in the observer frame) after the trigger, with a half-max time width of 22.0 days. We compare these values with those of SN1998bw, SN2006aj, and SN2013dx. Our best-fit model favours a very low density environment (log10(nISM/cm-3) = -2.38+1.45-1.60) and small values for the jet’s core angle θcore = 1.54+1.02-0.81 deg and viewing angle θobs = 0.76+1.29-0.76 deg. GRB 230812B is thus one of the best observed afterglows with a distinctive supernova bump. © 2023, CC BY.

关键词： Supernovae

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The role of environment on the star formation history of disc galaxies

arXiv

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arXiv 2017年

作者： Kang, Xiaoyu Zhang, Fenghui Chang, Ruixiang Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China

NGC 2403, NGC 300 and M33 are three nearby pure-disc galaxies with similar stellar mass in different environments, they are benchmarks for understanding late-type spiral galaxies in different environments. The chemical evolution and growth of their discs are investigated by using the simple chemical evolution model, in which their discs are assumed to originate and grow through the accretion of the primordial gas, and the gas outflow process is also taken into account. Through comparative study of the best-fitting model predicted star formation histories for them, we hope to derive a picture of the local environment on the evolution and star formation histories of galaxies and whether or not the isolated galaxies follow similar evolution history. Our results show that these three galaxies accumulated more than 50 percent of their stellar mass at z 25−1. The similar metallicity gradients in NGC 2403 and NGC 300 indicate that they may experience similar chemical evolutionary histories. The principal epoch of star formation on the discs of NGC 2403 and NGC 300 is earlier than that on the disc of M33, and the mean age of stellar populations along the discs of both NGC 2403 and NGC 300 is older than that of M33. Our results indicates that the evolution and star formation history of a galaxy indeed depends on its local environment, at least for galaxies with stellar mass of 109.2 M ∼ 109.7 M. Copyright © 2017, The Authors. All rights reserved.

关键词： Galaxies

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Astrometry of three near Earth asteroids with the Lijiang 2.4 m telescope

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Research in Astronomy and Astrophysics 2015年第3期15卷 435-442页

作者： Xi-Liang Zhang Yong Yu Xue-Li Wang Chuan-Jun Wang Liang Chang Yu-Feng Fan Zheng-Hong Tang Yunnan Observatories Chinese Academy of Sciences Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Shanghai Astronomical Observatory Chinese Academy of Sciences

Under the framework of observational campaigns organized by the GAIA Follow Up Network for Solar System objects, three near Earth asteroids, 367943 Duende, 99942 Apophis and 2013 TV135, were observed with the Lijiang 2.4m telescope administered by Yunnan Observatories. The software package PRISM was used to calibrate the CCD fields and measure the positions of 99942 Apophis and 2013 TV135, and our own software was used for 367943 Duende. A comparison of the results show that the ephemerides of INPOP10a and JPL are consistent for 99942 Apophis and 2013 TV135, however, they are quite inconsistent for 367943 Duende. Moreover, we have found that differences between the mean values in the ephemerides of INPOP10a and JPL are about 72＂ and -199＂ in right ascension and declination respectively for 367943 Duende. Moreover, the ephemeris published by JPL is reliable in terms of the mean observed-minus-calculated （O - C） residuals in right ascension and declination of about 2.72＂ and 1.49＂ respectively.

关键词： astrometry -- near Earth objects -- astrometric observation --ephemerides

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LAMOST Views δ Scuti Pulsating Stars

arXiv

引用

arXiv 2017年

作者： Qian, S.-B. Li, L.-J. He, J.-J. Zhang, J. Zhu, L.-Y. Han, Z.-T. P. O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang Dis- trict Beijing100012 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China

About 766 δ Scuti stars were observed by LAMOST by 2017 June 16. Stellar atmospheric parameters of 525 variables were determined, while spectral types were obtained for all samples. In the paper, those spectroscopic data are catalogued. We detect a group of 131 unusual and cool variable stars (UCVs) that are distinguished from the normal δ Scuti stars (NDSTs). On the H−R diagram and the log g − T diagram, the UCVs are far beyond the red edge of pulsational instability trip. Their effective temperatures are lower than 6700 K with periods in the range from 0.09 to 0.22 d. NDSTs have metallicity close to that of the Sun as expected, while UCVs are slightly metal poor than NDSTs. The two peaks on the distributions of the period and stellar atmospheric parameters are all caused by the existence of UCVs. When those UCVs are excluded, it is discovered that the effective temperature, the gravitational acceleration, and the metallicity all are correlated with the pulsating period for NDSTs and their physical properties and evolutionary states are discussed. Detection of those UCVs indicates that about 25% of the known δ Scuti stars may be misclassified. However, if some of them are confirmed to be pulsating stars, they will be a new-type pulsator and their investigations will shed light on theoretical instability domains and on the theories of interacting between the pulsation and the convection of solar-type stars. Meanwhile, 88 δ Scuti stars are detected to be the candidates of binary or multiple systems. Copyright © 2017, The Authors. All rights reserved.

关键词： Temperature

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SN 2016X: A type ii-p supernova with a signature of shock breakout from explosion of a massive red supergiant

arXiv

引用

arXiv 2018年

作者： Huang, F. Wang, X.-F. Hosseinzadeh, G. Brown, P.J. Mo, J. Zhang, J.-J. Zhang, K.-C. Zhang, T.-M. Howell, D.-A. Arcavi, I. McCully, C. Valenti, S. Rui, L.-M. Song, H. Xiang, D.-F. Li, W.-X. Lin, H. Wang, L.-F. Physics Department and Tsinghua Centre for Astrophysics Tsinghua University Beijing100084 China Department of Astronomy Shanghai Jiao Tong University Shanghai200240 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Department of Physics University of California Santa BarbaraCA93106-9530 United States Las Cumbres Observatory 6740 Cortona Dr. Suite 102 GoletaCA93117-5575 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A&M University Department of Physics Astr Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Centre for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Department of Physics University of California 1 Shields Avenue DavisCA95616-5270 United States

We present extensive ultraviolet (UV) and optical photometry, as well as dense optical spectroscopy for type II Plateau (IIP) supernova SN 2016X that exploded in the nearby (- 15 Mpc) spiral galaxy UGC 08041. The observations span the period from 2 to 180 days after the explosion;in particular, the Swift UV data probably captured the signature of shock breakout associated with the explosion of SN 2016X. It shows very strong UV emission during the first week after explosion, with contribution of - 20 – 30% to the bolometric luminosity (versus . 15% for normal SNe IIP). Moreover, we found that this supernova has an unusually long rise time of about 12.6 ± 0.5 days in the R band (versus - 7.0 days for typical SNe IIP). The optical light curves and spectral evolution are quite similar to the fast-declining type IIP object SN 2013ej, except that SN 2016X has a relatively brighter tail. Based on the evolution of photospheric temperature as inferred from the Swift data in the early phase, we derive that the progenitor of SN 2016X has a radius of about 930 ± 70 R. This large-size star is expected to be a red supergiant star with an initial mass of & 19 – 20 M based on the mass −− radius relation of the Galactic red supergiants, and it represents one of the most largest and massive progenitors found for SNe IIP. Copyright © 2018, The Authors. All rights reserved.

关键词： Supernovae

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Discovery of two new hypervelocity stars from the lamost spectroscopic surveys

arXiv

引用

arXiv 2017年

作者： Huang, Y. Liu, X.-W. Zhang, H.-W. Chen, B.-Q. Xiang, M.-S. Wang, C. Yuan, H.-B. Tian, Z.-J. Li, Y.-B. Wang, B. South-Western Institute for Astronomy Research Yunnan University Kunming650500 China Department of Astronomy Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy Beijing Normal University Beijing100875 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories CAS Kunming650216 China LAMOST Fellow

We report the discovery of two new unbound hypervelocity stars (HVSs) from the LAMOST spectroscopic surveys. They are respectively a B2V type star of ∼ 7 Mowith a Galactic rest-frame radial velocity of 502 km s-1at a Galactocentric radius of ∼ 21 kpc and a B7V type star of ∼ 4 Mowith a Galactic rest-frame radial velocity of 408 km s-1at a Galactocentric radius of ∼ 30 kpc. The origins of the two HVSs are not clear given their currently poorly measured proper motions. However, the future data releases of Gaia should provide proper motion measurements accurate enough to solve this problem. The ongoing LAMOST spectroscopic surveys are expected to yield more HVSs to form a statistical sample, providing vital constraint on understanding the nature of HVSs and their ejection mechanisms. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

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A new mechanism of long-term period variations for W UMa-type contact binaries

arXiv

引用

arXiv 2017年

作者： Liu, L. Qian, S.-B. Xiong, X. Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

W UMa-type contact binaries belong to close binary systems whose components exactly overflow their Roche lobes and share a common convective envelope (CCE). In the last twenty years, the long-term variations of their orbital periods have been thought to depend on several mechanisms. Now, we suggest a new mechanism: CCE-dominated mechanism. The CCE-dominated mechanism is found based on our numerical result, especially at high mass ratios, that the orbital periods (P) of contact binaries change very much with their fill-out factors (f). Because f is taken as a measurement of the thickness of CCE, the physical cause for the variation of P is a mass transfer between CCE and components. Further, an f-dominated simplification model for this mechanism is introduced. According to it, P may change in a long-term oscillation way with a similar time scale of the thermal modulation, meanwhile q is decreasing slowly till the two components merge. It could be also applied to explain the presence of extremely short period, high mass ratio and deep contact binaries. Moreover, the CCE-dominated mechanism should always work due to mass transfer and mass loss both occurring via CCE. Therefor, the effect of CCE on the variations of orbital periods may have been underestimated before. Copyright © 2017, The Authors. All rights reserved.

关键词： Mass transfer

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Discovery of a deep, low mass ratio overcontact binary GSC 03517–00663

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Research in Astronomy and Astrophysics 2015年第6期15卷 889-895页

作者： Di-Fu Guo Kai Li Shao-Ming Hu Yun-Guo Jiang Dong-Yang Gao Xu Chen Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

When observing blazars, we identified a new eclipsing binary named GSC 03517-00663. The light curves of GSC 03517-00663 are typical of EW-type light curves. Based on the observation using the 1 m telescope at the Weihai Observatory of Shandong University, complete VRI light curves were determined. Then, we analyzed the multiple light curves using the Wilson-Devinney program. It was found that GSC 03517-00663 has a mass ratio of q = 0.164 and a degree of contact of f = 69.2%. GSC 03517-00663 is a deep, low mass ratio overcontact binary. The light curves of GSC 03517-00663 show a strong O＇Connell effect, which was explained by employing a dark spot on the secondary component.

关键词： stars binaries close -- stars binaries eclipsing -- stars individual （GSC 03517-00663）

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Light curve inversion of asteroid(585)Bilkis with Lommel-Seeliger ellipsoid method

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Research in Astronomy and Astrophysics 2016年第12期16卷 19-26页

作者： Ao Wang Xiao-Bin Wang Karri Muinonen Xianming L.Han Yi-Bo Wang Yunnan Observatories Chinese Academy of SciencesKunming 650011China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650011China University of Chinese Academy of Sciences Beijing 100049China Department of Physics University of HelsinkiGustaf Hallstromin katu 2aEO.Box 64FI-00014 U.HelsinkiFinland Finnish Geospatial Research Institute Geodeetinrinne 2FI-02430 MasalaFinland Department of Physics and Astronomy Butler UniversityIndianapolisIN 46208USA

The basic physical parameters of asteroids, such as spin parameters, shape and scattering parameters, can provide us with information on the formation and evolution of both the asteroids themselves and the entire solar system. In a majority of asteroids, the disk-integrated photometry measurement constitutes the primary source of the above knowledge. In the present paper, newly observed photometric data and existing data on（585） Bilkis are analyzed based on a Lommel-Seeliger ellipsoid model. With a Markov chain Monte Carlo（MCMC） method, we have determined the spin parameters（period, pole orientation）and shape（b/a, c/a） of（585） Bilkis and their uncertainties. As a result, we obtained a rotational period of 8.5738209 h with an uncertainty of 9×10^-7h, and derived a pole of（136.46°, 29.0°） in the ecliptic frame of J2000.0 with uncertainties of 0.67°and 1.1°in longitude and latitude respectively. We also derived triaxial ratios b/a and c/a of（585） Bilkis as 0.736 and 0.70 with uncertainties of 0.003 and 0.03 respectively.

关键词： asteroids -- photometric observation -- spin parameter -- shape -- MCMC method

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Effects of magnetic fields on equation of state of rotating stars

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Science China(Physics,Mechanics & Astronomy) 2015年第2期58卷 109-113页

作者： NA WeiWei LIN GuiFang HUANG RunQian Department of Physics Yunnan University Department of Physics Yuxi Normal University Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

The evolution of rotating stars with magnetic fields has been studied with focus given to the following aspects: the effects of magnetic fields on equation of state for stellar matter and the thermodynamic quantities; the effects of magnetic energy and pressure on the internal structure of stars. The differences between the structure and evolution of a 15M⊙rotating star with and without magnetic fields are discussed. Our results show that the magnetic fields have an effect on the structure and evolution of the star mainly during the central helium burning phase; and this influences the physical quantities in the stellar envelope where hydrogen and helium are partially ionized. This may influence stellar pulsation.

关键词： stars： magnetic fields stars： evolution stars： equation of state

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