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arXiv 2023年

作者： Li, Zhitong Zhang, Tianmeng Wang, Xiaofeng Zhang, Jujia Galbany, Lluís Filippenko, Alexei V. Brink, Thomas G. Ashall, Chris Zheng, WeiKang de Jaeger, Thomas Ragosta, Fabio Deckers, Maxime Gromadzki, Mariusz Young, D.R. Xi, Gaobo Chen, Juncheng Zhao, Xulin Sai, Hanna Yan, Shengyu Xiang, Danfeng Chen, Zhihao Li, Wenxiong Wang, Bo Zou, Hu Sui, Jipeng Wang, Jiali Ma, Jun Nie, Jundan Xue, Suijian Zhou, Xu Zhou, Zhimin Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China Key Laboratory of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Beijing100101 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain BarcelonaE-08034 Spain Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Physics Virginia Tech 850 West Campus Drive BlacksburgVA24061 United States Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States INAF – Osservatorio Astronomico di Roma via di Frascati 33 Monte Porzio Catone RomaI-00078 Italy School of Physics Trinity College Dublin The University of Dublin Dublin 2 Ireland Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 1NN United Kingdom Wu Zhou University Wuzhou543002 China Department of Physics Tianjin University of Technology Tianjin300384 China The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel

We have conducted photometric and spectroscopic observations of the peculiar Type Ia supernova (SN Ia) 2016ije that was discovered through the Tsinghua-NAOC Transient Survey. This peculiar object exploded in the outskirts of a metal-poor, low-surface brightness galaxy (i.e., Mg = −14.5 mag). Our photometric analysis reveals that SN 2016ije is subluminous (MB,max = −17.65±0.06 mag) but exhibits relatively broad light curves (∆m15(B) = 1.35±0.14 mag), similar to the behavior of SN 2002es. Our analysis of the bolometric light curve indicates that only 0.14±0.04 Mo of 56Ni was synthesized in the explosion of SN 2016ije, which suggests a less energetic thermonuclear explosion when compared to normal SNe Ia, and this left a considerable amount of unburned materials in the ejecta. Spectroscopically, SN 2016ije resembles other SN 2002es-like SNe Ia, except that the ejecta velocity inferred from its carbon absorption line (∼ 4500 km s−1) is much lower than that from silicon lines (∼ 8300 km s−1) at around the maximum light. Additionally, most of the absorption lines are broader than other 02es-like SNe Ia. These peculiarities suggest the presence of significant unburned carbon in the inner region and a wide line-forming region along the line of sight. These characteristics suggest that SN 2016ije might originate from the violent merger of a white dwarf binary system, when viewed near an orientation along the iron-group-element cavity caused by the companion star. © 2023, CC BY.

关键词： Supernovae

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Photometric investigations on two totally eclipsing contact binaries: V342 UMa and V509 Cam

arXiv

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arXiv 2019年

作者： Li, Kai Xia, Qi-Qi Liu, Jin-Zhong Zhang, Yu Gao, Xing Hu, Shao-Ming Guo, Di-Fu Chen, Xu Liu, Yuan Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Weihai264209 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Xinjiang Astronomical Observatory Chinese Academy of Sciences Urumqi830011 China Qilu Institute of Technology Jinan250200 China

By analyzing two sets of complete BV RcIc light curves of V342 UMa and three sets of complete BV RcIc light curves of V509 Cam, we determined that the two systems are both W-subtype contact binaries and that V342 UMa shows a shallow contact configuration, while V509 Cam exhibits a medium contact configuration. Since both of them are totally eclipsing binaries, the physical parameters derived only by the photometric light curves are ***, the period changes of the two targets were analyzed based on all available eclipsing times. We discovered that V342 UMa shows long-term period decrease with a rate of −1.02(±0.54) × 10−7 days/year and that V509 Cam exhibits long-term period increase with a rate of 3.96(±0.90) × 10−8 days/year. Both the conservative mass transfer and AML via magnetic stellar winds can interpret the long-term period decrease of V342 UMa. The long-term period increase of V509 Cam can be explained by mass transfer from the less massive star to the more massive one. The absolute parameters of the two binaries were estimated according to the Gaia distances and our derived photometric solution results. This method can be extended to other contact binaries without radial velocities but with reliable photometric solutions. The evolutionary states of them were discussed, we found that they reveal identical properties of other W-subtype contact systems. Copyright © 2019, The Authors. All rights reserved.

关键词： Cams

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The contact binary V344 Lacertae: Is it a triple system?

arXiv

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arXiv 2020年

作者： Liang, Liu Shengbang, Qian Kai, Li Jiajia, He Linjia, Li Ergang, Zhao Xuzhi, Li 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 University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space Sciences Shandong University Weihai264209 China

The V RI passbands light curves of V344 Lac were presented and analyzed by using the latest version of the W-D code. The observed spectrum reveals that V344 Lac is not an A3 type but would be a later F type star according to the yielded temperature. The results of solution show that V344 Lac is an A-subtype contact binary, with a mediate photometric mass ratio of 0.387 ± 0.003 and a mediate contact factor of 44.6 ± 3.0%. Based on the parallax given by Gaia, the parameters of the components are estimated as: M1 = 1.16 M☉, M2 = 0.45 M☉, R1 = 1.31 R☉, R2 = 0.88 R☉, L1 = 2.512 L☉, L2 = 1.057 L☉. The period investigation indicates that V344 Lac may have an eccentric orbital oscillation, with P3 = 12.4 ± 0.5 yr, A3 = 0.0020 ± 0.0002 d, and e = 0.38 ± 0.16. Analysis shows such oscillation would be caused by a magnetic activity which can be explained by the Applegate mechanism. Meanwhile, according to the value of l3 and the estimated physical parameters of V344 Lac, the mass of the third companion may be 0.79M☉. This third body could be a wide company. Copyright © 2020, The Authors. All rights reserved.

关键词： Parameter estimation

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The environmental dependence of Spitzer dusty Supernovae

arXiv

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arXiv 2023年

作者： Xiao, Lin Szalai, Tamás Galbany, Lluís Fox, Ori Hu, Lei Hu, Maokai Yang, Yi Moriya, Takashi J. Pessi, Thallis Han, Zhanwen Wang, Xiaofeng Yan, Shengyu Department of Physics Hebei University Baoding071002 China Hebei Key Laboratory of High-precision Computation and Application of Quantum Field Theory Baoding071002 China Hebei Research Center of the Basic Discipline for Computational Physics Baoding071002 China Department of Experimental Physics Institute of Physics University of Szeged Dóm tér 9 SzegedH-6720 Hungary HUN-REN–SZTE Stellar Astrophysics Research Group H-6500 BajaSzegedi út Kt. 766 Hungary Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain BarcelonaE-08034 Spain Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States McWilliams Center for Cosmology Department of Physics Carnegie Mellon University 5000 Forbes Ave PittsburghPA15213 United States Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China Tsinghua University Beijing100084 China Department of Astronomy University of California BerkeleyCA94720-3411 United States National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan School of Physics and Astronomy Monash University ClaytonVIC3800 Australia Instituto de Estudios Astrofísicos Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército Libertador 441 Santiago Chile Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories CAS Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China

Thanks to the mid-infrared capability offered by Spitzer, systematic searches of dust in SNe have been carried out over the past decade. Studies have revealed the presence of a substantial amount of dust over a broad range of SN subtypes. How normal SNe present mid-IR excess at later time and turn out to be dusty SNe can be affected by several factors, such as mass-loss history and envelope structure of progenitors and their explosion environment. All these can be combined and related to their environmental properties. A systematic analysis of SNe that exploded under a dusty environment could be of critical importance to measure the properties of the dust-veiled exploding stars, and whether such an intense dust production process is associated with the local environment. In this work, we firstly use the IFS data to study the environmental properties of dusty SNe compared to those of normal ones, and analyze correlations between the environmental properties and their dust parameters. We find that dusty SNe have a larger proportion located at higher SFR regions compared to the normal types. The occurrence of dusty SNe is less dependent on metallicity, with the oxygen abundance spanning from subsolar to oversolar metallicity. We also find the host extinction of dusty SNe scatters a lot, with about 40% of dusty SN located at extremely low extinction environments, and another 30% of them with considerably high host extinction of E(B-V)>0.6 mag. Copyright © 2023, The Authors. All rights reserved.

关键词： Supernovae

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Sensitive Chandra coverage of a representative sample of weak-line quasars: revealing the full range of X-ray properties

arXiv

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arXiv 2022年

作者： Ni, Qingling Brandt, W.N. Luo, B. Garmire, G.P. Hall, P.B. Plotkin, R.M. Shemmer, O. Timlin, J.D. Vito, F. Wu, J. Yi, W. Department of Astronomy and Astrophysics 525 Davey Lab The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Department of Physics The Pennsylvania State University University ParkPA16802 United States School of Astronomy and Space Science Nanjing University Nanjing Jiangsu 210093 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education Jiangsu Nanjing210093 China Huntingdon Institute for X-ray Astronomy LLC 10677 Franks Road HuntingdonPA16652 United States Department of Physics & Astronomy York University 4700 Keele Street TorontoONM3J 1P3 Canada Department of Physics University of Nevada 1664 N. Virginia St RenoNV89557 United States Department of Physics University of North Texas DentonTX76203 United States Scuola Normale Superiore Piazza dei Cavalieri 7 Pisa56126 Italy Department of Astronomy Xiamen University Fujian Xiamen361005 China Yunnan Observatories Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

We present deeper Chandra observations for weak-line quasars (WLQs) in a representative sample that previously had limited X-ray constraints, and perform X-ray photometric analyses to reveal the full range of X-ray properties of WLQs. Only 5 of the 32 WLQs included in this representative sample remain X-ray undetected after these observations, and a stacking analysis shows that these 5 have an average X-ray weakness factor of > 85. One of the WLQs in the sample that was known to have extreme X-ray variability, SDSS J1539+3954, exhibited dramatic X-ray variability again: it changed from an X-ray normal state to an X-ray weak state within ≈ 3 months in the rest frame. This short timescale for an X-ray flux variation by a factor of 9 further supports the thick disk and outflow (TDO) model proposed to explain the X-ray and multiwavelength properties of WLQs. The overall distribution of the X-ray-to-optical properties of WLQs suggests that the TDO has an average covering factor of the X-ray emitting region of ∼ 0.5, and the column density of the TDO can range from NH ∼ 1023−24 cm−2 to NH 1024 cm−2, which leads to different levels of absorption and Compton reflection (and/or scattering) among WLQs. Copyright © 2022, The Authors. All rights reserved.

关键词： Galaxies

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Characterizing the Gamma-ray Emission Properties of the Globular Cluster M5 with the Fermi-LAT

arXiv

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arXiv 2024年

作者： Hou, X. Zhang, W. Freire, P.C.C. Torres, D.F. Ballet, J. Smith, D.A. Johnson, T.J. Kerr, M. Cheung, C.C. Guillemot, L. Li, J. Zhang, L. Ridolfi, A. Wang, P. Li, D. Yuan, J. Wang, N. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China Campus UAB Barcelona08193 Spain Barcelona08034 Spain Max-Planck Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany BarcelonaE-08010 Spain Université Paris Saclay Université Paris Cité CEA CNRS AIM Gif-sur-YvetteF-91191 France Laboratoire d'Astrophysique de Bordeaux Université de Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire PessacF-33615 France College of Science George Mason University FairfaxVA22030 United States Naval Research Laboratory WashingtonDC20375 United States Space Science Division Naval Research Laboratory WashingtonDC20375-5352 United States Laboratoire de Physique et Chimie de l'Environnement et de l'Espace Université d'Orléans CNRS OrléansF-45071 Cedex 02 France Station de radioastronomie de Nançay Observatoire de Paris CNRS INSU NançayF-18330 France CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Centre for Astrophysics and Supercomputing Swinburne University of Technology P.O. Box 218 HawthornVIC3122 Australia INAF - Osservatorio Astronomico di Cagliari Via della Scienza 5 CA SelargiusI-09047 Italy Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China University of Chinese Academy of Sciences Chinese Academy of Sciences Beijing100101 China Zhijiang Lab Hangzhou311121 China Xinjiang Astronomical Observatory Chinese Academy of Sciences Xinjiang Urumqi830011 China

We analyzed the globular cluster M5 (NGC 5904) using 15 yr of gamma-ray data from the Fermi Large Area Telescope (LAT). Using rotation ephemerides generated from Arecibo and FAST radio telescope observations, we searched for gamma-ray pulsations from the seven millisecond pulsars (MSPs) identified in M5. We detected no significant pulsations from any of the individual pulsars. In addition, we searched for possible variations of the gamma-ray emission as a function of orbital phase for all six MSPs in binary systems, but we did not detect any significant modulations. The gamma-ray emission from the direction of M5 is well described by an exponentially cutoff power-law spectral model, although other models cannot be excluded. The phase-averaged emission is consistent with being steady on a time scale of a few months. We estimate the number of MSPs in M5 to be between 1 and 10, using the gamma-ray conversion efficiencies for well-characterized gamma-ray MSPs in the Third Fermi LAT of Gamma-ray Pulsars, suggesting that the sample of known MSPs in M5 is (nearly) complete, even if it is not currently possible to rule out a diffuse component of the observed gamma rays from the cluster. Copyright © 2024, The Authors. All rights reserved.

关键词： Gamma rays

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SN 2012ij: A low-luminosity type Ia supernova and evidence for continuous distribution from 91bg-like explosion to normal ones

arXiv

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arXiv 2022年

作者： Li, Zhitong Zhang, Tianmeng Wang, Xiaofeng Sai, Hanna Zhang, Jujia Chen, Juncheng Zhao, Xulin Yan, Shengyu Wang, Bo Phillips, Mark M. Hsiao, Eric Y. Morrell, Nidia Contreras, Carlos Burns, Christopher R. Ashall, Christopher Stritzinger, Maximilian Krisciunas, Kevin Prieto, Jose Zou, Hu Wang, Jiali Ma, Jun Nie, Jundan Xue, Suijian Zhou, Xu Zhou, Zhimin Xiang, Danfeng Xi, Gaobo Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Wu Zhou University Wuzhou543002 China Department of Physics Tianjin University of Technology Tianjin300384 China Carnegie Observatories Las Campanas Observatory Casilla 601 La Serena Chile Observatories of the Carnegie Institution for Science 813 Santa Barbara Street PasadenaCA91101 United States Institute for Astronomy University of Hawai'i at Manoa 2680 Woodlawn Dr. Hawai'i HI96822 United States Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University Department of Physics and Astronomy College StationTX77843 United States Department of Astrophysical Sciences Princeton University 4 Ivy Ln. Princeton NJ08544 United States

In this paper, we present photometric and spectroscopic observations of a subluminous type Ia supernova (SN Ia) 2012ij, which has an absolute B-band peak magnitude MB,max = −17.95 ± 0.15 mag. The B-band light curve exhibits a fast post-peak decline with ∆m15(B) = 1.86 ± 0.05 mag. All the R and I/i-band light curves show a weak secondary peak/shoulder feature at about 3 weeks after the peak, like some transitional subclass of SNe Ia, which could result from an incomplete merger of near-infrared (NIR) double peaks. The spectra are characterized by Ti ii and strong Si ii λ5972 absorption features that are usually seen in low-luminosity objects like SN 1999by. The NIR spectrum before maximum light reveals weak carbon absorption features, implying the existence of unburned materials. We compare the observed properties of SN 2012ij with those predicted by the sub-Chandrasekhar-mass and the Chandrasekhar-mass delayed-detonation models, and find that both optical and NIR spectral properties can be explained to some extent by these two models. By comparing the secondary maximum features in I and i bands, we suggest that SN 2012ij is a transitional object linking normal SNe Ia to typical 91bg-like ones. From the published sample of SNe Ia from the Carnegie S upernova Pro ject II (CSP-II), we estimate that the fraction of SN 2012ij-like SNe Ia is not lower than ∼ 2%. Copyright © 2022, The Authors. All rights reserved.

关键词： Supernovae

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Asteroseismology of the DOV star PG 1159-035

arXiv

引用

arXiv 2019年

作者： Chen, Y.H. Institute of Astrophysics Chuxiong Normal University Chuxiong675000 China School of Physics and Electronical Science Chuxiong Normal University Chuxiong675000 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650011 China

Grids of DOV star models are evolved by WDEC with fixed atmospheric constituent to the spectral values of XC/XHe/XO = 50/33/17. The core compositions are from white dwarf models at highest Teff evolved by MESA. The eigenfrequencies are calculated and used to fit the observed modes. Based on 264.1 hours of photometric observations on PG 1159-035, Winget et al. identified 125 individual frequencies. Costa et al. identified 198 pulsation modes for PG 1159-035 according to the WET photometric data from 1983, 1985, 1989, and 2002. Both of them derived frequency splitting values of δσl=1 ∼ 4.2µHz and δσl=2 ∼ 6.9µHz. According to the values of δσl=1 and δσl=2, 20 triplets and 9 quintuplets are selected and used to constrain the fitting models. Our optimal model has Teff = 129000K, M∗ = 0.63M☉, logg = 7.59, log(Menv/M∗) = -5.0, and σRMS = 1.97s. The values of Teff and logg are consistent with that values of Córsico et al.. The calculated modes of minimum rate of period change correspond to modes with maximum kinetic energy distributed in the envelope. The observed rates of period change with positive and negative values can also be partially reproduced. In particular, there are negative rates of period change for the calculated modes from our optimal model, which is not found in previous work. Copyright © 2019, The Authors. All rights reserved.

关键词： White dwarfs

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Absolute physical parameters of three poorly studied detached eclipsing binaries

arXiv

引用

arXiv 2020年

作者： Yang, Daoye Y. Li, L.-F. Han, Q.-W. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China University of the Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Beijing100012 China Key Lab of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang Beijing100012 China School of Physics and Electronics Qiannan Normal University for Nationalities Duyun558000 China

The photometric and spectroscopic data for three double-lined detached eclipsing binaries were collected from the photometric and spectral surveys. The light and radial velocity curves of each binary system were simultaneously analyzed by using Wilson-Devinney (WD) code, and the absolute physical and orbital parameters of these binaries were derived. The masses of both components of ASASSN-V J063123.82+192341.9 were found to be M1 = 1.088 ± 0.016 and M2 = 0.883 ± 0.016 M☉;and those of ASAS J011416+0426.4 were determined to be M1 = 0.934 ± 0.046 and M2 = 0.754 ± 0.043M☉;those of MW Aur were derived to be M1 = 2.052 ± 0.196 and M2 = 1.939 ± 0.193 M☉. At last, the evolutionary status of these detached binaries was discussed based on their absolute parameters and the theoretical stellar models. Copyright © 2020, The Authors. All rights reserved.

关键词： Photometry

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The amplitude of the kilohertz quasi-periodic oscillations in 4U 1636−53 in the frequency-energy space

arXiv

引用

arXiv 2019年

作者： Ribeiro, Evandro M. Méndez, Mariano de Avellar, Marcio G.B. Zhang, Guobao Karpouzas, Konstantinos Kapteyn Astronomical Institute University of Groningen P.O. BOX 800 Groningen9700 AV Netherlands Instituto Tecnológico de Aeronáutica ITA Brazil Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China

We present for the neutron-star low-mass X-ray binary 4U 1636−53, and for the first time for any source of kilohertz quasi-periodic oscillations (kHz QPOs), the two-dimensional behaviour of the fractional rms amplitude of the kHz QPOs in the parameter space defined by QPO frequency and photon energy. We find that the rms amplitude of the lower kHz QPO increases with energy up to ∼ 12 keV and then decreases at higher energies, while the rms amplitude of the upper kHz QPO either continues increasing or levels off at high energies. The rms amplitude of the lower kHz QPO increases and then decreases with frequency, peaking at ∼ 760 Hz, while the amplitude of the upper kHz QPO decreases with frequency, with a local maximum at around ∼ 770 Hz, and is consistent with becoming zero at the same QPO frequency, ∼ 1400 Hz, in all energy bands, thus constraining the neutron-star mass at MNS ≤ 1.6M , under the assumption that this QPO reflects the Keplerian frequency at the inner edge of the accretion disc. We show that the slope of the rms energy spectrum is connected to the changing properties of the kHz QPOs in different energy bands as its frequencies change. Finally, we discuss a possible mechanism responsible for the radiative properties of the kHz QPOs and, based on a model in which the QPO arises from oscillations in a Comptonising cloud of hot electrons, we show that the properties of the kHz QPOs can constrain the thermodynamic properties of the inner accretion flow. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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