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arXiv 2021年

作者： Zeng, Xiangyun Wang, Xiaofeng Esamdin, Ali Pellegrino, Craig Zheng, Weikang Zhang, Jujia Mo, Jun Li, Wenxiong Howell, D. Andrew Filippenko, Alexei V. Lin, Han Brink, Thomas G. Baron, Edward A. Burke, Jamison Derkacy, James M. McCully, Curtis Hiramatsu, Daichi Hosseinzadeh, Griffin Jeffers, Benjamin T. Ross, Timothy W. Stahl, Benjamin E. Stegman, Samantha Valenti, Stefano Wang, Lifan Xiang, Danfeng Zhang, Jicheng Zhang, Tianmeng Xinjiang Astronomical Observatory Chinese Academy of Sciences Xinjiang Urumqi830011 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing100049 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science of Technology Beijing100044 China Department of Physics University of California Santa BarbaraCA93106-9530 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States 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 20A Datun Road Chaoyang District Beijing100012 China School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Homer L. Dodge Department of Physics and Astronomy University of Oklahoma United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA9311-5575 United States Department of Physics University of California BerkeleyCA94720-7300 United States Department of Chemistry University of Wisconsin MadisonWI53706 United States Department of Physics University of California DavisCA95616 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A&M University Department of Physics and Astronomy 4242 TAMU College StationTX77843 United States Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China

We present extensive, well-sampled optical and ultraviolet photometry and optical spectra of the Type Ia supernova (SN Ia) 2017hpa. The light curves indicate that SN 2017hpa is a normal SN Ia with an absolute peak magnitude of MmaxB ≈ −19.12 ± 0.11 mag and a post-peak decline rate ∆m15(B) = 1.02 ± 0.07 mag. According to the quasibolometric light curve, we derive a peak luminosity of 1.25 × 1043 erg s−1and a 56Ni mass of 0.63 ± 0.02 M☉. The spectral evolution of SN 2017hpa is similar to that of normal SNe Ia, while it exhibits unusually rapid velocity evolution resembling that of SN 1991bg-like SNe Ia or the high-velocity subclass of SNe Ia, with a post-peak velocity gradient of ∼ 130 ± 7 km s−1 d−1. Moreover, its early spectra (t © 2021, CC BY.

关键词： White dwarfs

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Search for γ-ray emission from dark matter particle interactions from the Andromeda and Triangulum galaxies with the Fermi Large Area Telescope

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Physical Review D 2019年第12期99卷 123027-123027页

作者： Mattia Di Mauro Xian Hou Christopher Eckner Gabrijela Zaharijas Eric Charles NASA Goddard Space Flight Center Greenbelt Maryland 20771 USA Catholic University of America Department of Physics Washington D.C. 20064 USA Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 People’s Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 People’s Republic of China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing 100012 People’s Republic of China Center for Astrophysics and Cosmology University of Nova Gorica Vipavska 13 SI-5000 Nova Gorica Slovenia SLAC National Accelerator Laboratory Stanford University Stanford California 94305 USA

The Andromeda (M31) and Triangulum (M33) galaxies are the closest Local Group galaxies to the Milky Way, being only 785 and 870 kpc away. These two galaxies provide an independent view of high-energy processes that are often obscured in our own Galaxy, including possible signals of dark matter (DM) particle interactions. The Fermi Large Area Telescope (Fermi-LAT) preliminary eight year list of sources includes both M31, which is detected as extended with a size of about 0.4°, and M33, which is detected as a pointlike source. The spatial morphology of M31 γ-ray emission could trace a population of unresolved sources and energetic particles originating in sources not related to massive star formation. Alternatively, the γ-ray emission could also be an indication of annihilation or decay of DM particles. We investigate these two possibilities using almost 10 years of data from the Fermi-LAT. An interpretation that involves only a DM γ-ray emission is in tension with the current limits from other searches, such as those targeting Milky Way dwarf spheroidal galaxies. When we include a template of astrophysical emission, tuned on γ-ray data or from observations of these galaxies in other wavelengths, we do not find any significant evidence for a DM contribution and we set limits for the annihilation cross section that probe the thermal cross section for DM masses up to a few tens of GeV in the bb¯ and τ+τ− channels. For models where the DM substructures have masses above 10−6 solar masses our limits probe the DM interpretation of the Fermi-LAT Galactic center excess. We provide also the lower limit for the DM lifetime assuming the same spatial models of the DM distribution in M31 and M33.

关键词： Cosmic ray sources Gamma ray astronomy Particle dark matter

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White dwarf deflagrations for Type Iax supernovae: Polarisation signatures from the explosion and companion interaction

arXiv

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arXiv 2020年

作者： Bulla, M. Liu, Z.-W. Röpke, F.K. Sim, S.A. Fink, M. Kromer, M. Pakmor, R. Seitenzahl, I.R. Nordita KTH Royal Institute of Technology Stockholm University Roslagstullsbacken 23 StockholmSE-106 91 Sweden Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China Center for Astronomical Mega-Science CAS Beijing100012 China Zentrum für Astronomie der Universität Heidelberg Institut für Theoretische Astrophysik Philosophenweg 12 Heidelberg69120 Germany Heidelberger Institut für Theoretische Studien Schloss-Wolfsbrunnenweg 35 Heidelberg69118 Germany Astrophysics Research Centre School of Mathematics and Physics Queen's University BelfastBT7 1NN United Kingdom Institut für Theoretische Physik und Astrophysik Universität Würzburg Emil-Fischer-Straße 31 WürzburgD-97074 Germany Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany School of Science University of New South Wales Australian Defence Force Academy Northcott Drive CanberraACT2600 Australia

Growing evidence suggests that Type Iax supernovae might be the result of thermonuclear deflagrations of Chandrasekhar-mass white dwarfs in binary systems. We carry out Monte Carlo radiative transfer simulations and predict spectropolarimetric features originating from the supernova explosion and subsequent ejecta interaction with the companion star. Specifically, we calculate viewing-angle dependent flux and polarisation spectra for a 3D model simulating the deflagration of a Chandrasekhar-mass white dwarf and, for a second model, simulating the ejecta interaction with a main-sequence star. We find that the intrinsic signal is weakly polarised and only mildly viewing-angle dependent, owing to the overall spherical symmetry of the explosion and the depolarising contribution of iron-group elements dominating the ejecta composition. The interaction with the companion star carves out a cavity in the ejecta and produces a detectable, but modest signal that is significant only at relatively blue wavelengths (. 5000 Å). In particular, increasingly fainter and redder spectra are predicted for observer orientations further from the cavity, while a modest polarisation signal P ∼ 0.2 per cent is found at blue wavelengths for orientations 30◦ and 45◦ away from the cavity. We find a reasonable agreement between the interaction model viewed from these orientations and spectropolarimetric data of SN 2005hk and interpret the maximum-light polarisation signal seen at blue wavelengths for this event as a possible signature of the ejecta-companion interaction. We encourage further polarimetric observations of SNe Iax to test whether our results can be extended and generalised to the whole SN Iax class. Copyright © 2020, The Authors. All rights reserved.

关键词： Radiative transfer

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Formation of hot subdwarf B stars with neutron star components

arXiv

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arXiv 2018年

作者： Wu, You Chen, Xuefei Li, Zhenwei Han, Zhanwen 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 Science Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

Context. Binary population synthesis predicts the existence of subdwarf B stars (sdBs) with neutron star (NS) or black hole (BH) companions. Several works have been dedicated to finding such systems, but none has been confirmed yet. Theoretically, the formation of sdBs with white dwarf (WD) and main sequence (MS) companions has been well investigated, while those with NS or BH companions remain to be explored further. Aims. We systematically investigate the formation of sdB+NS binaries from binary evolution and aim to obtain some clues for a search for such systems. Methods. We started from a series of MS+NS systems and determined the parameter spaces for producing sdB+NS binaries from the stable Roche-lobe overflow (RLOF) channel and from the common envelope (CE) ejection channel. The parameters for sdB+NS binaries were obtained from detailed binary evolution calculation with the code called modules for experiments in stellar astrophysics (MESA), and the CE parameters were given by the standard energy budget for CE evolution. The MS star had an initial mass ranging from 0.8 to 5 M. Various NS accretion efficiencies and NS masses were examined to investigate the effects they have. We show the characteristics of the produced sdB+NS systems, such as the mass of components, orbital period, the semi-amplitude of the radial velocity (K), and the spin of the NS component. Results. sdB+NS binaries can be produced either from stable RLOF or from CE ejection. In the stable RLOF channel, sdBs can be formed when the donor starts mass transfer close to the tip of the giant branch if the donor has an initial mass ≤ 2.0M. For more massive donors, sdBs can be formed when the donor starts mass transfer during the Hertzsprung gap or near the end of the MS. The orbital period of sdB+NS binaries produced in this way ranges from several days to more than 1000 days and moves toward the short-period (∼ hr) side with increasing initial MS mass. The highest K is about 150km s−1 for an MS s

关键词： Neutrons

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Subdwarf B stars as possible surviving companions in Type Ia supernova remnants

arXiv

引用

arXiv 2018年

作者： Meng, Xiangcun Li, Jiao 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 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China

Although type Ia supernovae (SNe Ia) are so important in many astrophysical fields, a debate on their progenitor model is still endless. Searching the surviving companion in a supernova remnant (SNR) may distinguish different progenitor models, since a companion still exists in the remnant for the single-degenerate (SD) model, but does not for the double degenerate (DD) model. However, some recent surveys do not discover the surviving companions in the remnant of SN 1006 and Kepler’s supernova, which seems to disfavor the SD model. Such a result could be derived from an incorrect survey target. Here, based on the common-envelope wind SD model for SNe Ia, in which the initial binary system consists of a white dwarf (WD) and a main-sequence (MS) star, we found that the companion at the moment of supernova explosion may be a MS, red-giant (RG) or subdwarf B (sdB) star if a spin-down timescale of less than 107 yr is assumed. We show the properties of the companions at the moment of supernova explosion, which are key clues to search the surviving companions in SNRs. Here, we suggest that the sdB star may be the surviving companion in some SNRs, even if the progenitor systems are the WD + MS systems. The SNe Ia with the sdB companions may contribute to all SNe Ia as much as 22%. Copyright © 2018, The Authors. All rights reserved.

关键词： White dwarfs

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Disruption of a planet spiralling into its host star

arXiv

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arXiv 2018年

作者： Jia, Shi Spruit, H.C. Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China University of Chinese Academy of Sciences Beijing100049 China

The processes leading deformation and destruction of planets spiraling into the convective envelope of their host stars are described. The planet is compressed by the ram pressure, and deformed into a attened shape for which a quantitative model is developed. Compression increases the planet's density contrast with the envelope and its gravitational binding energy. This increases the survivability especially of gas planets. An estimate is given for the depth of disruption by ram pressure, and for the subsequent fragmentation of the remnants. We show how the debris of rocky or iron planets, instead of mixing through the convection zone, sinks below the base of the convection zone. The time scale of the entire sequence of events is of the order of a few orbital times of the planet. If spiral-in of (partly) icy, rocky or iron planets has happened to the pre-main sequence Sun, it could account for the higher opacity below the base of the convection zone as inferred from helioseismology. Copyright © 2018, The Authors. All rights reserved.

关键词： Planets

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Black hole and neutron star binary mergers in triple systems: Merger fraction and spin-orbit misalignment

arXiv

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arXiv 2018年

作者： Liu, Bin Lai, Dong Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Cornell Center for Astrophysics and Planetary Science Cornell University IthacaNY14853 United States Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Tsung-Dao Lee Institute Shanghai200240 China

Black hole (BH) mergers driven by gravitational perturbations of external companions constitute an important class of formation channels for merging BH binaries detected by LIGO. We have studied the orbital and spin evolution of binary BHs in triple systems, where the tertiary companion excites large eccentricity in the inner binary through Lidov-Kozai oscillations, causing the binary to merge via gravitational radiation. Using the single-averaged and double-averaged secular dynamics of triples (where the equations of motion are averaged over the inner orbit and both orbits, respectively), we perform a large set of numerical integrations to determine the merger window (the range of companion inclinations that allows the inner binary to merge within ∼10 Gyrs) and the merger fraction as a function of various system parameters (e.g., the binary masses m1;m2 and initial semi-major axis a0, the mass, semi-major axis and eccentricity eout of the outer companion). For typical BH binaries (m1;2 20Mo - 30Mo and a0 10 AU), the merger fraction increases rapidly with eout because of the octupole perturbation, ranging from ∼ 1% at eout = 0 to 10 - 20% at eout = 0:9. We derive the analytical expressions and approximate scaling relations for the merger window and merger fraction for systems with negligible octupole effect, and apply them to neutron star binary mergers in triples. We also follow the spin evolution of the BHs during the companion-induced orbital decay, where de-Sitter spin precession competes with Lidov-Kozai orbital precession/nutation. Starting from aligned spin axes (relative to the orbital angular momentum axis), a wide range of final spin-orbit misalignment angle θf sl can be generated when the binary enters the LIGO sensitivity band. For systems where the octupole effect is small (such as those with m1 m2 or eout ∼ 0), the distribution of θf sl peaks around 90_. As the octuple effect increases, a more isotropic distribution of final spin axis is produced. Over

关键词： Merging

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Statistical analysis on XMM-Newton X-ray flares of Mrk 421: distributions of peak flux and flaring time duration

arXiv

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arXiv 2018年

作者： Yan, Dahai Yang, Shenbang Zhang, Pengfei Dai, Benzhong Wang, Jiancheng Zhang, Li Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008

The energy dissipation mechanism in blazar jet is unknown. Blazar’s flares could provide insights on this problem. Here we report statistical results of XMM-Newton X-ray flares of Mrk 421. We analyze all public XMM-Newton X-ray observations for Mrk 421, and construct the light curves. Through fitting light curves, we obtain the parameters of flare-profiles, such as peak flux (Fp) and flaring time duration (Tfl). It is found that both the distributions of Fp and Tfl obey a power-law form, with the same index of αF = αT ≈ 1. The statistical properties are consistent with the predictions by a self-organized criticality (SOC) system with energy dissipation in one-dimensional space. This is similar to solar flare, but with different space dimensions of the energy dissipation domain. This suggests that X-ray flaers of Mrk 421 are possibly driven by a magnetic reconnection mechanism. Moreover, in the analysis, we find that variability on timescale of ∼ 1000 s frequently appears. Such rapid variability indicates a magnetic field of ≥ 2.1δD−1/3 G (δD is the Doppler factor) in emission region. Copyright © 2018, The Authors. All rights reserved.

关键词： Energy dissipation

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Resolved neutral carbon emission in nearby galaxies: [C i] lines as total molecular gas tracers

arXiv

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arXiv 2019年

作者： Jiao, Qian Zhao, Yinghe Lu, Nanyao Gao, Yu Salak, Dragan Zhu, Ming Zhang, Zhiyu Jiang, Xuejian Tan, Qinghua Nanjing210008 China Yunnan Observatories & Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Camino El Observatorio 1515 Las Condes Santiago Chile National Astronomical Observatories & Key Lab of Radio Astronomy CAS Beijing100012 China School of Science and Technology Kwansei Gakuin University 2-1 Gakuen SandaHyogo669-1337 Japan Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom ESO Karl Schwarzschild Strasse 2 Garching MunichD-85748 Germany

We present maps of atomic carbon [C i] (3P1 → 3P0) and [C i] (3P2 → 3P1) emission (hereafter [C i] (1−0) and [C i] (2−1), respectively) at a linear resolution ∼ 1 kpc scale for a sample of one Hii, six LINER, three Seyfert and five starburst galaxies observed with the Herschel Space Observatory. We compare spatial distributions of two [C i] lines with that of CO J = 1 → 0 (hereafter CO (1−0)) emission, and find that both [C i] lines distribute similarly to CO (1−0) emission in most galaxies. We present luminosity ratio maps of L0[CI](1−0)/L0CO(1−0), L0[CI](2−1)/L0CO(1−0), L0[CI](2−1)/L0[CI](1−0) (hereafter R[CI]) and 70-to-160 µm far-infrared color of f70/f160. L0[CI](2−1)/L0CO(1−0), R[CI] and f70/f160 are centrally peaked in starbursts;whereas remain relatively constant in LINERs, indicating that star-forming activity can enhance carbon emission, especially for [C i] (2−1). We explore the correlations between the luminosities of CO (1−0) and [C i] lines, and find that L0CO(1−0) correlates tightly and almost linearly with both L0[CI](1−0) and L0[CI](2−1), suggesting that [C i] lines, similar as CO (1−0), can trace total molecular gas in Hii, LINER, Seyfert and starburst galaxies on kpc scales. We investigate the dependence of L0[CI](1−0)/L0CO(1−0), L0[CI](2−1)/L0CO(1−0) and [C i] excitation temperature of Tex on dust temperature of Tdust, and find non-correlation, a weak and modest correlation, respectively. The ratio of L0[CI](1−0)/L0CO(1−0) stays smooth distribution in most galaxies, indicating that the conversion factor of [C i] (1−0) luminosity to H2 mass (X[CI](1−0)) changes with CO (1−0) conversion factor (αCO) proportionally. Under optically thin and local thermodynamical equilibrium (LTE) assumptions, we derive a galaxy-wide average carbon excitation temperature of Tex ∼ 19.7 ± 0.5 K and an average neutral carbon abundance of X[CI]/X[H2] ∼ 2.5 ± 1.0 × 10−5 in our resolved sample, which is comparable to the usually adopted value of 3 × 10−5, but ∼ 3 times low

关键词： Galaxies

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Fast inflow directly feeding black hole accretion disk in quasars

arXiv

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arXiv 2019年

作者： Zhou, Hongyan Shi, Xiheng Yuan, Weimin Hao, Lei Chen, Xiangjun Ge, Jian Ji, Tuo Jiang, Peng Li, Ge Liu, Bifang Liu, Guilin Liu, Wenjuan Lu, Honglin Pan, Xiang Shen, Juntai Shu, Xinwen Sun, Luming Tian, Qiguo Wang, Huiyuan Wang, Tinggui Wu, Shengmiao Yang, Chenwei Zhang, Shaohua Zhong, Zhihao Antarctic Astronomy Research Division Key Laboratory for Polar Science of the State Oceanic Administration Polar Research Institute of China Shanghai China School of Astronomy and Space Sciences University of Science and Technology of China Hefei China Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences Department of Astronomy University of Science and Technology of China Hefei China National Astronomical Observatories of China Chinese Academy of Sciences Beijing China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai China Department of Astronomy University of Florida Bryant Space Science Center GainesvilleFL United States Yunnan Observatories Chinese Academy of Sciences Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Department of Physics Anhui Normal University Wuhu China

Quasars are high-luminosity active galactic nuclei believed to be powered by accretion of interstellar matter onto a super-massive black hole (SMBH) therein. Most of the observed energy is released in an accretion disk of inspiralling gas surrounding the SMBH. An enormous amount of fueling material, up to several tens solar masses per year, is expected to be transported inwards and consumed in the end. However, basic questions remain unanswered as to whether and how the accretion disks are supplied with external gas, since no disk-feeding inflow has hitherto been observed clearly. Here we report the discovery of highly redshifted broad absorption lines arising from neutral hydrogen and helium atoms in a small sample of quasars. Their absorption troughs show a broad range of Doppler velocities from zero extending continuously inward up to as high as ∼ 5, 000 km s−1, comparable to the free-fall speeds close to the SMBH and constraining the fastest in-falling gas to be within 104 gravitational radii. We thus see through streams of cold gas moving with a radially inward velocity component that spans an immense gradient—a result of gravitational acceleration by the central SMBH. Extensive photo-ionization modeling for the archetypical object SDSS J103516.20+142200.6 indicates the inflowing gas to be dense, thick and moderately ionized, with a characteristic distance to the SMBH of ∼ 1, 000 gravitational radii, possibly overlapping or close to the outer accretion disk. Our results present the first compelling evidence for the long-sought inflow directly feeding quasars’ accretion disks with external materials, likely originating from the dusty torus at a parsec scale. Our approach provides a new tool to probe the bulk of the so far elusive fueling inflows in quasars. Their studies may help address some of the fundamental questions concerning accretion physics, the onset and sustainment of quasar activity, and the SMBH growth at centers of most galaxies. Copyright © 2019,

关键词： Galaxies

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