RAS_WEB (Page 2,437)

A variable ionized disk wind in the black-hole candidate EXO 1846-031. (arXiv:2010.14662v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Y/0/1/0/all/0/1">Yanan Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ji_L/0/1/0/all/0/1">Long Ji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_J/0/1/0/all/0/1">Javier A. Garcia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dauser_T/0/1/0/all/0/1">Thomas Dauser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendez_M/0/1/0/all/0/1">Mariano Mendez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mao_J/0/1/0/all/0/1">Junjie Mao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tao_L/0/1/0/all/0/1">L. Tao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altamirano_D/0/1/0/all/0/1">Diego Altamirano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maggi_P/0/1/0/all/0/1">Pierre Maggi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">S. N. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ge_M/0/1/0/all/0/1">M. Y. Ge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_L/0/1/0/all/0/1">L. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qu_J/0/1/0/all/0/1">J. L. Qu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">S. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ma_X/0/1/0/all/0/1">X. Ma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_F/0/1/0/all/0/1">F. J. Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_T/0/1/0/all/0/1">T. P. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_Y/0/1/0/all/0/1">Y. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_S/0/1/0/all/0/1">S. J. Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_Z/0/1/0/all/0/1">Z. Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tuo_Y/0/1/0/all/0/1">Y. L. Tuo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Song_L/0/1/0/all/0/1">L. M. Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Y/0/1/0/all/0/1">Y. P. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Y. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_C/0/1/0/all/0/1">C. Z. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bu_Q/0/1/0/all/0/1">Q. C. Bu</a>, <aRead More →

Interacting Dark Energy in a closed universe. (arXiv:2011.00283v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Valentino_E/0/1/0/all/0/1">Eleonora Di Valentino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melchiorri_A/0/1/0/all/0/1">Alessandro Melchiorri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mena_O/0/1/0/all/0/1">Olga Mena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pan_S/0/1/0/all/0/1">Supriya Pan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_W/0/1/0/all/0/1">Weiqiang Yang</a> Recent measurements of the Cosmic Microwave Anisotropies power spectra measured by the Planck satellite show a preference for a closed universe at more than $99 %$ Confidence Level. Such a scenario is however in disagreement with several low redshift observables, including luminosity distances of Type Ia Supernovae. Here we show that Interacting Dark Energy (IDE) models can ease the discrepancies between Planck and Supernovae Ia data in a closed Universe. Therefore IDE cosmologies remain as very appealing scenarios, asRead More →

Constraining the shear acceleration model for the X-ray emission of large-scale extragalactic jets. (arXiv:2011.03264v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Tavecchio_F/0/1/0/all/0/1">F. Tavecchio</a> The nature of the intense X-ray emission from powerful extragalactic jets at large ($>1$ kpc) scale is still debated. The scenario that invokes the inverse Compton scattering of the CMB by electrons is challenged by the lack of gamma-ray emission in the GeV band. An alternative assumes synchrotron emission by a distinct population of ultra-high energy electrons. Here we present a concrete attempt to apply this scenario, exploring the specific model in which the ultra-high energy electrons are accelerated in a shear layer surrounding the jet.Read More →

Extreme ultra-soft X-ray variability in an eROSITA observation of the Narrow-Line Seyfert 1 Galaxy 1H 0707-495. (arXiv:2011.03307v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Boller_T/0/1/0/all/0/1">Th. Boller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_T/0/1/0/all/0/1">T. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weber_P/0/1/0/all/0/1">P. Weber</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcodia_R/0/1/0/all/0/1">R. Arcodia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dauser_T/0/1/0/all/0/1">T. Dauser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilms_J/0/1/0/all/0/1">J. Wilms</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nandra_K/0/1/0/all/0/1">K. Nandra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buchner_J/0/1/0/all/0/1">J. Buchner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Merloni_A/0/1/0/all/0/1">A. Merloni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freyberg_M/0/1/0/all/0/1">M.J. Freyberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krumpe_M/0/1/0/all/0/1">M. Krumpe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Waddell_S/0/1/0/all/0/1">S. G. H. Waddell</a> The ultra-soft narrow-line Seyfert 1 galaxy 1H 0707-495 is a well-known and highly variable active galactic nucleus (AGN), with a complex, steep X-ray spectrum, and has been studied extensively with XMM-Newton. 1H 0707-495 was observed with the extended ROentgen Survey with an Imaging Telescope Array (eROSITA) aboard theRead More →

Sensitivity of future liquid argon dark matter search experiments to core-collapse supernova neutrinos. (arXiv:2011.07819v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Agnes_P/0/1/0/all/0/1">P. Agnes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albergo_S/0/1/0/all/0/1">S. Albergo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albuquerque_I/0/1/0/all/0/1">I. F. M. Albuquerque</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alexander_T/0/1/0/all/0/1">T. Alexander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alici_A/0/1/0/all/0/1">A. Alici</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alton_A/0/1/0/all/0/1">A. K. Alton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amaudruz_P/0/1/0/all/0/1">P. Amaudruz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcelli_S/0/1/0/all/0/1">S. Arcelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ave_M/0/1/0/all/0/1">M. Ave</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avetissov_I/0/1/0/all/0/1">I. Ch. Avetissov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avetisov_R/0/1/0/all/0/1">R. I. Avetisov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Azzolini_O/0/1/0/all/0/1">O. Azzolini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Back_H/0/1/0/all/0/1">H. O. Back</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balmforth_Z/0/1/0/all/0/1">Z. Balmforth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbarian_V/0/1/0/all/0/1">V. Barbarian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olmedo_A/0/1/0/all/0/1">A. Barrado Olmedo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barrillon_P/0/1/0/all/0/1">P. Barrillon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basco_A/0/1/0/all/0/1">A. Basco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batignani_G/0/1/0/all/0/1">G. Batignani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bondar_A/0/1/0/all/0/1">A. Bondar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonivento_W/0/1/0/all/0/1">W. M. Bonivento</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borisova_E/0/1/0/all/0/1">E. Borisova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bottino_B/0/1/0/all/0/1">B. Bottino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boulay_M/0/1/0/all/0/1">M. G. Boulay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buccino_G/0/1/0/all/0/1">G. Buccino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bussino_S/0/1/0/all/0/1">S. Bussino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busto_J/0/1/0/all/0/1">J.Read More →

Compressive Shack-Hartmann Wavefront Sensor based on Deep Neural Networks. (arXiv:2011.10241v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Jia_P/0/1/0/all/0/1">Peng Jia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ma_M/0/1/0/all/0/1">Mingyang Ma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_D/0/1/0/all/0/1">Dongmei Cai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_W/0/1/0/all/0/1">Weihua Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Juanjuan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">Can Li</a> The Shack-Hartmann wavefront sensor is widely used to measure aberrations induced by atmospheric turbulence in adaptive optics systems. However if there exists strong atmospheric turbulence or the brightness of guide stars is low, the accuracy of wavefront measurements will be affected. In this paper, we propose a compressive Shack-Hartmann wavefront sensing method. Instead of reconstructing wavefronts with slope measurements of all sub-apertures, our method reconstructs wavefronts with slope measurements of sub-apertures which have spot imagesRead More →

Production of axion-like particles from photon conversions in large-scale solar magnetic fields. (arXiv:2010.06601v2 [hep-ph] UPDATED) <a href="http://arxiv.org/find/hep-ph/1/au:+Guarini_E/0/1/0/all/0/1">Ersilia Guarini</a> (Bari Univ.), <a href="http://arxiv.org/find/hep-ph/1/au:+Carenza_P/0/1/0/all/0/1">Pierluca Carenza</a> (Bari Univ. &amp; INFN Bari), <a href="http://arxiv.org/find/hep-ph/1/au:+Galan_J/0/1/0/all/0/1">Javier Galan</a> (Zaragoza Univ.), <a href="http://arxiv.org/find/hep-ph/1/au:+Giannotti_M/0/1/0/all/0/1">Maurizio Giannotti</a> (Barry Univ.), <a href="http://arxiv.org/find/hep-ph/1/au:+Mirizzi_A/0/1/0/all/0/1">Alessandro Mirizzi</a> (Bari Univ. &amp; INFN Bari) The Sun is a well-studied astrophysical source of axion-like particles (ALPs), produced mainly through the Primakoff process. Moreover, in the Sun there exist large-scale magnetic fields that catalyze an additional ALP production via a coherent conversion of thermal photons. We study this contribution to the solar ALP emissivity, typically neglected in previous investigations. Furthermore, we discuss additional bounds onRead More →

Insight-HXMT Identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428. (arXiv:2005.11071v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">C.K. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_L/0/1/0/all/0/1">L. Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xiong_S/0/1/0/all/0/1">S.L. Xiong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ge_M/0/1/0/all/0/1">M.Y. Ge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">X.B. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_T/0/1/0/all/0/1">T.P. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_F/0/1/0/all/0/1">F.J. Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">S.N. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tuo_Y/0/1/0/all/0/1">Y.L. Tuo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nang_Y/0/1/0/all/0/1">Y. Nang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_B/0/1/0/all/0/1">B. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xiao_S/0/1/0/all/0/1">S. Xiao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Y. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Song_L/0/1/0/all/0/1">L.M. Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Y/0/1/0/all/0/1">Y.P. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_C/0/1/0/all/0/1">C.Z. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jia_S/0/1/0/all/0/1">S.M. Jia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cao_X/0/1/0/all/0/1">X.L. Cao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qu_J/0/1/0/all/0/1">J.L. Qu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">S. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gu_Y/0/1/0/all/0/1">Y.D. Gu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liao_J/0/1/0/all/0/1">J.Y. Liao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_X/0/1/0/all/0/1">X.F. Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tan_Y/0/1/0/all/0/1">Y. Tan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nie_J/0/1/0/all/0/1">J.Y. Nie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_H/0/1/0/all/0/1">H.S. Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_S/0/1/0/all/0/1">S.J. Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_Y/0/1/0/all/0/1">Y.G. Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luo_Q/0/1/0/all/0/1">Q. Luo</a>, <aRead More →

Analytic infinite derivative gravity, $R^2$-like inflation, quantum gravity and CMB. (arXiv:2005.09550v3 [hep-th] UPDATED) <a href="http://arxiv.org/find/hep-th/1/au:+Koshelev_A/0/1/0/all/0/1">Alexey S. Koshelev</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Kumar_K/0/1/0/all/0/1">K. Sravan Kumar</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Starobinsky_A/0/1/0/all/0/1">Alexei A. Starobinsky</a> Emergence of $R^2$ inflation which is the best fit framework for CMB observations till date comes from the attempts to attack the problem of quantization of gravity which in turn have resulted in the trace anomaly discovery. Further developments in trace anomaly and different frameworks aiming to construct quantum gravity indicate an inevitability of non-locality in fundamental physics at small time and length scales. A natural question would be to employ the $R^2$ inflation as a probe for signatures ofRead More →

Modeling the spectrum and composition of ultrahigh-energy cosmic rays with two populations of extragalactic sources. (arXiv:2004.07621v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Das_S/0/1/0/all/0/1">Saikat Das</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Razzaque_S/0/1/0/all/0/1">Soebur Razzaque</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_N/0/1/0/all/0/1">Nayantara Gupta</a> We fit the ultrahigh-energy cosmic-ray (UHECR, $Egtrsim0.1$ EeV) spectrum and composition data from the Pierre Auger Observatory at energies $Egtrsim5cdot10^{18}$ eV, i.e., beyond the ankle using two populations of astrophysical sources. One population, accelerating dominantly protons ($^1$H), extends up to the highest observed energies with maximum energy close to the GZK cutoff and injection spectral index near the Fermi acceleration model; while another population accelerates light-to-heavy nuclei ($^4$He, $^{14}$N, $^{28}$Si, $^{56}$Fe) with a relatively low rigidity cutoff andRead More →

Measuring black hole masses from tidal disruption events and testing the $M_{rm BH}-sigma_*$ relation. (arXiv:2002.02267v4 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_Z/0/1/0/all/0/1">Z.Q. Zhou</a> (PKU), <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_F/0/1/0/all/0/1">F.K. Liu</a> (PKU, KIAA), <a href="http://arxiv.org/find/astro-ph/1/au:+Komossa_S/0/1/0/all/0/1">S. Komossa</a> (MPIfR), <a href="http://arxiv.org/find/astro-ph/1/au:+Cao_R/0/1/0/all/0/1">R. Cao</a> (PKU), <a href="http://arxiv.org/find/astro-ph/1/au:+Ho_L/0/1/0/all/0/1">L.C. Ho</a> (KIAA, PKU), <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_X/0/1/0/all/0/1">Xian Chen</a> (PKU, KIAA), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_S/0/1/0/all/0/1">Shuo Li</a> (NAOC, PKU) Liu and collaborators recently proposed an elliptical accretion disk model for tidal disruption events (TDEs). They showed that the accretion disks of optical/UV TDEs are large and highly eccentric and suggested that the broad optical emission lines with complex and diverse profiles originate in the cool eccentric accretion disk of random inclination and orientation. In thisRead More →

Probing the interior physics of stars through asteroseismology. (arXiv:1912.12300v3 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Aerts_C/0/1/0/all/0/1">C. Aerts</a> Yearslong time series of high-precision brightness measurements have been assembled for thousands of stars with telescopes operating in space. Such data have allowed astronomers to measure the physics of stellar interiors via nonradial oscillations, opening a new avenue to study the stars in the Universe. Asteroseismology, the interpretation of the characteristics of oscillation modes in terms of the physical properties of the stellar interior, brought entirely new insights in how stars rotate and how they build up their chemistry throughout their evolution. Data-driven space asteroseismology delivered a drastic increase in theRead More →