December 2020

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 →

A Bayesian interpretation of inconsistency measures in cosmology. (arXiv:1909.10991v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_W/0/1/0/all/0/1">Weikang Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishak_M/0/1/0/all/0/1">Mustapha Ishak</a> Measures of discordance between datasets have become an essential part of cosmological analyses. It is important to accurately evaluate the significance of such discordances when present. We propose here a Bayesian interpretation of inconsistency measures that can extract information about physical inconsistencies in the presence of data scatter. The new framework is based on the conditional probability distribution of the level of physical inconsistency given the obtained value of the measure. We use the index of inconsistency as a case study to illustrate the new interpretation framework, butRead More →

Shape-based Feature Engineering for Solar Flare Prediction. (arXiv:2012.14405v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Deshmukh_V/0/1/0/all/0/1">Varad Deshmukh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berger_T/0/1/0/all/0/1">Thomas Berger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meiss_J/0/1/0/all/0/1">James Meiss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bradley_E/0/1/0/all/0/1">Elizabeth Bradley</a> Solar flares are caused by magnetic eruptions in active regions (ARs) on the surface of the sun. These events can have significant impacts on human activity, many of which can be mitigated with enough advance warning from good forecasts. To date, machine learning-based flare-prediction methods have employed physics-based attributes of the AR images as features; more recently, there has been some work that uses features deduced automatically by deep learning methods (such as convolutional neural networks). We describe a suite of novel shape-based featuresRead More →

CMB lensing in “u$Lambda$CDM in the light of $H_0$ tension. (arXiv:2012.14377v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Moshafi_H/0/1/0/all/0/1">Hossein Moshafi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baghram_S/0/1/0/all/0/1">Shant Baghram</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khosravi_N/0/1/0/all/0/1">Nima Khosravi</a> The observed discrepancy of the Hubble parameter measurements in the local universe with the CMB data may indicate a new physics. It is vital to test the alternative models that reconcile the Hubble tension with other cosmological observations in this direction. The CMB lensing is a crucial observation that relates the early universe perturbations to the matter’s late time distribution. In this work, we study the prediction of the “u$Lambda$CDM as a probable solution for $H_0$ tension for CMB lensing. We show that thisRead More →

Impacts of dark matter on the curvature of the neutron star. (arXiv:2007.05382v2 [nucl-th] UPDATED) <a href="http://arxiv.org/find/nucl-th/1/au:+Das_H/0/1/0/all/0/1">H. C. Das</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Kumar_A/0/1/0/all/0/1">Ankit Kumar</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Kumar_B/0/1/0/all/0/1">Bharat Kumar</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Biswal_S/0/1/0/all/0/1">S. K. Biswal</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Patra_S/0/1/0/all/0/1">S. K. Patra</a> The effects of dark matter (DM) on the curvatures of the neutron star (NS) are examined by using the stiff and soft relativistic mean-field equation of states. The curvatures of the NSs are calculated with the variation of baryon density. Also, it is found that the radial variation of the different curvatures significantly affected by the presence of DM inside the NS. The effects of DM are less pronounced on the compactness ofRead More →

Physical insights from the spectrum of the radio halo in MACS J0717.5+3745. (arXiv:2012.14373v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rajpurohit_K/0/1/0/all/0/1">K. Rajpurohit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brunetti_G/0/1/0/all/0/1">G. Brunetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonafede_A/0/1/0/all/0/1">A. Bonafede</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weeren_R/0/1/0/all/0/1">R. J. van Weeren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botteon_A/0/1/0/all/0/1">A. Botteon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vazza_F/0/1/0/all/0/1">F. Vazza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoeft_M/0/1/0/all/0/1">M. Hoeft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riseley_C/0/1/0/all/0/1">C. J.Riseley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnassieux_E/0/1/0/all/0/1">E. Bonnassieux</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brienza_M/0/1/0/all/0/1">M. Brienza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forman_W/0/1/0/all/0/1">W. R. Forman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rottgering_H/0/1/0/all/0/1">H. J. A. R&#xf6;ttgering</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rajpurohit_A/0/1/0/all/0/1">A. S. Rajpurohit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Locatelli_N/0/1/0/all/0/1">N. Locatelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shimwell_T/0/1/0/all/0/1">T. W. Shimwell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cassano_R/0/1/0/all/0/1">R. Cassano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gennaro_G/0/1/0/all/0/1">G. Di Gennaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruggen_M/0/1/0/all/0/1">M. Br&#xfc;ggen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wittor_D/0/1/0/all/0/1">D. Wittor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drabent_A/0/1/0/all/0/1">A. Drabent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ignesti_A/0/1/0/all/0/1">A. Ignesti</a> We present new LOFAR observations of the massive merging galaxy cluster MACS J0717.5+3745. The cluster hosts the most powerful radioRead More →

The Atacama Cosmology Telescope: Detection of mm-wave transient sources. (arXiv:2012.14347v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Naess_S/0/1/0/all/0/1">Sigurd Naess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nick Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_J/0/1/0/all/0/1">J.Richard Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">Erminia Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_S/0/1/0/all/0/1">Steve K. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cothard_N/0/1/0/all/0/1">Nicholas F. Cothard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duell_C/0/1/0/all/0/1">Cody J. Duell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duivenvoorden_A/0/1/0/all/0/1">Adriaan J. Duivenvoorden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunkley_J/0/1/0/all/0/1">Jo Dunkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunner_R/0/1/0/all/0/1">Rolando D&#xfc;nner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallardo_P/0/1/0/all/0/1">Patricio A. Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gralla_M/0/1/0/all/0/1">Megan Gralla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guan_Y/0/1/0/all/0/1">Yilun Guan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halpern_M/0/1/0/all/0/1">Mark Halpern</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_J/0/1/0/all/0/1">J. Colin Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_M/0/1/0/all/0/1">Matt Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huffenberger_K/0/1/0/all/0/1">Kevin M. Huffenberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koopman_B/0/1/0/all/0/1">Brian J. Koopman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kosowsky_A/0/1/0/all/0/1">Arthur B. Kosowsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madhavacheril_M/0/1/0/all/0/1">Mathew S. Madhavacheril</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">Jeff McMahon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nati_F/0/1/0/all/0/1">Federico Nati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemack_M/0/1/0/all/0/1">Michael D. Niemack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Page_L/0/1/0/all/0/1">Lyman Page</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Partridge_B/0/1/0/all/0/1">Bruce Partridge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salatino_M/0/1/0/all/0/1">Maria Salatino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sehgal_N/0/1/0/all/0/1">NeelimaRead More →

Storms and the Depletion of Ammonia in Jupiter: II. Explaining the Juno Observations. (arXiv:2012.14316v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Guillot_T/0/1/0/all/0/1">Tristan Guillot</a> (LAGRANGE), <a href="http://arxiv.org/find/astro-ph/1/au:+Li_C/0/1/0/all/0/1">Cheng Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bolton_S/0/1/0/all/0/1">Scott Bolton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_S/0/1/0/all/0/1">Shannon Brown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ingersoll_A/0/1/0/all/0/1">Andrew Ingersoll</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janssen_M/0/1/0/all/0/1">Michael Janssen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levin_S/0/1/0/all/0/1">Steven Levin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lunine_J/0/1/0/all/0/1">Jonathan Lunine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orton_G/0/1/0/all/0/1">Glenn Orton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steffes_P/0/1/0/all/0/1">Paul Steffes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevenson_D/0/1/0/all/0/1">David Stevenson</a> Observations of Jupiter’s deep atmosphere by the Juno spacecraft have revealed several puzzling facts: The concentration of ammonia is variable down to pressures of tens of bars, and is strongly dependent on latitude. While most latitudes exhibit a low abundance, the Equatorial Zone of Jupiter has an abundance of ammonia that is high and nearly uniformRead More →

Tracing the formation history of giant planets in protoplanetary disks with Carbon, Oxygen, Nitrogen and Sulphur. (arXiv:2012.14315v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Turrini_D/0/1/0/all/0/1">Diego Turrini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schisano_E/0/1/0/all/0/1">Eugenio Schisano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fonte_S/0/1/0/all/0/1">Sergio Fonte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molinari_S/0/1/0/all/0/1">Sergio Molinari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Politi_R/0/1/0/all/0/1">Romolo Politi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fedele_D/0/1/0/all/0/1">Davide Fedele</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panic_O/0/1/0/all/0/1">Olja Panic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kama_M/0/1/0/all/0/1">Mihkel Kama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Changeat_Q/0/1/0/all/0/1">Quentin Changeat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tinetti_G/0/1/0/all/0/1">Giovanna Tinetti</a> The composition of giant planets is imprinted by their migration history and the compositional structure of their hosting disks. Studies in recent literature investigate how the abundances of C and O can constrain the formation pathways of giant planets forming within few tens of au from the star. New ALMA observations, however, suggest planet-forming regions possibly extendingRead More →

Avenues to new-physics searches in cosmic ray air showers. (arXiv:2012.14293v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Fischer_O/0/1/0/all/0/1">Oliver Fischer</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Reininghaus_M/0/1/0/all/0/1">Maximilian Reininghaus</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ulrich_R/0/1/0/all/0/1">Ralf Ulrich</a> Cosmic Rays (CR) impinging on the terrestrial atmosphere provide a viable opportunity to study new physics in hadron-nucleus collisions at energies covering many orders of magnitude, including a regime well beyond LHC energies. The permanent flux of primary CR can be used to estimate event rates for a given type of new physics scenario. As a step to estimate the potential for new-physics searches in CR-induced Extensive Air Showers (EAS), we here determine the total luminosity, including the contribution stemming from the cascade of secondariesRead More →