RAS_WEB (Page 2,672)

Large-N Expansion and String Theory Out of Equilibrium. (arXiv:2008.11685v1 [hep-th]) <a href="http://arxiv.org/find/hep-th/1/au:+Horava_P/0/1/0/all/0/1">Petr Horava</a>, <a href="http://arxiv.org/find/hep-th/1/au:+Mogni_C/0/1/0/all/0/1">Christopher J. Mogni</a> We analyze the large-$N$ expansion of general non-equilibrium systems with fluctuating matrix degrees of freedom and $SU(N)$ symmetry, using the Schwinger-Keldysh formalism and its closed real-time contour with a forward and backward component. In equilibrium, the large-$N$ expansion of such systems leads to a sum over topologies of two-dimensional surfaces of increasing topological complexity, predicting the possibility of a dual description in terms of string theory. We extend this argument away from equilibrium, and study the universal features of the topological expansion in the dual string theory. WeRead More →

Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle. (arXiv:2008.11681v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Gunther_M/0/1/0/all/0/1">Maximilian N. G&#xfc;nther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berardo_D/0/1/0/all/0/1">David A. Berardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ducrot_E/0/1/0/all/0/1">Elsa Ducrot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murray_C/0/1/0/all/0/1">Catriona A. Murray</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stassun_K/0/1/0/all/0/1">Keivan G. Stassun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olah_K/0/1/0/all/0/1">Katalin Olah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouma_L/0/1/0/all/0/1">L.G. Bouma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rappaport_S/0/1/0/all/0/1">Saul Rappaport</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Winn_J/0/1/0/all/0/1">Joshua N. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feinstein_A/0/1/0/all/0/1">Adina D. Feinstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matthews_E/0/1/0/all/0/1">Elisabeth Matthews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sebastian_D/0/1/0/all/0/1">Daniel Sebastian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rackham_B/0/1/0/all/0/1">Benjamin V. Rackham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seli_B/0/1/0/all/0/1">B&#xe1;lint Seli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Triaud_A/0/1/0/all/0/1">Amaury H. M. J. Triaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gillen_E/0/1/0/all/0/1">Edward Gillen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levine_A/0/1/0/all/0/1">Alan M. Levine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Demory_B/0/1/0/all/0/1">Brice-Olivier Demory</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gillon_M/0/1/0/all/0/1">Micha&#xeb;l Gillon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Queloz_D/0/1/0/all/0/1">Didier Queloz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">George Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderspek_R/0/1/0/all/0/1">Roland K. Vanderspek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seager_S/0/1/0/all/0/1">Sara Seager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">David W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">Jon M. Jenkins</a>, <aRead More →

Probing galaxy evolution in massive clusters using ACT and DES: splashback as a cosmic clock. (arXiv:2008.11663v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_S/0/1/0/all/0/1">Susmita Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shin_T/0/1/0/all/0/1">Tae-hyeon Shin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jain_B/0/1/0/all/0/1">Bhuvnesh Jain</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:+Baxter_E/0/1/0/all/0/1">Eric Baxter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_C/0/1/0/all/0/1">Chihway Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wechsler_R/0/1/0/all/0/1">Risa H. Wechsler</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:+Bocquet_S/0/1/0/all/0/1">Sebastian Bocquet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeRose_J/0/1/0/all/0/1">Joseph DeRose</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:+Devlin_M/0/1/0/all/0/1">Mark Devlin</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:+Evrard_A/0/1/0/all/0/1">August E. Evrard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</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:+Hughes_J/0/1/0/all/0/1">John P. Hughes</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:+Lokken_M/0/1/0/all/0/1">Martine Lokken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacInnis_A/0/1/0/all/0/1">Amanda MacInnis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">Jeffrey McMahon</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:+Nati_F/0/1/0/all/0/1">Frederico Nati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Newburgh_L/0/1/0/all/0/1">Laura B. Newburgh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemack_M/0/1/0/all/0/1">Michael D. Niemack</a>,Read More →

Fear the Shadows of the Giants: On Secular Perturbations in Circumstellar Habitable Zones of Double Stars. (arXiv:2008.11651v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bazso_A/0/1/0/all/0/1">&#xc1;kos Bazs&#xf3;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pilat_Lohinger_E/0/1/0/all/0/1">Elke Pilat-Lohinger</a> After the detection of extrasolar planets in binary and multiple star systems questions arose about their dynamics and habitability. In this study we investigate a five-dimensional parameter space for wide binary stars with a massive planet beyond the habitable zone (HZ). Our aim is to reveal those orbital and physical parameter combinations that expose bodies in the primary star’s HZ to secular perturbations. Building upon an established semi-analytical model, we combine two separate analytical models into a new one to treatRead More →

Lithologic Controls on Silicate Weathering Regimes of Temperate Planets. (arXiv:2008.11620v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hakim_K/0/1/0/all/0/1">Kaustubh Hakim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bower_D/0/1/0/all/0/1">Dan J. Bower</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tian_M/0/1/0/all/0/1">Meng Tian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deitrick_R/0/1/0/all/0/1">Russell Deitrick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auclair_Desrotour_P/0/1/0/all/0/1">Pierre Auclair-Desrotour</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kitzmann_D/0/1/0/all/0/1">Daniel Kitzmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dorn_C/0/1/0/all/0/1">Caroline Dorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mezger_K/0/1/0/all/0/1">Klaus Mezger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heng_K/0/1/0/all/0/1">Kevin Heng</a> The atmospheres of temperate planets may be regulated by geochemical cycles. Silicate weathering provides essential negative feedback to the carbonate-silicate cycle (carbon cycle) to maintain temperate climates on Earth and possibly on Earth-sized temperate exoplanets. The intensity of weathering is normally attributed to the kinetics of weathering reactions of individual minerals. The implementation of a transport-controlled weathering model shows that when the CO$_2$ volume mixing ratioRead More →

How attractive is the isotropic attractor solution of axion-SU(2) inflation?. (arXiv:2003.01617v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Wolfson_I/0/1/0/all/0/1">Ira Wolfson</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Maleknejad_A/0/1/0/all/0/1">Azadeh Maleknejad</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Komatsu_E/0/1/0/all/0/1">Eiichiro Komatsu</a> The key to the phenomenological success of inflation models with axion and SU(2) gauge fields is the isotropic background of the SU(2) field. Previous studies showed that this isotropic background is an attractor solution during inflation starting from anisotropic (Bianchi Type I) spacetime; however, not all possible initial anisotropic parameter space was explored. In this paper, we explore more generic initial conditions without assuming the initial slow-roll dynamics. We find some initial anisotropic parameter space which does not lead to the isotropic background,Read More →

Physics-inspired deep learning to characterize the signal manifold of quasi-circular, spinning, non-precessing binary black hole mergers. (arXiv:2004.09524v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Khan_A/0/1/0/all/0/1">Asad Khan</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Huerta_E/0/1/0/all/0/1">E. A. Huerta</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Das_A/0/1/0/all/0/1">Arnav Das</a> The spin distribution of binary black hole mergers contains key information concerning the formation channels of these objects, and the astrophysical environments where they form, evolve and coalesce. To quantify the suitability of deep learning to characterize the signal manifold of quasi-circular, spinning, non-precessing binary black hole mergers, we introduce a modified version of WaveNet trained with a novel optimization scheme that incorporates general relativistic constraints of the spin properties of astrophysical black holes. The neuralRead More →

Deep learning the astrometric signature of dark matter substructure. (arXiv:2008.11577v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vattis_K/0/1/0/all/0/1">Kyriakos Vattis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toomey_M/0/1/0/all/0/1">Michael W. Toomey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koushiappas_S/0/1/0/all/0/1">Savvas M. Koushiappas</a> We study the application of machine learning techniques for the detection of the astrometric signature of dark matter substructure. In this proof of principle a population of dark matter subhalos in the Milky Way will act as lenses for sources of extragalactic origin such as quasars. We train ResNet-18, a state-of-the-art convolutional neural network to classify angular velocity maps of a population of quasars into lensed and no lensed classes. We show that an SKA -like survey with extended operational baseline can beRead More →

Electron Energization in Quasi-Parallel Shocks: Test-Particle-Electrons in a Proton Driven Turbulence. (arXiv:2007.06478v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Hanusch_A/0/1/0/all/0/1">Adrian Hanusch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liseykina_T/0/1/0/all/0/1">Tatyana Liseykina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malkov_M/0/1/0/all/0/1">Mikhail Malkov</a> In situ observations of energetic particles at the Earth’s bow-shock that are attainable by the satellite missions have long created the opinion that electrons are most efficiently accelerated in a quasi-perpendicular shock geometry. However, shocks that are deemed to be responsible for the production of cosmic ray electrons and their radiation from sources such as supernova remnants are much more powerful and larger than the Earth’s bow-shock. Their remote observations and in situ measurements at Saturn’s bow shock, suggest that electrons areRead More →

Neutrino decoupling including flavour oscillations and primordial nucleosynthesis. (arXiv:2008.01074v1 [hep-ph] CROSS LISTED) <a href="http://arxiv.org/find/hep-ph/1/au:+Froustey_J/0/1/0/all/0/1">Julien Froustey</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Pitrou_C/0/1/0/all/0/1">Cyril Pitrou</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Volpe_M/0/1/0/all/0/1">Maria Cristina Volpe</a> We revisit the decoupling of neutrinos in the early universe with flavour oscillations. We rederive the quantum kinetic equations which determine the neutrino evolution based on a BBGKY-like hierarchy, and include the full collision term. We focus on the case of zero chemical potential and solve these equations numerically. We also develop an approximate scheme based on the adiabatic evolution in the matter basis. In fact, the large difference between the oscillations and cosmological time scales allows to consider averaged flavour oscillations whichRead More →

New Constraints on Millicharged Particles from Cosmic-ray Production. (arXiv:2002.11732v2 [hep-ph] CROSS LISTED) <a href="http://arxiv.org/find/hep-ph/1/au:+Plestid_R/0/1/0/all/0/1">Ryan Plestid</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Takhistov_V/0/1/0/all/0/1">Volodymyr Takhistov</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Tsai_Y/0/1/0/all/0/1">Yu-Dai Tsai</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Bringmann_T/0/1/0/all/0/1">Torsten Bringmann</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Kusenko_A/0/1/0/all/0/1">Alexander Kusenko</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Pospelov_M/0/1/0/all/0/1">Maxim Pospelov</a> We study the production of exotic millicharged particles (MCPs) from cosmic ray-atmosphere collisions which constitutes a permanent MCP production source for all terrestrial experiments Our calculation of the MCP flux can be used to reinterpret existing limits from experiments such as MACRO and Majorana on an ambient flux of ionizing particles. Large-scale underground neutrino detectors are particularly favorable targets for the resulting MCPs. Using available data from the Super-K experiment, we set new limits onRead More →

A study of extragalactic planetary nebulae populations basedon spectroscopy. I. Data compilation and first findings. (arXiv:2008.11097v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Delgado_Inglada_G/0/1/0/all/0/1">Gloria Delgado-Inglada</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Rojas_J/0/1/0/all/0/1">Jorge Garc&#xed;a-Rojas</a> (2,3), <a href="http://arxiv.org/find/astro-ph/1/au:+Stasinska_G/0/1/0/all/0/1">Grazyna Stasi&#x144;ska</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Rechy_Garcia_J/0/1/0/all/0/1">Jackeline S. Rechy-Garc&#xed;a</a> (5) ((1) IA-UNAM, Mexico, (2) IAC, Spain, (3) ULL, Spain, (4) LUTH, Observatoire de Paris, France, (5) IRyA, UNAM, Mexico) We compile published spectroscopic data and [O III] magnitudes of almost 500 extragalactic planetary nebulae (PNe) in 13 galaxies of various masses and morphological types. This is the first paper of a series that aims to analyze the PN populations and their progenitors in these galaxies. Although the samples are notRead More →

Polarization of GRB Prompt Emission and its Application to POLAR’s Data. (arXiv:2008.10746v2 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Lan_M/0/1/0/all/0/1">Mi-Xiang Lan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_X/0/1/0/all/0/1">Xue-Feng Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_Z/0/1/0/all/0/1">Zi-Gao Dai</a> Synchrotron emission polarization is very sensitive to the magnetic field configuration. Recently, polarization of synchrotron emission with a mixed (SM) magnetic field in Gamma-ray burst (GRB) afterglow phase had been developed. Here, we apply these SM models to GRB prompt phase and compare their polarization properties with that of synchrotron emission in purely ordered (SO) magnetic field. We find that the polarization properties in a SM model are very similar to these in a corresponding SO model (e.g., synchrotron emission in aRead More →

Binary black hole spectroscopy: a toupee test of GW190814 and GW190412. (arXiv:2008.02248v2 [gr-qc] UPDATED) <a href="http://arxiv.org/find/gr-qc/1/au:+Capano_C/0/1/0/all/0/1">Collin D. Capano</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Nitz_A/0/1/0/all/0/1">Alexander H. Nitz</a> Gravitational waves provide a window to probe general relativity (GR) under extreme conditions. The recent observations of GW190412 and GW190814 are unique high-mass-ratio mergers that enable the observation of gravitational-wave harmonics beyond the dominant $ell = m = 2$ mode. Using these events, we search for physics beyond GR by allowing the source parameters measured from the sub-dominant harmonics to deviate from that of the dominant mode. All results are consistent with GR. We constrain the chirp mass as measured by the $ellRead More →

A Gravitational Redshift Measurement of the White Dwarf Mass-Radius Relation. (arXiv:2007.14517v2 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Chandra_V/0/1/0/all/0/1">Vedant Chandra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hwang_H/0/1/0/all/0/1">Hsiang-Chih Hwang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zakamska_N/0/1/0/all/0/1">Nadia L. Zakamska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_S/0/1/0/all/0/1">Sihao Cheng</a> The mass-radius relation of white dwarfs is largely determined by the equation of state of degenerate electrons, which causes the stellar radius to decrease as mass increases. Here we observationally measure this relation using the gravitational redshift effect, a prediction of general relativity that depends on the ratio between stellar mass and radius. Using observations of over three thousand white dwarfs from the Sloan Digital Sky Survey and the Gaia space observatory, we derive apparent radial velocities from absorptionRead More →

Ionized and atomic interstellar medium in the z = 6.003 quasar SDSS J2310+1855. (arXiv:2007.12339v2 [astro-ph.GA] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Li_J/0/1/0/all/0/1">Jianan Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_R/0/1/0/all/0/1">Ran Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cox_P/0/1/0/all/0/1">Pierre Cox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_Y/0/1/0/all/0/1">Yu Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walter_F/0/1/0/all/0/1">Fabian Walter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wagg_J/0/1/0/all/0/1">Jeff Wagg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">Karl M. Menten</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertoldi_F/0/1/0/all/0/1">Frank Bertoldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shao_Y/0/1/0/all/0/1">Yali Shao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venemans_B/0/1/0/all/0/1">Bram P. Venemans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Decarli_R/0/1/0/all/0/1">Roberto Decarli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riechers_D/0/1/0/all/0/1">Dominik Riechers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Neri_R/0/1/0/all/0/1">Roberto Neri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fan_X/0/1/0/all/0/1">Xiaohui Fan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omont_A/0/1/0/all/0/1">Alain Omont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Narayanan_D/0/1/0/all/0/1">Desika Narayanan</a> Observing the interstellar medium (ISM) in $z gtrsim 6$ quasars host galaxies is essential for understanding the co-evolution between the supermassive black holes and their hosts. To probe the gas physical conditions and search for imprints of Active GalacticRead More →

Salt, Hot Water, and Silicon Compounds Tracing Massive Twin Disks. (arXiv:2007.02962v4 [astro-ph.SR] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Tanaka_K/0/1/0/all/0/1">Kei E. I. Tanaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Y/0/1/0/all/0/1">Yichen Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirota_T/0/1/0/all/0/1">Tomoya Hirota</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sakai_N/0/1/0/all/0/1">Nami Sakai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Motogi_K/0/1/0/all/0/1">Kazuhito Motogi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomida_K/0/1/0/all/0/1">Kengo Tomida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tan_J/0/1/0/all/0/1">Jonathan C. Tan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosero_V/0/1/0/all/0/1">Viviana Rosero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Higuchi_A/0/1/0/all/0/1">Aya E. Higuchi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohashi_S/0/1/0/all/0/1">Satoshi Ohashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_M/0/1/0/all/0/1">Mengyao Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sugiyama_K/0/1/0/all/0/1">Koichiro Sugiyama</a> We report results of 0.05″-resolution observations toward the O-type proto-binary system IRAS 16547-4247 with the Atacama Large Millimeter/submillimeter Array (ALMA). We present dynamical and chemical structures of the circumbinary disk, circumstellar disks, outflows and jets, illustrated by multi-wavelength continuum and various molecular lines. In particular, we detect sodium chloride, silicon compounds, andRead More →

Dark matter nugget and new early dark energy from interacting neutrino: A promising solution to Hubble anomaly. (arXiv:2005.11889v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Gogoi_A/0/1/0/all/0/1">Antareep Gogoi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chanda_P/0/1/0/all/0/1">Prolay Chanda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Das_S/0/1/0/all/0/1">Subinoy Das</a> We present a novel scenario, in which light (mass $sim$ few rm{eV}) sterile neutrinos interact with a dynamical scalar field and for some duration prior to matter-radiation equality (MRE), the neutrino-scalar fluid behaves like early dark energy (EDE) as the field adiabatically stays at minimum of effective potential. In this scenario, when (sterile) neutrino becomes non-relativistic before MRE, we show that, neutrino-scalar fluid develops instability in perturbations followed by formation of neutrino-nuggets which redshifts like coldRead More →

Impact of Tides on the Potential for Exoplanets to Host Exomoons. (arXiv:2007.01487v2 [astro-ph.EP] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Tokadjian_A/0/1/0/all/0/1">Armen Tokadjian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_A/0/1/0/all/0/1">Anthony L. Piro</a> Exomoons may play an important role in determining the habitability of worlds outside of our solar system. They can stabilize conditions, alter the climate by breaking tidal locking with the parent star, drive tidal heating, and perhaps even host life themselves. However, the ability of an exoplanet to sustain an exomoon depends on complex tidal interactions. Motivated by this, we make use of simplified tidal lag models to follow the evolution of the separations and orbital and rotational periods in planet, star, and moonRead More →

The surface brightness of megaconstellation satellites trails on large telescopes. (arXiv:2007.00609v2 [astro-ph.IM] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Ragazzoni_R/0/1/0/all/0/1">Roberto Ragazzoni</a> On large telescopes trails of MegaConstellation’s satellites will appears significantly defocused because of their relatively short distance. Because of such effect their apparent surface brightness will be, under a range of conditions, almost constant during their apparent sweeping on the focal plane of such large facilities. A few simple relationships are worked out and discussed to show the apparent brightness of such trails, in order to evaluate their impact on operations of large optical ground based facilities. On large telescopes trails of MegaConstellation’s satellites will appears significantly defocused becauseRead More →