RAS_WEB (Page 4,307)

Investigation of surface homogeneity of (3200) Phaethon. (arXiv:1812.01851v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_H/0/1/0/all/0/1">Hee-Jae Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_M/0/1/0/all/0/1">Myung-Jin Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_D/0/1/0/all/0/1">Dong-Heun Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moon_H/0/1/0/all/0/1">Hong-Kyu Moon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_Y/0/1/0/all/0/1">Young-Jun Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_C/0/1/0/all/0/1">Chun-Hwey Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_B/0/1/0/all/0/1">Byeong-Cheol Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yoshida_F/0/1/0/all/0/1">Fumi Yoshida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roh_D/0/1/0/all/0/1">Dong-Goo Roh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seo_H/0/1/0/all/0/1">Haingja Seo</a> Time-series multi-band photometry and spectrometry were performed in Nov.-Dec. 2017 to investigate the homogeneity of the surface of asteroid (3200) Phaethon. We found that Phaethon is a B-type asteroid, in agreement with previous studies, and that it shows no evidence for rotational color variation. The sub-solar latitude during our observation period was approximately 55 degree S, which corresponded to the southern hemisphere of Phaethon. Thus, weRead More →

Kinematics of Subclusters in Star Cluster Complexes: Imprint of their Parental Molecular Clouds. (arXiv:1812.01858v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fujii_M/0/1/0/all/0/1">M. S. Fujii</a> Star cluster complexes such as the Carina Nebula can have formed in turbulent giant molecular clouds. We perform a series of $N$-body simulations starting from subclustering initial conditions based on hydrodynamic simulations of turbulent molecular clouds. These simulations finally result in the formation of star cluster complexes consisting of several subclusters (clumps). We obtain the inter-clump velocity distribution, the size of the region, and the mass of the most massive cluster in our simulated complex and compare the results with observed ones (the Carina Nebula andRead More →

Constraints on $H_0$ from WMAP and baryon acoustic osillation measurements. (arXiv:1812.01877v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_X/0/1/0/all/0/1">Xue Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_Q/0/1/0/all/0/1">Qing-Guo Huang</a> We report the constraints of $H_0$ obtained from Wilkinson Microwave Anisotropy Probe (WMAP) combined with the latest baryonic acoustic oscillations (BAO) measurements. We use the BAO measurements from the 6dF Galaxy Survey (6dFGS), the SDSS DR7 main galaxies sample (MGS), the BOSS DR12 galaxies and the eBOSS DR14 quasars. Adding the recent BAO measurements to the cosmic microwave background (CMB) data from WMAP, we constrain cosmological parameters $Omega_m=0.298pm0.005$, $H_0=68.36^{+0.53}_{-0.52}$ km s$^{-1}$ Mpc$^{-1}$, $sigma_8=0.8170^{+0.0159}_{-0.0175}$ in a spatially flat $Lambda$ cold dark matter ($Lambda$CDM) model, and $Omega_m=0.302pm0.008$, $H_0=67.63pm1.30$ kmRead More →

On slow solar wind with high Alfv’enicity: from composition and microphysics to spectral properties. (arXiv:1812.01899v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+DAmicis_R/0/1/0/all/0/1">Raffaella D&#x27;Amicis</a>, <a href="http://arxiv.org/find/physics/1/au:+Matteini_L/0/1/0/all/0/1">Lorenzo Matteini</a>, <a href="http://arxiv.org/find/physics/1/au:+Bruno_R/0/1/0/all/0/1">Roberto Bruno</a> Alfv’enic fluctuations are very common features in the solar wind and are found especially within the main portion of fast wind streams while the slow wind usually is less Alfv’enic and more variable. In general, fast and slow wind show many differences which span from the large scale structure to small scale phenomena including also a different turbulent behaviour. Recent studies, however, have shown that even slow wind can be sometimes highly Alfv’enic with fluctuations as large as those ofRead More →

A distributed data warehouse system for astroparticle physics. (arXiv:1812.01906v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nguyen_M/0/1/0/all/0/1">Minh-Duc Nguyen</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kryukov_A/0/1/0/all/0/1">Alexander Kryukov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dubenskaya_J/0/1/0/all/0/1">Julia Dubenskaya</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Korosteleva_E/0/1/0/all/0/1">Elena Korosteleva</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Polyakov_S/0/1/0/all/0/1">Stanislav Polyakov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Postnikov_E/0/1/0/all/0/1">Evgeny Postnikov</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Bychkov_I/0/1/0/all/0/1">Igor Bychkov</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Mikhailov_A/0/1/0/all/0/1">Andrey Mikhailov</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Shigarov_A/0/1/0/all/0/1">Alexey Shigarov</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Fedorov_O/0/1/0/all/0/1">Oleg Fedorov</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Kazarina_Y/0/1/0/all/0/1">Yulia Kazarina</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Shipilov_D/0/1/0/all/0/1">Dmitry Shipilov</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhurov_D/0/1/0/all/0/1">Dmitry Zhurov</a> (3) ((1) Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics, (2) Matrosov Institute for System Dynamics and Control Theory, Siberian Branch of Russian Academy of Sciences, (3) Applied Physics Institute, Irkutsk State University) A distributed data warehouse system is one of the actualRead More →

Evolution of spectral and temporal properties of MAXI~J1836-194 during 2011 outburst. (arXiv:1812.01918v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jana_A/0/1/0/all/0/1">Arghajit Jana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Debnath_D/0/1/0/all/0/1">Dipak Debnath</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chakrabarti_S/0/1/0/all/0/1">Sandip K. Chakrabarti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mondal_S/0/1/0/all/0/1">Santanu Mondal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molla_A/0/1/0/all/0/1">Aslam Ali Molla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_D/0/1/0/all/0/1">Debjit Chatterjee</a> We study transient Galatic black hole candidate MAXI~J1836-194 during its 2011 outburst using RXTE/PCA archival data. 2.5-25~keV spectra are fitted with Two Component Advective Flow (TCAF) model fits file as an additive table local model in XSPEC. From TCAF model spectral fits, physical parameters such as Keplerian disk rate, sub-Keplerian halo rate, shock location and compression ratio are extracted directly for better understanding of accretion processes around the BHC during this outburst.Read More →

Formation and Evolution of Primordial Black Hole Binaries in the Early Universe. (arXiv:1812.01930v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Raidal_M/0/1/0/all/0/1">Martti Raidal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spethmann_C/0/1/0/all/0/1">Christian Spethmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaskonen_V/0/1/0/all/0/1">Ville Vaskonen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Veermae_H/0/1/0/all/0/1">Hardi Veerm&#xe4;e</a> The abundance of primordial black holes (PBHs) in the mass range $0.1 – 10^3 M_odot$ can potentially be tested by gravitational wave observations due to the large merger rate of PBH binaries formed in the early universe. To put the estimates of the latter on a firmer footing, we first derive analytical PBH merger rate for the general mass function considering only initial configurations that give a conservative result. We then study the formation and evolution of PBH binariesRead More →

Cosmic ray transport and radiative processes in nuclei of starburst galaxies. (arXiv:1812.01996v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Peretti_E/0/1/0/all/0/1">Enrico Peretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blasi_P/0/1/0/all/0/1">Pasquale Blasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aharonian_F/0/1/0/all/0/1">Felix Aharonian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morlino_G/0/1/0/all/0/1">Giovanni Morlino</a> The high rate of star formation and supernova explosions of starburst galaxies make them interesting sources of high energy radiation. Depending upon the level of turbulence present in the their interstellar medium, the bulk of cosmic rays produced inside starburst galaxies may lose most of their energy before escaping, thereby making these sources behave as calorimeters, at least up to some maximum energy. Contrary to previous studies, here we investigate in detail the conditions under which cosmic ray confinement mayRead More →

ANAIS-112 sensitivity in the search for dark matter annual modulation. (arXiv:1812.02000v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Coarasa_I/0/1/0/all/0/1">I. Coarasa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amare_J/0/1/0/all/0/1">J. Amar&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cebrian_S/0/1/0/all/0/1">S. Cebri&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuesta_C/0/1/0/all/0/1">C. Cuesta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_E/0/1/0/all/0/1">E. Garc&#xed;a</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martinez_M/0/1/0/all/0/1">M. Mart&#xed;nez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olivan_M/0/1/0/all/0/1">M.A. Oliv&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ortigoza_Y/0/1/0/all/0/1">Y. Ortigoza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Solorzano_A/0/1/0/all/0/1">A. Ortiz de Sol&#xf3;rzano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puimedon_J/0/1/0/all/0/1">J. Puimed&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salinas_A/0/1/0/all/0/1">A. Salinas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarsa_M/0/1/0/all/0/1">M.L. Sarsa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villar_P/0/1/0/all/0/1">P. Villar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villar_J/0/1/0/all/0/1">J.A. Villar</a> The annual modulation measured by the DAMA/LIBRA experiment can be explained by the interaction of dark matter WIMPs in NaI(Tl) scintillator detectors. Other experiments, with different targets or techniques, exclude the region of parameters singled out by DAMA/LIBRA, but the comparison of their results relies on several hypotheses regardingRead More →

Equation of state effects in core-collapse supernovae. (arXiv:1812.02002v1 [nucl-th]) <a href="http://arxiv.org/find/nucl-th/1/au:+Yasin_H/0/1/0/all/0/1">Hannah Yasin</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Schafer_S/0/1/0/all/0/1">Sabrina Sch&#xe4;fer</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Arcones_A/0/1/0/all/0/1">Almudena Arcones</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Schwenk_A/0/1/0/all/0/1">Achim Schwenk</a> We investigate the impact of different properties of the nuclear equation of state in core-collapse supernovae, with a focus on the proto-neutron-star contraction and its impact on the shock evolution. To this end, we introduce a range of equations of state that vary the nucleon effective mass, incompressibility, symmetry energy, and nuclear saturation point. This allows us to point to the different effects in changing these properties from the Lattimer and Swesty to the Shen et al. equations of state, the two most commonlyRead More →

Frequency-Dependent Template Profiles for High Precision Pulsar Timing. (arXiv:1812.02006v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pennucci_T/0/1/0/all/0/1">Timothy T. Pennucci</a> Pulsar timing experiments require high fidelity template profiles in order to minimize the biases in pulse time-of-arrival (TOA) measurements and their uncertainties. Efforts to acquire more precise TOAs given fixed effective area of telescopes, finite receiver noise, and limited integration time have led pulsar astronomers to the solution of implementing ultra-wideband receivers. This solution, however, has run up against the problem that pulse profile shapes evolve with frequency, which raises the question of how to properly measure and analyze TOAs obtained using template-matching methods. This paper proposes a new method forRead More →

Starspot activity of HD 199178 – Doppler images from 1994–2017. (arXiv:1812.02013v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hackman_T/0/1/0/all/0/1">Thomas Hackman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilyin_I/0/1/0/all/0/1">Iya Ilyin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lehtinen_J/0/1/0/all/0/1">Jyri J. Lehtinen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kochukhov_O/0/1/0/all/0/1">Oleg Kochukhov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kapyla_M/0/1/0/all/0/1">Maarit J. K&#xe4;pyl&#xe4;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piskunov_N/0/1/0/all/0/1">Nikolai Piskunov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Willamo_T/0/1/0/all/0/1">Teemu Willamo</a> Context. Studying spots of late-type stars is crucial for distinguishing between the various proposed dynamo mechanisms believed to be the main cause of starspot activity. For this research it is important to collect long enough time series of observations to unravel both long and short-term spot evolution. Doppler imaging is a very efficient method to study spots of stars, that cannot be angularly resolved. Aims. High-resolution spectral observations during 1994–2017Read More →

Evolutionary models of cold and low-mass planets: Cooling curves, magnitudes, and detectability. (arXiv:1812.02027v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Linder_E/0/1/0/all/0/1">Esther F. Linder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mordasini_C/0/1/0/all/0/1">Christoph Mordasini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molliere_P/0/1/0/all/0/1">Paul Molliere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marleau_G/0/1/0/all/0/1">Gabriel-Dominique Marleau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malik_M/0/1/0/all/0/1">Matej Malik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quanz_S/0/1/0/all/0/1">Sascha P. Quanz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_M/0/1/0/all/0/1">Michael R. Meyer</a> Future instruments like NIRCam and MIRI on JWST or METIS at the ELT will be able to image exoplanets that are too faint for current direct imaging instruments. Evolutionary models predicting the planetary intrinsic luminosity as a function of time have traditionally concentrated on gas-dominated giant planets. We extend these cooling curves to Saturnian and Neptunian planets. We simulate the cooling of isolated core-dominated and gas giantRead More →

TASI Lectures on Indirect Searches For Dark Matter. (arXiv:1812.02029v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Hooper_D/0/1/0/all/0/1">Dan Hooper</a> In these lectures, I describe a variety of efforts to identify or constrain the identity of dark matter by detecting the annihilation or decay products of these particles, or their effects. After reviewing the motivation for indirect searches, I discuss what we have learned about dark matter from observations of gamma rays, cosmic rays and neutrinos, as well as the cosmic microwave background. Measurements such as these have been used to significantly constrain a wide range of thermal relic dark matter candidates, in particular those with masses below a few hundred GeV.Read More →

The Relationship between Precipitation and Aerosol: Evidence from Satellite Observation. (arXiv:1812.02036v1 [physics.ao-ph]) <a href="http://arxiv.org/find/physics/1/au:+Fan_C/0/1/0/all/0/1">Chongxing Fan</a>, <a href="http://arxiv.org/find/physics/1/au:+Fan_Y/0/1/0/all/0/1">Yaqi Fan</a>, <a href="http://arxiv.org/find/physics/1/au:+Wu_P/0/1/0/all/0/1">Peipei Wu</a>, <a href="http://arxiv.org/find/physics/1/au:+Ding_M/0/1/0/all/0/1">Maiqi Ding</a> The interaction of aerosol-cloud-precipitation has an important impact on the global climate. The understanding of this issue is related to the uncertainty of climate change prediction. The traditional indirect effect of aerosols suggests that when the number of aerosols increases, it will act to suppress precipitation. However, recent studies on satellite observations have found that aerosols are positively correlated with precipitation, which is contrary to conventional views. This study attempts to use the A-Train satellite product to verify the correlation betweenRead More →

Formation of massive black holes via collisions and accretion. (arXiv:1812.02052v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Schleicher_D/0/1/0/all/0/1">D.R.G. Schleicher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fellhauer_M/0/1/0/all/0/1">M.A. Fellhauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boekholt_T/0/1/0/all/0/1">T. Boekholt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reinoso_B/0/1/0/all/0/1">B. Reinoso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">R.S. Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vergara_M/0/1/0/all/0/1">M.Z.C. Vergara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seguel_P/0/1/0/all/0/1">P.J. Alister Seguel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bovino_S/0/1/0/all/0/1">S. Bovino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olave_C/0/1/0/all/0/1">C. Olave</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_V/0/1/0/all/0/1">V.B. D&#xed;az</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fibla_P/0/1/0/all/0/1">P. Fibla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riaz_R/0/1/0/all/0/1">R. Riaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bandyopadhyay_B/0/1/0/all/0/1">B. Bandyopadhyay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_Perez_R/0/1/0/all/0/1">R.I. San Martin-Perez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamponi_J/0/1/0/all/0/1">J. Zamponi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haemmerle_L/0/1/0/all/0/1">L. Haemmerle</a> To explain the observed population of supermassive black holes at z~7, very massive seed black holes or, alternatively, super-Eddington scenarios are needed to reach final masses of the order of 10^9 solar masses. A popular explanation for massive seeds has been the direct collapseRead More →

Characterizing and Improving the Data Reduction Pipeline for the Keck OSIRIS Integral Field Spectrograph. (arXiv:1812.02053v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lockhart_K/0/1/0/all/0/1">Kelly E. Lockhart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Do_T/0/1/0/all/0/1">Tuan Do</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Larkin_J/0/1/0/all/0/1">James E. Larkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehle_A/0/1/0/all/0/1">Anna Boehle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campbell_R/0/1/0/all/0/1">Randy D. Campbell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chappell_S/0/1/0/all/0/1">Samantha Chappell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chu_D/0/1/0/all/0/1">Devin Chu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciurlo_A/0/1/0/all/0/1">Anna Ciurlo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cosens_M/0/1/0/all/0/1">Maren Cosens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fitzgerald_M/0/1/0/all/0/1">Michael P. Fitzgerald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghez_A/0/1/0/all/0/1">Andrea Ghez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_J/0/1/0/all/0/1">Jessica R. Lu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lyke_J/0/1/0/all/0/1">Jim E. Lyke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mieda_E/0/1/0/all/0/1">Etsuko Mieda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rudy_A/0/1/0/all/0/1">Alexander R. Rudy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vayner_A/0/1/0/all/0/1">Andrey Vayner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Walth_G/0/1/0/all/0/1">Gregory Walth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wright_S/0/1/0/all/0/1">Shelley A. Wright</a> OSIRIS is a near-infrared (1.0–2.4 $mu$m) integral field spectrograph operating behind the adaptive optics system at Keck Observatory, and is one of the first lenslet-based integral fieldRead More →

Magnetic wind-driven accretion in dwarf novae. (arXiv:1812.02076v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Scepi_N/0/1/0/all/0/1">Nicolas Scepi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dubus_G/0/1/0/all/0/1">Guillaume Dubus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lesur_G/0/1/0/all/0/1">Geoffroy Lesur</a> Dwarf novae (DNe) and X-ray binaries exhibit outbursts thought to be due to a thermal-viscous instability in the accretion disk. The disk instability model (DIM) assumes that accretion is driven by turbulent transport, customarily attributed to the magneto-rotational instability (MRI). Recent results point out that MRI turbulence alone fails to reproduce the light curves of DNe. We aim to study the impact of wind-driven accretion on the light curves of DNe. Local and global simulations show that magneto-hydrodynamic winds are present when a magnetic field threads the disk,Read More →

Unresolved Gamma-Ray Sky through its Angular Power Spectrum. (arXiv:1812.02079v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Ackermann_M/0/1/0/all/0/1">M. Ackermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ajello_M/0/1/0/all/0/1">M. Ajello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldini_L/0/1/0/all/0/1">L. Baldini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ballet_J/0/1/0/all/0/1">J. Ballet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbiellini_G/0/1/0/all/0/1">G. Barbiellini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bastieri_D/0/1/0/all/0/1">D. Bastieri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellazzini_R/0/1/0/all/0/1">R. Bellazzini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bissaldi_E/0/1/0/all/0/1">E. Bissaldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blandford_R/0/1/0/all/0/1">R. D. Blandford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonino_R/0/1/0/all/0/1">R. Bonino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bottacini_E/0/1/0/all/0/1">E. Bottacini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bregeon_J/0/1/0/all/0/1">J. Bregeon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bruel_P/0/1/0/all/0/1">P. Bruel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buehler_R/0/1/0/all/0/1">R. Buehler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burns_E/0/1/0/all/0/1">E. Burns</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buson_S/0/1/0/all/0/1">S. Buson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cameron_R/0/1/0/all/0/1">R. A. Cameron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caputo_R/0/1/0/all/0/1">R. Caputo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caraveo_P/0/1/0/all/0/1">P. A. Caraveo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cavazzuti_E/0/1/0/all/0/1">E. Cavazzuti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_S/0/1/0/all/0/1">S. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiaro_G/0/1/0/all/0/1">G. Chiaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ciprini_S/0/1/0/all/0/1">S. Ciprini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costantin_D/0/1/0/all/0/1">D. Costantin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cuoco_A/0/1/0/all/0/1">A. Cuoco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cutini_S/0/1/0/all/0/1">S. Cutini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAmmando_F/0/1/0/all/0/1">F. D&#x27;Ammando</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luque_P/0/1/0/all/0/1">P. de la Torre Luque</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palma_F/0/1/0/all/0/1">F. de Palma</a>, <aRead More →

Cosmological constraints on sterile neutrino oscillations from Planck. (arXiv:1812.02102v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Knee_A/0/1/0/all/0/1">Alan M. Knee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Contreras_D/0/1/0/all/0/1">Dagoberto Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scott_D/0/1/0/all/0/1">Douglas Scott</a> Both particle physics experiments and cosmological surveys can constrain the properties of sterile neutrinos, but do so with different parameterizations that naturally use different prior information. We present joint constraints on the 3$+$1 sterile neutrino model oscillation parameters, $Delta m_{41}^2$ and $sin^22theta$, with uniform priors on those parameters using cosmological data from the Planck satellite. Two cases are considered, one where the sterile neutrino mixes with electron neutrinos solely, and another where the sterile neutrino mixes exclusively with muon neutrinos, allowing us to constrain theRead More →