RAS_WEB (Page 4,567)

A Search for Water Vapor Plumes on Europa using SOFIA. (arXiv:1901.00086v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sparks_W/0/1/0/all/0/1">William Sparks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richter_M/0/1/0/all/0/1">M. Richter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+deWitt_C/0/1/0/all/0/1">C. deWitt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montiel_E/0/1/0/all/0/1">E. Montiel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Russo_N/0/1/0/all/0/1">N. Dello Russo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grunsfeld_J/0/1/0/all/0/1">J. Grunsfeld</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGrath_M/0/1/0/all/0/1">M. A. McGrath</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_H/0/1/0/all/0/1">H. Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hand_K/0/1/0/all/0/1">K.P. Hand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergeron_E/0/1/0/all/0/1">E. Bergeron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reach_W/0/1/0/all/0/1">W. Reach</a> We present mid-infrared SOFIA/EXES spectroscopy of Europa, seeking direct evidence of the presence of water vapor arising from plumes venting from the surface of Europa. We place quantitatively useful upper limits on the strength of water vibrational-rotational emission lines. Conversion to water mass limits is dependent on the rotational temperature of the vapor. For low rotational temperature, theRead More →

Different contributions to space weather and space climate from different big solar active regions. (arXiv:1901.00116v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jiang_J/0/1/0/all/0/1">Jie Jiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Song_Q/0/1/0/all/0/1">Qiao Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">Jing-Xiu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baranyi_T/0/1/0/all/0/1">Tunde Baranyi</a> The purpose of this paper is to show that large active regions (ARs) with different magnetic configurations have different contributions to short-term and long-term variations of the Sun. As a case study, the complex $delta$-type AR 12673 and the simple $beta$-type AR 12674 are investigated in detail. Since the axial dipole moment at cycle minimum determines the amplitude of the subsequent cycle and space climate, we have assimilated the individual observed magnetic configurations of these two ARsRead More →

Snakes on a Spaceship – An Overview of Python in Heliophysics. (arXiv:1901.00143v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Burrell_A/0/1/0/all/0/1">A.G. Burrell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halford_A/0/1/0/all/0/1">A. Halford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klenzing_J/0/1/0/all/0/1">J. Klenzing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stoneback_R/0/1/0/all/0/1">R. A. Stoneback</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morley_S/0/1/0/all/0/1">S. K. Morley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annex_A/0/1/0/all/0/1">A. M. Annex</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Laundal_K/0/1/0/all/0/1">K. M. Laundal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kellerman_A/0/1/0/all/0/1">A. C. Kellerman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stansby_D/0/1/0/all/0/1">D. Stansby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ma_J/0/1/0/all/0/1">J. Ma</a> Computational analysis has become ubiquitous within the heliophysics community. However, community standards for peer-review of codes and analysis have lagged behind these developments. This absence has contributed to the reproducibility crisis, where inadequate analysis descriptions and loss of scientific data have made scientific studies difficult or impossible to replicate. The heliophysics community has responded to this challengeRead More →

Cherenkov light imaging in astroparticle physics. (arXiv:1901.00146v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_U/0/1/0/all/0/1">U.F. Katz</a> (Erlangen Centre for Astroparticle Physics, Friedrich-Alexander University Erlangen-N&#xfc;rnberg) Cherenkov light induced by fast charged particles in transparent dielectric media such as air or water is exploited by a variety of experimental techniques to detect and measure extraterrestrial particles impinging on Earth. A selection of detection principles is discussed and corresponding experiments are presented together with breakthrough-results they achieved. Some future developments are highlighted. Cherenkov light induced by fast charged particles in transparent dielectric media such as air or water is exploited by a variety of experimental techniques to detect and measure extraterrestrial particles impingingRead More →

Puzzles of the cosmic ray anisotropy. (arXiv:1901.00160v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Erlykin_A/0/1/0/all/0/1">Anatoly Erlykin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Machavariani_S/0/1/0/all/0/1">Svetlana Machavariani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolfendale_A/0/1/0/all/0/1">Arnold Wolfendale</a> We discuss three of the known puzzles of the cosmic ray anisotropy in the PeV and sub-PeV energy region. They are: (1) the so called inverse anisotropy, (2) the irregularity in the energy dependence of the amplitude and phase of the first harmonic and (3) the contribution of the single source. We discuss three of the known puzzles of the cosmic ray anisotropy in the PeV and sub-PeV energy region. They are: (1) the so called inverse anisotropy, (2) the irregularity in the energy dependence of the amplitudeRead More →

The Peebles – Vilenkin quintessential inflation model resivited. (arXiv:1901.00167v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Haro_J/0/1/0/all/0/1">Jaume Haro</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Amoros_J/0/1/0/all/0/1">Jaume Amor&#xf3;s</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Pan_S/0/1/0/all/0/1">Supriya Pan</a> We review the well-known Peebles-Vilenkin (PV) quintessential inflation model and discuss its possible improvements in agreement with the recent observations. The improved PV model depends only on two parameters: the inflaton mass $m$, and another smaller mass $M$; where the latter has to be chosen in order to undertake that, at present time, the dark energy density of the universe is approximately about 70% of the total energy budget of the universe. The value of the inflaton mass $m$ is calculated using the observational value ofRead More →

On the mass of supernova progenitors: the role of the $^{12}$C$+^{12}$C reaction. (arXiv:1901.00173v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Straniero_O/0/1/0/all/0/1">Oscar Straniero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piersanti_L/0/1/0/all/0/1">Luciano Piersanti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dominguez_I/0/1/0/all/0/1">Inmaculata Dominguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tumino_A/0/1/0/all/0/1">Aurora Tumino</a> A precise knowledge of the masses of supernova progenitors is essential to answer various questions of modern astrophysics, such as those related to the dynamical and chemical evolution of Galaxies. In this paper we revise the upper bound for the mass of the progenitors of CO white dwarfs (mup) and the lower bound for the mass of the progenitors of normal type II supernovae (mups). In particular, we present new stellar models with mass between 7 and 10 msun,Read More →

The CARMA-NRO Orion Survey: The filamentary structure as seen in C$^{18}$O emission. (arXiv:1901.00176v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Suri_S/0/1/0/all/0/1">S. T. Suri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Monge_A/0/1/0/all/0/1">A. Sanchez-Monge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schilke_P/0/1/0/all/0/1">P. Schilke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clarke_S/0/1/0/all/0/1">S. D. Clarke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_R/0/1/0/all/0/1">R. J. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ossenkopf_Okada_V/0/1/0/all/0/1">V. Ossenkopf-Okada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klessen_R/0/1/0/all/0/1">R. Klessen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padoan_P/0/1/0/all/0/1">P. Padoan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Goldsmith_P/0/1/0/all/0/1">P. Goldsmith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arce_H/0/1/0/all/0/1">H. G. Arce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bally_J/0/1/0/all/0/1">J. Bally</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">J. M. Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginsburg_A/0/1/0/all/0/1">A. Ginsburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnstone_D/0/1/0/all/0/1">D. Johnstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kauffmann_J/0/1/0/all/0/1">J. Kauffmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kong_S/0/1/0/all/0/1">S. Kong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lis_D/0/1/0/all/0/1">D. C. Lis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mairs_S/0/1/0/all/0/1">S. Mairs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pillai_T/0/1/0/all/0/1">T. Pillai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pineda_J/0/1/0/all/0/1">J. E. Pineda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duarte_Cabral_A/0/1/0/all/0/1">A. Duarte-Cabral</a> We present an initial overview of the filamentary structure in the Orion A molecular cloud utilizing a high angular and velocityRead More →

Accounting for Incompleteness due to Transit Multiplicity in Kepler Planet Occurrence Rates. (arXiv:1901.00196v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zink_J/0/1/0/all/0/1">Jon K. Zink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christiansen_J/0/1/0/all/0/1">Jessie L. Christiansen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hansen_B/0/1/0/all/0/1">Bradley M. S. Hansen</a> We investigate the role that planet detection order plays in the Kepler planet detection pipeline. The Kepler pipeline typically detects planets in order of descending signal strength (MES). We find that the detectability of transits experiences an additional $5.5%$ and $15.9%$ efficiency loss, for periods $200$ days respectively, when detected after the strongest signal transit in a multiple-planet system. We provide a method for determining the transit probability for multiple-planet systems by marginalizing over the empirical Kepler dataset.Read More →

Simulations of radiation damage in spacecraft camera for ESA JUICE mission. (arXiv:1901.00205v1 [physics.space-ph]) <a href="http://arxiv.org/find/physics/1/au:+Xiao_H/0/1/0/all/0/1">Hualin Xiao</a>, <a href="http://arxiv.org/find/physics/1/au:+Hajdas_W/0/1/0/all/0/1">Wojtek Hajdas</a>, <a href="http://arxiv.org/find/physics/1/au:+Beauvivre_S/0/1/0/all/0/1">Stephane Beauvivre</a>, <a href="http://arxiv.org/find/physics/1/au:+Kraehenbuehl_D/0/1/0/all/0/1">Daniel Kraehenbuehl</a>, <a href="http://arxiv.org/find/physics/1/au:+Ziethe_R/0/1/0/all/0/1">Ruth Ziethe</a>, <a href="http://arxiv.org/find/physics/1/au:+Banerji_N/0/1/0/all/0/1">Nikhil Banerji</a> The JUpiter ICy moons Explorer (JUICE) is an ESA interplanetary spacecraft being developed to perform detailed investigations of the Jupiter system and three of its icy moons: Europa, Callisto and Ganymede. The emphasis will be given on Ganymede as a small planetary body to be studied as a potential habitat. The spacecraft is set for launch in 2022 and would reach Jupiter in 2030. Two identical optical cameras are proposed for the mission toRead More →

The Evolution of Massive Helium Stars Including Mass Loss. (arXiv:1901.00215v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Woosley_S/0/1/0/all/0/1">S. E. Woosley</a> The evolution of helium stars with initial masses in the range 1.6 to 120 Msun is studied, including the effects of mass loss by winds. It is assumed that these stars are formed in binary systems when their expanding hydrogenic envelopes are promptly lost at helium ignition. Significant differences are found with single star evolution, chiefly because the helium core loses mass during helium burning rather than gaining it from hydrogen shell burning. Consequently presupernova stars for a given initial mass function have considerably smaller mass when they die andRead More →

Breezing through the space environment of Barnard’s Star b. (arXiv:1901.00219v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Alvarado_Gomez_J/0/1/0/all/0/1">Juli&#xe1;n D. Alvarado-G&#xf3;mez</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Garraffo_C/0/1/0/all/0/1">Cecilia Garraffo</a> (2,1), <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_J/0/1/0/all/0/1">Jeremy J. Drake</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Brown_B/0/1/0/all/0/1">Benjamin P. Brown</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Oishi_J/0/1/0/all/0/1">Jeffrey S. Oishi</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Moschou_S/0/1/0/all/0/1">Sofia P. Moschou</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Cohen_O/0/1/0/all/0/1">Ofer Cohen</a> (5) ((1) Center for Astrophysics | Harvard &amp; Smithsonian, (2) Institute for Applied Computational Science, Harvard University (3) Department of Astrophysical and Planetary Sciences, Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder (4) Department of Physics and Astronomy, Bates College (5) University of Massachusetts at Lowell, Department of Physics &amp; Applied Physics) A physically realistic stellar wind model basedRead More →

Towards an anagraphical picture of high-energy Galactic neutrinos. (arXiv:1901.00223v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Marinelli_A/0/1/0/all/0/1">Antonio Marinelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grasso_D/0/1/0/all/0/1">Dario Grasso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ventura_S/0/1/0/all/0/1">Sofia Ventura</a> The TeV/PeV neutrino emission from our Galaxy is related to the distribution of cosmic-ray accelerators, their maximal energy of injection as well as the propagation of injected particles and their interaction with molecular gas. Interesting upper limits on the diffuse hadronic emission from the whole Galaxy, massive molecular clouds and Fermi Bubbles were set in the last years thanks to the IceCube and ANTARES as well as HAWC and Fermi-LAT observations. On the other hand no evidence of Galactic point-like excess has been observed up toRead More →

Period variations and long-term cyclic changes in the light curve for the very short-period K-type contact binary YZ Phe. (arXiv:1901.00237v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sarotsakulchai_T/0/1/0/all/0/1">T. Sarotsakulchai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qian_S/0/1/0/all/0/1">S.-B. Qian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soonthornthum_B/0/1/0/all/0/1">B. Soonthornthum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_X/0/1/0/all/0/1">X. Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">J. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_L/0/1/0/all/0/1">L.-J. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichart_D/0/1/0/all/0/1">D. E. Reichart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haislip_J/0/1/0/all/0/1">J. B. Haislip</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kouprianov_V/0/1/0/all/0/1">V. V. Kouprianov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poshyachinda_S/0/1/0/all/0/1">S. Poshyachinda</a> YZ Phe is a very short-period contact binary (Sp.= K2 V) with an orbital period of 0.2347 days near the short period limit (0.22,d). Here we present the complete light curves in $VRI$ bands, which photometric data were obtained with the 0.61-m reflector of PROMPT-8 at CTIO in Chile during JuneRead More →

The relation between outburst rate and orbital period in low-mass X-ray binary transients. (arXiv:1901.00239v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_J/0/1/0/all/0/1">Jie Lin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_Z/0/1/0/all/0/1">Zhen Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_Z/0/1/0/all/0/1">Zhanwen Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yu_W/0/1/0/all/0/1">Wenfei Yu</a> We have investigated the outburst properties of low-mass X-ray binary transients (LMXBTs) based on a comprehensive study of the outbursts observed in the past few decades. The outburst rates were estimated based on the X-ray monitoring data from Swift/BAT, RXTE/ASM and MAXI, and previous reports in the literature. We found that almost all LMXBTs with the orbital period below $sim$12 hr showed only one outburst in these observations. There are systematic difference in the outburst rate between long-periodRead More →

WALLABY Early Science – II. The NGC 7232 galaxy group. (arXiv:1901.00241v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_Waddell_K/0/1/0/all/0/1">K. Lee-Waddell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koribalski_B/0/1/0/all/0/1">B.S. Koribalski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Westmeier_T/0/1/0/all/0/1">T. Westmeier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elagali_A/0/1/0/all/0/1">A. Elagali</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+For_B/0/1/0/all/0/1">B.-Q. For</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kleiner_D/0/1/0/all/0/1">D. Kleiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madrid_J/0/1/0/all/0/1">J.P. Madrid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Popping_A/0/1/0/all/0/1">A. Popping</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reynolds_T/0/1/0/all/0/1">T.N. Reynolds</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rhee_J/0/1/0/all/0/1">J. Rhee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serra_P/0/1/0/all/0/1">P. Serra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shao_L/0/1/0/all/0/1">L. Shao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Staveley_Smith_L/0/1/0/all/0/1">L. Staveley-Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_J/0/1/0/all/0/1">J. Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Whiting_M/0/1/0/all/0/1">M.T. Whiting</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wong_O/0/1/0/all/0/1">O.I. Wong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allison_J/0/1/0/all/0/1">J.R. Allison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhandari_S/0/1/0/all/0/1">S. Bhandari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collier_J/0/1/0/all/0/1">J.D. Collier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heald_G/0/1/0/all/0/1">G. Heald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marvil_J/0/1/0/all/0/1">J. Marvil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ord_S/0/1/0/all/0/1">S.M. Ord</a> We report on neutral hydrogen (HI) observations of the NGC 7232 group with the Australian Square Kilometre Array Pathfinder (ASKAP). These observations were conducted as part ofRead More →

JCMT POL-2 and ALMA polarimetric observations of 6000-100 au scales in the protostar B335: linking magnetic field and gas kinematics in observations and MHD simulations. (arXiv:1901.00242v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yen_H/0/1/0/all/0/1">Hsi-Wei Yen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_B/0/1/0/all/0/1">Bo Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hsieh_I/0/1/0/all/0/1">I-Ta Hsieh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koch_P/0/1/0/all/0/1">Patrick Koch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krasnopolsky_R/0/1/0/all/0/1">Ruben Krasnopolsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_C/0/1/0/all/0/1">Chin-Fei Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Z/0/1/0/all/0/1">Zhi-Yun Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_S/0/1/0/all/0/1">Sheng-Yuan Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohashi_N/0/1/0/all/0/1">Nagayoshi Ohashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takakuwa_S/0/1/0/all/0/1">Shigehisa Takakuwa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tang_Y/0/1/0/all/0/1">Ya-Wen Tang</a> We present our analysis of the magnetic field structures from 6000 au to 100 au scales in the Class 0 protostar B335 inferred from our JCMT POL-2 observations and the ALMA archival polarimetric data. To interpret the observational results, we perform a series of (non-)idealRead More →