RAS_WEB (Page 4,066)

Polluted White Dwarfs: Mixing Regions and Diffusion Timescales. (arXiv:1812.09602v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bauer_E/0/1/0/all/0/1">Evan B. Bauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bildsten_L/0/1/0/all/0/1">Lars Bildsten</a> Many isolated white dwarfs (WDs) show spectral evidence of atmospheric metal pollution. Since heavy element sedimentation timescales are short, this most likely indicates ongoing accretion. Accreted metals encounter a variety of mixing processes at the WD surface: convection, gravitational sedimentation, overshoot, and thermohaline instability. We present MESA WD models that explore each of these processes and their implications for inferred accretion rates. We provide diffusion timescales for many individual metals, and we quantify the regimes in which thermohaline mixing dominates over gravitational sedimentation in setting the effective settlingRead More →

Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-Collapse Supernova Remnant G292.0+1.8. (arXiv:1812.09605v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bhalerao_J/0/1/0/all/0/1">Jayant Bhalerao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_S/0/1/0/all/0/1">Sangwook Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schenck_A/0/1/0/all/0/1">Andrew Schenck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Post_S/0/1/0/all/0/1">Seth Post</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_J/0/1/0/all/0/1">John P. Hughes</a> G292.0+1.8 (G292) is a young ($sim$3000 yr), Galactic textbook-type core-collapse supernova remnant (CCSNR). It is characterized by X-ray, optical and infrared emission from ejecta and circumstellar medium (CSM) features, and contains a pulsar (PSR J1124-5916) and pulsar wind nebula that have been observed in X-rays and radio. Previous studies have revealed a complex, dynamically evolving, oxygen-rich remnant, a striking relic from the explosion of a massive star. Here, using ourRead More →

A first search for a stochastic gravitational-wave background from ultralight bosons. (arXiv:1812.09622v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tsukada_L/0/1/0/all/0/1">Leo Tsukada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Callister_T/0/1/0/all/0/1">Thomas Callister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matas_A/0/1/0/all/0/1">Andrew Matas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyers_P/0/1/0/all/0/1">Patrick Meyers</a> In this work, we develop a Bayesian data analysis framework to study the SGWB from bosonic clouds using data from Advanced LIGO and Advanced Virgo, building on previous work by Brito et.al (2017). We further improve this model by adding a BH population of binary merger remnants. To assess the performance of our pipeline, we quantify the range of boson masses that can be constrained by Advanced LIGO and Advanced Virgo measurements at design sensitivity. Furthermore, we explore our capabilityRead More →

Constraining Theories of Polarized SiO Maser Transport: Multi-Epoch Analysis of a $pi/2$ Electric Vector Rotation Feature. (arXiv:1812.09631v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tobin_T/0/1/0/all/0/1">Taylor L. Tobin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kemball_A/0/1/0/all/0/1">Athol J. Kemball</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gray_M/0/1/0/all/0/1">Malcolm D. Gray</a> The detailed polarization mechanisms of SiO masers originating from the near circum-stellar environment of Asymptotic Giant Branch stars are not yet definitively known. Prevailing theories are broadly classified as either Zeeman or non-Zeeman in origin, the latter including effects such as anisotropic pumping or anisotropic resonant scattering. The predicted behavior of the linear and circular polarization fractions and electric vector position angle vary by theory. In particular, individual maser features that exhibit a rotation inRead More →

Median statistics estimate of the neutron lifetime. (arXiv:1812.09671v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Rajan_A/0/1/0/all/0/1">Ashwani Rajan</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Desai_S/0/1/0/all/0/1">Shantanu Desai</a> We construct the error distributions for the neutron lifetime using a subset of measurements compiled in the 2018 edition of Particle Data Group (PDG), as well as a few recent measurements, which are not yet included in PDG. We then checked the Gaussianity of the error distribution (using the techniques pioneered by Ratra and collaborators). We find that the error distributions using the weighted mean as well as median estimate are not consistent with a Gaussian distribution. We find that the Student’s $t$ and Cauchy distribution provide a better fitRead More →

Indication of nearby source signatures of cosmic rays from energy spectra and anisotropies. (arXiv:1812.09673v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_W/0/1/0/all/0/1">Wei Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guo_Y/0/1/0/all/0/1">Yi-Qing Guo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_Q/0/1/0/all/0/1">Qiang Yuan</a> The origin of Galactic cosmic rays (GCRs) remains a mystery after more than one century of their discovery. The diffusive propagation of charged particles in the turbulent Galactic magnetic field makes us unable to trace back to their acceleration sites. Nevertheless, nearby GCR source(s) may leave imprints on the locally measured energy spectra and the anisotropies of the arrival direction. In this work we propose a simple but natural description of the GCR production and propagation, within a two-zone disk-halo diffusionRead More →

Deep Drilling Fields for Solar System Science. (arXiv:1812.09705v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Trilling_D/0/1/0/all/0/1">David E. Trilling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bannister_M/0/1/0/all/0/1">Michele Bannister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuentes_C/0/1/0/all/0/1">Cesar Fuentes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerdes_D/0/1/0/all/0/1">David Gerdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mommert_M/0/1/0/all/0/1">Michael Mommert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwamb_M/0/1/0/all/0/1">Megan E. Schwamb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trujillo_C/0/1/0/all/0/1">Chad Trujillo</a> We propose an ecliptic Deep Drilling Field that will discover some 10,000~small and faint Kuiper Belt Objects (KBOs) — primitive rocky/icy bodies that orbit at the outside of our Solar System and uniquely record the processes of planetary system formation and evolution. The primary goals are to measure the KBO size and shape distributions down to 25~km, a size that probes both the early and ongoing evolution of this population. These goals canRead More →

The Local Group Dwarf Galaxies: The Star Formation Histories derived using the Long Period Variable stars. (arXiv:1812.09725v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Saremi_E/0/1/0/all/0/1">Elham Saremi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Javadi_A/0/1/0/all/0/1">Atefeh Javadi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loon_J/0/1/0/all/0/1">Jacco Th. van Loon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khosroshahi_H/0/1/0/all/0/1">Habib Khosroshahi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kh_S/0/1/0/all/0/1">Sara Rezaei Kh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golshan_R/0/1/0/all/0/1">Roya Hamedani Golshan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hashemi_S/0/1/0/all/0/1">Seyed Azim Hashemi</a> Dwarf galaxies in the Local Group (LG) represent a distinct as well as diverse family of tracers of the earliest phases of galaxy assembly and the processing resulting from galactic harassment. Their stellar populations can be resolved and used as probes of the evolution of their host galaxy. In this regard, we present the first reconstruction of the star formation historyRead More →

Fuzzy Dark Matter at Cosmic Dawn: New 21-cm Constraints. (arXiv:1812.09760v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nebrin_O/0/1/0/all/0/1">Olof Nebrin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghara_R/0/1/0/all/0/1">Raghunath Ghara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mellema_G/0/1/0/all/0/1">Garrelt Mellema</a> Potential small-scale discrepancies in the picture of galaxy formation painted by the $Lambda$CDM paradigm have led to considerations of modified dark matter models. One such dark matter model that has recently attracted much attention is fuzzy dark matter (FDM). In FDM models, the dark matter is envisaged to be an ultra-light scalar field with a particle mass $m_{rm FDM} sim 10^{-22} $ eV. This yields astronomically large de Broglie wavelengths which can suppress small-scale structure formation and give rise to the observed kpc-sized density coresRead More →

ALMA Observations of the massive molecular outflow G331.512-0.103 II: physical properties, kinematics, and geometry modeling. (arXiv:1812.09779v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hervias_Caimapo_C/0/1/0/all/0/1">Carlos Herv&#xed;as-Caimapo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Merello_M/0/1/0/all/0/1">Manuel Merello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bronfman_L/0/1/0/all/0/1">Leonardo Bronfman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+%5Cr%7BA%7Dke_Nyman_L/0/1/0/all/0/1">Lars &#xc5;ke-Nyman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garay_G/0/1/0/all/0/1">Guido Garay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lo_N/0/1/0/all/0/1">Nadia Lo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_N/0/1/0/all/0/1">Neal J. Evans II</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Calderon_C/0/1/0/all/0/1">Cristian L&#xf3;pez-Calder&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendoza_E/0/1/0/all/0/1">Edgar Mendoza</a> We present observations and analysis of the massive molecular outflow G331.512-0.103, obtained with ALMA band 7, continuing the work from Merello et al. (2013). Several lines were identified in the observed bandwidth, consisting of two groups: lines with narrow profiles, tracing the emission from the core ambient medium; and lines with broad velocity wings, tracing the outflow and shockedRead More →

Crater Density Predictions for New Horizons flyby target 2014 MU69. (arXiv:1812.09785v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Greenstreet_S/0/1/0/all/0/1">Sarah Greenstreet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gladman_B/0/1/0/all/0/1">Brett Gladman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKinnon_W/0/1/0/all/0/1">William McKinnon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kavelaars_J/0/1/0/all/0/1">JJ Kavelaars</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Singer_K/0/1/0/all/0/1">Kelsi Singer</a> In preparation for the Jan 1/2019 encounter between the New Horizons spacecraft and the Kuiper Belt object 2014 MU69, we provide estimates of the expected impact crater surface density on the Kuiper Belt object. Using the observed crater fields on Charon and Pluto down to the resolution limit of the 2015 New Horizons flyby of those bodies and estimates of the orbital distribution of the crater-forming projectiles, we calculate the number of craters per unit area formed asRead More →

Stress testing the dark energy equation of state imprint on supernova data. (arXiv:1812.09786v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Moews_B/0/1/0/all/0/1">Ben Moews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Souza_R/0/1/0/all/0/1">Rafael S. de Souza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ishida_E/0/1/0/all/0/1">Emille E. O. Ishida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Malz_A/0/1/0/all/0/1">Alex I. Malz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heneka_C/0/1/0/all/0/1">Caroline Heneka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vilalta_R/0/1/0/all/0/1">Ricardo Vilalta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zuntz_J/0/1/0/all/0/1">Joe Zuntz</a> (for the COIN Collaboration) This work determines the degree to which a standard Lambda-CDM analysis based on type Ia supernovae can identify deviations from a cosmological constant in the form of a redshift-dependent dark energy equation of state w(z). We introduce and apply a novel random curve generator to simulate instances of w(z) from constraint families with increasing distinction from a cosmological constant. After producingRead More →

Constraints on ion vs. electron heating by plasma turbulence at low beta. (arXiv:1812.09792v1 [physics.plasm-ph]) <a href="http://arxiv.org/find/physics/1/au:+Schekochihin_A/0/1/0/all/0/1">A. A. Schekochihin</a>, <a href="http://arxiv.org/find/physics/1/au:+Kawazura_Y/0/1/0/all/0/1">Y. Kawazura</a>, <a href="http://arxiv.org/find/physics/1/au:+Barnes_M/0/1/0/all/0/1">M. A. Barnes</a> (Oxford) It is shown that in low-beta plasmas, such as the solar corona, some instances of the solar wind, the aurora, inner regions of accretion discs, their coronae, and some laboratory plasmas, Alfvenic fluctuations produce no ion heating within the gyrokinetic approximation, i.e., as long as their amplitudes (at the Larmor scale) are small and their frequencies stay below the ion Larmor frequency. Thus, all low-frequency ion heating in such plasmas is due to compressive fluctuations: density perturbations and non-MaxwellianRead More →

Constraints on the curvature power spectrum from primordial black hole evaporation. (arXiv:1812.09807v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Dalianis_I/0/1/0/all/0/1">Ioannis Dalianis</a> We estimate the maximum allowed amplitude for the power spectrum of the primordial curvature perturbations, ${cal P_R}(k)$, on all scales from the absence of any detection signals of sub-solar mass black holes. In particular we analyze the constraints on the PBHs and we focus on the low mass limit where the Hawking radiation is expected to significantly influence the big bang observables, considering also different early cosmic histories. We derive the upper bounds for the variance of density perturbations, $sigma(M)$, for any possible reheating temperature as well as forRead More →

Comparing treatments of weak reactions with nuclei in simulations of core-collapse supernovae. (arXiv:1812.09811v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nagakura_H/0/1/0/all/0/1">Hiroki Nagakura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furusawa_S/0/1/0/all/0/1">Shun Furusawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Togashi_H/0/1/0/all/0/1">Hajime Togashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richers_S/0/1/0/all/0/1">Sherwood Richers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sumiyoshi_K/0/1/0/all/0/1">Kohsuke Sumiyoshi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yamada_S/0/1/0/all/0/1">Shoichi Yamada</a> We perform an extensive study of the influence of nuclear weak interactions on core-collapse supernovae (CCSNe), paying particular attention to consistency between nuclear abundances in the equation of state (EOS) and nuclear weak interactions. We compute properties of uniform matter based on the variational method. For inhomogeneous nuclear matter, we take a full ensemble of nuclei into account with various finite-density and thermal effects and directly use the nuclear abundances to compute nuclearRead More →

Thermal Sunyaev-Zel’dovich Effect in the IGM due to Primordial Magnetic Fields. (arXiv:1812.09813v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Minoda_T/0/1/0/all/0/1">Teppei Minoda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasegawa_K/0/1/0/all/0/1">Kenji Hasegawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tashiro_H/0/1/0/all/0/1">Hiroyuki Tashiro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ichiki_K/0/1/0/all/0/1">Kiyotomo Ichiki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sugiyama_N/0/1/0/all/0/1">Naoshi Sugiyama</a> In the present universe, magnetic fields exist with various strengths and on various scales. One possible origin of these cosmic magnetic fields is the primordial magnetic fields (PMFs) generated in the early universe. PMFs are considered to contribute to matter density evolution via Lorentz force and the thermal history of intergalactic medium (IGM) gas due to ambipolar diffusion. Therefore, information about PMFs should be included in the temperature anisotropy of the Cosmic Microwave Background through the thermalRead More →

Long-term X-ray variation of the colliding wind Wolf-Rayet binary WR 125. (arXiv:1812.09825v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Midooka_T/0/1/0/all/0/1">Takuya Midooka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sugawara_Y/0/1/0/all/0/1">Yasuharu Sugawara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ebisawa_K/0/1/0/all/0/1">Ken Ebisawa</a> WR 125 is considered as a Colliding Wind Wolf-rayet Binary (CWWB), from which the most recent infrared flux increase was reported between 1990 and 1993. We observed the object four times from November 2016 to May 2017 with Swift and XMM-Newton, and carried out a precise X-ray spectral study for the first time. There were hardly any changes of the fluxes and spectral shapes for half a year, and the absorption-corrected luminosity was 3.0e+33 erg/s in the 0.5 – 10.0 keV range atRead More →

A VLA-GMRT Look at 11 Powerful FR II Quasars. (arXiv:1812.09846v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Vaddi_S/0/1/0/all/0/1">S. Vaddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kharb_P/0/1/0/all/0/1">P. Kharb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daly_R/0/1/0/all/0/1">R.A. Daly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+ODea_C/0/1/0/all/0/1">C.P. O&#x27;Dea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baum_S/0/1/0/all/0/1">S.A. Baum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deo_D/0/1/0/all/0/1">D.K. Deo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbusca_T/0/1/0/all/0/1">T.C. Barbusca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Murali_C/0/1/0/all/0/1">C. Murali</a> We present results from 1.4 and 5 GHz observations at matched resolution with the Karl G. Jansky Very Large Array (VLA) of 11 powerful 3C FR II quasars. We examine the 11 quasars along with a sample of 13 narrow-line FR II radio galaxies and find that radio-loud unification largely holds but environmental effects cannot be ignored. The radio core prominence, largest linear size, and axial ratio parameter values indicateRead More →

Photometric Investigation of the Contact Binary GU Ori with High Metallicity. (arXiv:1812.09856v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_X/0/1/0/all/0/1">Xiao Zhou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qian_S/0/1/0/all/0/1">Shengbang Qian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soonthornthum_B/0/1/0/all/0/1">Boonrucksar Soonthornthum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poshyachinda_S/0/1/0/all/0/1">Saran Poshyachinda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_L/0/1/0/all/0/1">Li-Ying Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_N/0/1/0/all/0/1">Nian-Ping Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarotsakulchai_T/0/1/0/all/0/1">Thawicharat Sarotsakulchai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_X/0/1/0/all/0/1">Xiao-Hui Fang</a> GU Ori was observed with the 1m telescope at Yunnan Observatories in 2005. To determine its physical properties, the Wilson-Devinney program is used. The results reveal that GU Ori is a W-subtype shallow contact binary with a more massive but cooler star 2. The mass of its two component stars are estimated to be $M_1 = 0.45M_odot$, $M_2 = 1.05M_odot$. The O’Connell effect was reported to be negativeRead More →

A Quasi-periodic propagating wave and EUV waves excited simultaneously in a solar eruption event. (arXiv:1812.09858v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Miao_Y/0/1/0/all/0/1">Y. H. Miao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Y/0/1/0/all/0/1">Y. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shen_Y/0/1/0/all/0/1">Y. D. Shen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_H/0/1/0/all/0/1">H. B. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abidin_Z/0/1/0/all/0/1">Z. Z. Abidin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elmhamdi_A/0/1/0/all/0/1">A. Elmhamdi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kordi_A/0/1/0/all/0/1">A. S. Kordi</a> Quasi-periodic fast-propagating (QFP) magnetosonic waves and extreme ultraviolet (EUV) waves were proposed to be driven by solar flares and coronal mass ejections (CMEs), respectively. In this Letter, we present a detailed analysis of an interesting event in which we find that both QFP magnetosonic waves and EUV waves are excited simultaneously in one solar eruption event. The co-existence of the two wave phenomenaRead More →