August 2021 (Page 60)

Jupiter’s X-ray aurora during UV dawn storms and injections as observed by XMM-Newton, Hubble, and Hisaki. (arXiv:2107.14712v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wibisono_A/0/1/0/all/0/1">A. D. Wibisono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Branduardi_Raymont_G/0/1/0/all/0/1">G. Branduardi-Raymont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunn_W/0/1/0/all/0/1">W. R. Dunn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kimura_T/0/1/0/all/0/1">T. Kimura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coates_A/0/1/0/all/0/1">A. J. Coates</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grodent_D/0/1/0/all/0/1">D. Grodent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yao_Z/0/1/0/all/0/1">Z. H. Yao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kita_H/0/1/0/all/0/1">H. Kita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_P/0/1/0/all/0/1">P. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gladstone_G/0/1/0/all/0/1">G. R. Gladstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonfond_B/0/1/0/all/0/1">B. Bonfond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haythornthwaite_R/0/1/0/all/0/1">R. P. Haythornthwaite</a> We present results from a multiwavelength observation of Jupiter’s northern aurorae, carried out simultaneously by XMM-Newton, the Hubble Space Telescope (HST), and the Hisaki satellite in September 2019. HST images captured dawn storms and injection events in the far ultraviolet aurora several times during theRead More →

Constraints on Multicomponent Dark Energy from Cosmological Observations. (arXiv:2006.07534v2 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_K/0/1/0/all/0/1">Ke Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_L/0/1/0/all/0/1">Lu Chen</a> Dark energy (DE) plays an important role in the expansion history of our universe. But we only got limited knowledge about its nature and properties after decades of study.In most numerical researches, DE is usually considered as a dynamical whole. Actually, multicomponent DE models can also explain the accelerating expansion of our universe, which is accepted theoretically but lack of numerical researches. We try to study the multicomponent DE models from observation by constructing $w_n$CDM models. The total energy density of DE is separated into $n$ ($n=2,3,5$) partsRead More →

Magnetic field screening in strong crossed electromagnetic fields. (arXiv:2002.11681v4 [astro-ph.HE] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Campion_S/0/1/0/all/0/1">S. Campion</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rueda_J/0/1/0/all/0/1">J. A.Rueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruffini_R/0/1/0/all/0/1">R. Ruffini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xue_S/0/1/0/all/0/1">S. S. Xue</a> We consider crossed electric and a magnetic fields $left(vec{B}=B,hat{z},~vec{E}=E,hat{y}right)$, with $E/B<1$, in presence of some initial number of $e^{pm}$ pairs. We do not discuss here the mechanism of generation of these initial pairs. The electric field accelerates the pairs to high-energies thereby radiating high-energy synchrotron photons. These photons interact with the magnetic field via magnetic pair production process (MPP), i.e. $gamma+Brightarrow e^{+}+e^{-}$, producing additional pairs. We here show that the motion of all the pairs around the magnetic field lines generatesRead More →

Primordial non-Gaussianity without tails — how to measure fNL with the bulk of the density PDF. (arXiv:1912.06621v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Friedrich_O/0/1/0/all/0/1">Oliver Friedrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uhlemann_C/0/1/0/all/0/1">Cora Uhlemann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villaescusa_Navarro_F/0/1/0/all/0/1">Francisco Villaescusa-Navarro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baldauf_T/0/1/0/all/0/1">Tobias Baldauf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manera_M/0/1/0/all/0/1">Marc Manera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nishimichi_T/0/1/0/all/0/1">Takahiro Nishimichi</a> We investigate the possibility to detect primordial non-Gaussianity by analysing the bulk of the probability distribution function (PDF) of late-time cosmic density fluctuations. For this purpose we devise a new method to predict the impact of general non-Gaussian initial conditions on the late-time density PDF. At redshift $z=1$ and for a smoothing scale of 30Mpc/$h$ our predictions agree with the high-resolution Quijote N-body simulations to $sim 0.2%$ precision.Read More →

Internal kinematics of GAIA eDR3 wide binaries. (arXiv:2107.14797v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_X/0/1/0/all/0/1">X. Hernandez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cookson_S/0/1/0/all/0/1">S. Cookson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortes_R/0/1/0/all/0/1">R. A. M. Cortes</a> Using the recent GAIA eDR3 catalogue we construct a sample of solar neighbourhood isolated wide binaries satisfying a series of strict signal-to-noise data cuts, exclusion of random association criteria and detailed colour-magnitude diagram selections, to minimise the presence of any kinematic contaminating effects having been discussed in the literature to date. Our final high-purity sample consists of 421 binary pairs within 130 pc of the sun and in all cases high-quality GAIA single-stellar fits for both components of each binary (final average RUWE values ofRead More →

Non-principal axis rotation in binary asteroid systems and how it weakens the BYORP effect. (arXiv:2107.14789v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Quillen_A/0/1/0/all/0/1">Alice C. Quillen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+LaBarca_A/0/1/0/all/0/1">Anthony LaBarca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">YuanYuan Chen</a> Using viscoelastic mass/spring model simulations, we explore tidal evolution and migration of compact binary asteroid systems. We find that after the secondary is captured into a spin-synchronous state, non-principal axis rotation in the secondary can be long-lived. The secondary’s long axis can remain approximately aligned along the vector connecting secondary to primary while the secondary rocks back and forth about its long axis. Inward orbital semi-major axis migration can also resonantly excite non-principal axis rotation. By estimating solar radiationRead More →

Optimization of EMCCD operating parameters for the acquisitionsystem of SPARC4. (arXiv:2107.14769v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardes_D/0/1/0/all/0/1">Denis Varise Bernardes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martioli_E/0/1/0/all/0/1">Eder Martioli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spadoti_D/0/1/0/all/0/1">Danilo Henrique Spadoti</a> We present the Optimization Method for the Electron Multiplying Charge-Coupled Devices (EMCCDs) of the Acquisition System of the SPARC4 (OMASS4). The OMASS4 uses as figures of merit the signal-to-noise ratio (SNR) and the acquisition rate (AR) as a function of the operation mode of the CCDs. Three different modes of optimization are included in the OMASS4: (1) optimization of SNR only; (2) optimization of AR only; and (3) optimization of both SNR and AR simultaneously. The first two modes calculate an analyticalRead More →

XMM-Newton spectrum of the radio-loud quasar 3C 215: slim accretion disk or SMBH binary?. (arXiv:2107.14753v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mei_A/0/1/0/all/0/1">Alessio Mei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tombesi_F/0/1/0/all/0/1">Francesco Tombesi</a> We want to explore the geometrical structure and mutual interactions of the innermost components of the broad line radio galaxy (BLRG) 3C 215, with particular interest in the accretion and ejection mechanisms involving the central supermassive black hole (SMBH). We compare these observational features with the ones of the RQ Seyfert 1 galaxies. Investigating their differences it is possible to understand more about the jet launching mechanisms, and why this phenomenon is efficient only in a small fraction of all the AGNs. UsingRead More →

Regularization of a scalar charged particle for generic orbits in Kerr spacetime. (arXiv:2107.14750v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Heffernan_A/0/1/0/all/0/1">Anna Heffernan</a> A scalar charged particle moving in a curved background spacetime will emit a field effecting its own motion; the resolving of this resulting motion is often referred to as the self-force problem. This also serves as a toy model for the astrophysically interesting compact body binaries, Extreme Mass Ratio Inspirals, targets for the future space-based gravitational wave detector, LISA. In the modelling of such systems, a point particle assumption leads to problematic singularities which need to be safely removed to solve for the motion of the particle regardlessRead More →

A Second Planet Transiting LTT~1445A and a Determination of the Masses of Both Worlds. (arXiv:2107.14737v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Winters_J/0/1/0/all/0/1">J.G. Winters</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Cloutier_R/0/1/0/all/0/1">R. Cloutier</a> (1,53), <a href="http://arxiv.org/find/astro-ph/1/au:+Medina_A/0/1/0/all/0/1">A.A. Medina</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Irwin_J/0/1/0/all/0/1">J.M. Irwin</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Charbonneau_D/0/1/0/all/0/1">D. Charbonneau</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Astudillo_Defru_N/0/1/0/all/0/1">N. Astudillo-Defru</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Bonfils_X/0/1/0/all/0/1">X. Bonfils</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Howard_A/0/1/0/all/0/1">A.W. Howard</a> (4), <a href="http://arxiv.org/find/astro-ph/1/au:+Isaacson_H/0/1/0/all/0/1">H. Isaacson</a> (5,6), <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_J/0/1/0/all/0/1">J.L. Bean</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Seifahrt_A/0/1/0/all/0/1">A. Seifahrt</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Teske_J/0/1/0/all/0/1">J.K. Teske</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Eastman_J/0/1/0/all/0/1">J.D. Eastman</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Twicken_J/0/1/0/all/0/1">J.D. Twicken</a> (9,10), <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_K/0/1/0/all/0/1">K.A. Collins</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Jensen_E/0/1/0/all/0/1">E.L.N. Jensen</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Quinn_S/0/1/0/all/0/1">S.N. Quinn</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Payne_M/0/1/0/all/0/1">M.J. Payne</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Kristiansen_M/0/1/0/all/0/1">M.H. Kristiansen</a> (12,13), <a href="http://arxiv.org/find/astro-ph/1/au:+Spencer_A/0/1/0/all/0/1">A. Spencer</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderburg_A/0/1/0/all/0/1">A. Vanderburg</a> (15), <a href="http://arxiv.org/find/astro-ph/1/au:+Zechmeister_M/0/1/0/all/0/1">M. Zechmeister</a> (16), <aRead More →

A More Precise Mass for GJ 1214 b and the Frequency of Multi-Planet Systems Around Mid-M Dwarfs. (arXiv:2107.14732v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Cloutier_R/0/1/0/all/0/1">Ryan Cloutier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Charbonneau_D/0/1/0/all/0/1">David Charbonneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deming_D/0/1/0/all/0/1">Drake Deming</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonfils_X/0/1/0/all/0/1">Xavier Bonfils</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Astudillo_Defru_N/0/1/0/all/0/1">Nicola Astudillo-Defru</a> We present an intensive effort to refine the mass and orbit of the enveloped terrestrial planet GJ 1214 b using 165 radial velocity (RV) measurements taken with the HARPS spectrograph over a period of ten years. We conduct a joint analysis of the RVs with archival Spitzer/IRAC transits and measure a planetary mass and radius of $8.17pm 0.43 M_{oplus}$ and $2.742^{+0.050}_{-0.053} R_{oplus}$. Assuming GJ 1214 b is an Earth-like core surroundedRead More →

Assessing the signatures imprinted by star-forming galaxies in the cosmic $gamma$-ray background. (arXiv:2107.14729v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Owen_E/0/1/0/all/0/1">Ellis R. Owen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_K/0/1/0/all/0/1">Khee-Gan Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kong_A/0/1/0/all/0/1">Albert K. H. Kong</a> In recent years, $gamma$-ray emission has been detected from star-forming galaxies (SFGs) in the local universe, including M82, NGC 253, Arp 220 and M33. The bulk of this emission is thought to be of hadronic origin, arising from the interactions of cosmic rays (CRs) with the interstellar medium of their host galaxy. Distant SFGs are presumably also bright in $gamma$-rays. Although they would not be resolvable as point sources, distant unresolved SFG populations contribute $gamma$-rays to the extra-galactic $gamma$-rayRead More →

The spatially offset quasar E1821+643: New evidence for gravitational recoil. (arXiv:2107.14711v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jadhav_Y/0/1/0/all/0/1">Yashashree Jadhav</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robinson_A/0/1/0/all/0/1">Andrew Robinson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almeyda_T/0/1/0/all/0/1">Triana Almeyda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Curran_R/0/1/0/all/0/1">Rachel Curran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marconi_A/0/1/0/all/0/1">Alessandro Marconi</a> A galaxy merger is expected to cause the formation of a supermassive black hole (SMBH) binary, which itself eventually coalesces through the anisotropic emission of gravitational waves. This may result in the merged SMBH receiving a recoil kick velocity ~100 – 1000 km/s, causing it to oscillate in the gravitational potential of the host galaxy. The luminous quasar E1821+643, identified as an SMBH recoil candidate via spectropolarimetry observations, shows Doppler shifting of the broad emission lines in directRead More →

Testing the equivalence principle on cosmological scales using the odd multipoles of galaxy cross-power spectrum and bispectrum. (arXiv:2011.05876v3 [astro-ph.CO] UPDATED) <a href="http://arxiv.org/find/astro-ph/1/au:+Umeh_O/0/1/0/all/0/1">Obinna Umeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koyama_K/0/1/0/all/0/1">Kazuya Koyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crittenden_R/0/1/0/all/0/1">Robert Crittenden</a> One of the cornerstones of general relativity is the equivalence principle. However, the validity of the equivalence principle has only been established on solar system scales for standard matter fields; this result cannot be assumed to hold for the non-standard matter fields that dominate the gravitational dynamics on cosmological scales. Here we show how the equivalence principle may be tested on cosmological scales for non-standard matter fields using the odd multipoles of the galaxy cross-power spectrumRead More →

Spectral and Energy Morphology Analysis Study of HAWC J2031+415. (arXiv:2107.14703v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Herzog_I/0/1/0/all/0/1">Ian Herzog</a> The Cygnus Cocoon region is a complex region containing an OB star cluster that is prominent in the TeV energy range. Located in this region is 3HWC J2031+415, a significant TeV gamma-ray source whose emission is possibly associated with 2 components, the Cygnus OB2 star cluster and a pulsar wind nebula (PWN). In this work, several modelling methods are presented to best describe the emission. These models disentangle emission believed to be from the Cocoon and isolate the component emitted by the probable PWN. I will present several spectral models toRead More →

Hourglass Magnetic Field from a Survey of Current Density Profiles. (arXiv:2107.14679v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bino_G/0/1/0/all/0/1">Gianfranco Bino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_S/0/1/0/all/0/1">Shantanu Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sharkawi_M/0/1/0/all/0/1">Mahmoud Sharkawi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Das_I/0/1/0/all/0/1">Indrani Das</a> Modelling the magnetic field in prestellar cores can serve as a useful tool for studying the initial conditions of star formation. The analytic hourglass model of Ewertowski and Basu (2013) provides a means to fit observed polarimetry measurements and extract useful information. The original model does not specify any radial distribution of the electric current density. Here, we perform a survey of possible centrally-peaked radial distributions of the current density, and numerically derive the full hourglass patterns. Since the vertical distributionRead More →

Thar she blows! How to inflate a wind-blown bubble. (arXiv:2107.14673v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pittard_J/0/1/0/all/0/1">J. M. Pittard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wareing_C/0/1/0/all/0/1">C. J. Wareing</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kupilas_M/0/1/0/all/0/1">M. M. Kupilas</a> Stellar winds are one of several ways that massive stars can affect the star formation process on local and galactic scales. In this paper we investigate the resolution requirements to inflate a stellar wind bubble in an external medium. We find that the radius of the wind injection region, $r_{rm inj}$, must be below a maximum value, $r_{rm inj,max}$, in order for a bubble to be produced, but must be significantly below this value if the bubble is to be modelled correctly.Read More →

Search for relativistic Magnetic Monopoles with ten years of the ANTARES detector data. (arXiv:2107.14660v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Boumaaza_J/0/1/0/all/0/1">J. Boumaaza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brunner_J/0/1/0/all/0/1">J. Brunner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moussa_A/0/1/0/all/0/1">A. Moussa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tayalati_Y/0/1/0/all/0/1">Y. Tayalati</a> (on behalf of the ANTARES Collaboration) The presented study is an updated search for magnetic monopoles using data taken with the ANTARES neutrino telescope over a period of 10 years (January 2008 to December 2017). In accordance with some grand unification theories, magnetic monopoles were created during the phase of symmetry breaking in the early Universe, and accelerated by galactic magnetic fields. As a consequence of their high energy, they could cross the Earth and emit a significantRead More →

Meeting the challenge of Open Science in KM3NeT. (arXiv:2107.14652v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Schnabel_J/0/1/0/all/0/1">Jutta Schnabel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kalaczynski_P/0/1/0/all/0/1">Piotr Kalaczy&#x144;ski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bozza_C/0/1/0/all/0/1">Cristiano Bozza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gal_T/0/1/0/all/0/1">Tamas Gal</a> In the upcoming decades, the KM3NeT detectors will produce valuable data that can be used in various scientific contexts from astro- and particle physics to environmental and Earth and Sea science. Based on the Open Science policy established by the KM3NeT Collaboration, several efforts to offer science-ready data, foster common analysis approaches and publish open source software are currently pursued. In this contribution, ongoing projects focusing on the exchange of high-level data and simulation derivatives, production of particle event simulations and establishment ofRead More →

Probing Neutrino Emission from X-ray Blazar Flares observed with Swift-XRT. (arXiv:2107.14632v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stathopoulos_S/0/1/0/all/0/1">Stamatios I. Stathopoulos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petropoulou_M/0/1/0/all/0/1">Maria Petropoulou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giommi_P/0/1/0/all/0/1">Paolo Giommi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vasilopoulos_G/0/1/0/all/0/1">Georgios Vasilopoulos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padovani_P/0/1/0/all/0/1">Paolo Padovani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mastichiadis_A/0/1/0/all/0/1">Apostolos Mastichiadis</a> Blazars are the most extreme subclass of active galactic nuclei with relativistic jets emerging from a super-massive black hole and forming a small angle with respect to our line of sight. Blazars are also known to be related to flaring activity as they exhibit large flux variations over a wide range of frequency and on multiple timescales, ranging from a few minutes to several months. The detection of a high-energy neutrino from the flaringRead More →