RAS_WEB (Page 4,536)

Early Cosmological Evolution of Primordial Electromagnetic Fields. (arXiv:1903.02561v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_T/0/1/0/all/0/1">Takeshi Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sloth_M/0/1/0/all/0/1">Martin S. Sloth</a> It is usually assumed that when Weyl invariance is unbroken in the electromagnetic sector, the energy density of primordial magnetic fields will redshift as radiation. Here we show that primordial magnetic fields do not exhibit radiation-like redshifting in the presence of stronger electric fields, as a consequence of Faraday’s law of induction. In particular for the standard Maxwell theory, magnetic fields on super-horizon scales can redshift as $B^2 propto a^{-6} H^{-2}$, instead of the usually assumed $a^{-4}$. Taking into account this effect for inflationary magnetogenesis can correct previous estimatesRead More →

Planet-planet scattering as the source of the highest eccentricity exoplanets. (arXiv:1903.02564v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Carrera_D/0/1/0/all/0/1">Daniel Carrera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raymond_S/0/1/0/all/0/1">Sean R. Raymond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_M/0/1/0/all/0/1">Melvyn B. Davies</a> Most giant exoplanets discovered by radial velocity surveys have much higher eccentricities than those in the Solar System. The planet-planet scattering mechanism has been shown to match the broad eccentricity distribution, but the highest-eccentricity planets are often attributed to Kozai-Lidov oscillations induced by a stellar companion. Here we investigate whether the highly eccentric exoplanet population can be produced entirely by scattering. We ran 500 N-body simulations of closely packed giant planet systems that became unstable under their own mutual perturbations. We findRead More →

Using Torque to Understand Barred Galaxy Models. (arXiv:1903.02566v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Petersen_M/0/1/0/all/0/1">Michael S. Petersen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weinberg_M/0/1/0/all/0/1">Martin D. Weinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_N/0/1/0/all/0/1">Neal Katz</a> We present n-body simulations of barred galaxies to understand the dynamical mechanisms responsible for the evolution of the bar-disc-dark matter halo system. We find evidence for three distinct phases of barred galaxy evolution: assembly, secular growth, and steady-state equilibrium. Using an ensemble decomposition of the disc into orbital families, we track bar mass, geometry, and angular momentum through time and correlate the quantities with the phases of evolution. We follow the angular momentum transfer between particles and identify the dominant torque channels. We find thatRead More →

X-ray Observation of a Magnetized Hot Gas Outflow in the Galactic Center Region. (arXiv:1903.02571v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Nakashima_S/0/1/0/all/0/1">Shinya Nakashima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koyama_K/0/1/0/all/0/1">Katsuji Koyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Q/0/1/0/all/0/1">Q. Daniel Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Enokiya_R/0/1/0/all/0/1">Rei Enokiya</a> We report the discovery of a $1^circ$ scale X-ray plume in the northern Galactic Center (GC) region observed with Suzaku. The plume is located at ($l$, $b$) $sim$ ($0mbox{$.!!^circ$}2$, $0mbox{$.!!^circ$}6$), east of the radio lobe reported by previous studies. No significant X-ray excesses are found inside or to the west of the radio lobe. The spectrum of the plume exhibits strong emission lines from highly ionized Mg, Si, and S that is reproduced by a thin thermalRead More →

WASP-4b Arrived Early for the TESS Mission. (arXiv:1903.02573v1 [astro-ph.EP]) <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:+Winn_J/0/1/0/all/0/1">J. N. Winn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baxter_C/0/1/0/all/0/1">C. Baxter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhatti_W/0/1/0/all/0/1">W. Bhatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_F/0/1/0/all/0/1">F. Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Daylan_T/0/1/0/all/0/1">T. Daylan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desert_J/0/1/0/all/0/1">J.-M. D&#xe9;sert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_M/0/1/0/all/0/1">M. L. Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kane_S/0/1/0/all/0/1">S. R. Kane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stassun_K/0/1/0/all/0/1">K. G. Stassun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villasenor_J/0/1/0/all/0/1">J. Villasenor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricker_G/0/1/0/all/0/1">G. R. Ricker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanderspek_R/0/1/0/all/0/1">R. Vanderspek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Latham_D/0/1/0/all/0/1">D. W. Latham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seager_S/0/1/0/all/0/1">S. Seager</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jenkins_J/0/1/0/all/0/1">J. M. Jenkins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berta_Thompson_Z/0/1/0/all/0/1">Z. Berta-Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colon_K/0/1/0/all/0/1">K. Col&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fausnaugh_M/0/1/0/all/0/1">M. Fausnaugh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glidden_A/0/1/0/all/0/1">Ana Glidden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerrero_N/0/1/0/all/0/1">N. Guerrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_J/0/1/0/all/0/1">J. E. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Twicken_J/0/1/0/all/0/1">J. D. Twicken</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wohler_B/0/1/0/all/0/1">B. Wohler</a> The Transiting Exoplanet Survey Satellite (TESS) recently observed 18 transits of the hot JupiterRead More →

X-rays Studies of the Solar System. (arXiv:1903.02574v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Snios_B/0/1/0/all/0/1">Bradford Snios</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunn_W/0/1/0/all/0/1">William R. Dunn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lisse_C/0/1/0/all/0/1">Carey M. Lisse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Branduardi_Raymont_G/0/1/0/all/0/1">Graziella Branduardi-Raymont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dennerl_K/0/1/0/all/0/1">Konrad Dennerl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhardwaj_A/0/1/0/all/0/1">Anil Bhardwaj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gladstone_G/0/1/0/all/0/1">G. Randall Gladstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nulsen_S/0/1/0/all/0/1">Susan Nulsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bodewits_D/0/1/0/all/0/1">Dennis Bodewits</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jackman_C/0/1/0/all/0/1">Caitriona M. Jackman</a>, <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>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bunce_E/0/1/0/all/0/1">Emma J. Bunce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Combi_M/0/1/0/all/0/1">Michael R. Combi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cravens_T/0/1/0/all/0/1">Thomas E. Cravens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cumbee_R/0/1/0/all/0/1">Renata S. Cumbee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drake_J/0/1/0/all/0/1">Jeremy J. Drake</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elsner_R/0/1/0/all/0/1">Ronald F. Elsner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grodent_D/0/1/0/all/0/1">Denis Grodent</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_J/0/1/0/all/0/1">Jae Sub Hong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kharchenko_V/0/1/0/all/0/1">Vasili Kharchenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">Ralph P. Kraft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marler_J/0/1/0/all/0/1">Joan P. Marler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moschou_S/0/1/0/all/0/1">Sofia P. Moschou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mullen_P/0/1/0/all/0/1">Patrick D. Mullen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolk_S/0/1/0/all/0/1">Scott J. Wolk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yao_Z/0/1/0/all/0/1">Zhonghua Yao</a> X-ray observatoriesRead More →

Radio Emission from the unbound Debris of Tidal Disruption Events. (arXiv:1903.02575v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Yalinewich_A/0/1/0/all/0/1">Almog Yalinewich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steinberg_E/0/1/0/all/0/1">Elad Steinberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piran_T/0/1/0/all/0/1">Tsvi Piran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krolik_J/0/1/0/all/0/1">Julian H. Krolik</a> When a star gets too close to a supermassive black hole, it is torn apart by the tidal forces. Roughly half of the stellar mass becomes unbound and flies away at tremendous velocities. In this work we explore the idea that the shock produced by the interaction of the unbound debris with the ambient medium gives rise to the synchrotron radio emission observed in several TDEs. We use a moving mesh numerical simulation to study the evolution of the unboundRead More →

Helium Absorption at 1083 nm from Extended Exoplanet Atmospheres: Dependence on Stellar Radiation. (arXiv:1903.02576v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Oklopcic_A/0/1/0/all/0/1">Antonija Oklop&#x10d;i&#x107;</a> Strong absorption signatures in the helium line at 1083 nm have recently been detected in transmission spectra of several close-in exoplanets. This absorption line originates from neutral helium atoms in an excited, metastable 2$^3$S state. The population of helium atoms in this excited state is governed by the spectral shape and intensity of the incident stellar radiation field. We investigate what kind of stellar environments are most favorable for populating the metastable helium state in extended planetary atmospheres. Our results suggest that planets orbiting at close separationsRead More →

Segregation of Stellar-Mass Black Holes at the Galactic Center. (arXiv:1903.02578v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Emami_R/0/1/0/all/0/1">Razieh Emami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard University) We simulate the star cluster near the center of the Milky Way galaxy. Using the Fokker Planck approach we consider the time evolution of the density profile of stars and stellar mass black holes (BHs) for various initial profiles. BHs sink toward the center of the galaxy where they are swallowed by SgrA*. We show that the mass loss increases the mass of SgrA* by up to 20 % for shallow initial radial profile with a power-law slope $gamma = 0.8$, and BH mass of $40Read More →

Gravitational Waves from Stellar Mass Black Holes Around SgrA*. (arXiv:1903.02579v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Emami_R/0/1/0/all/0/1">Razieh Emami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a> (Harvard University) We consider the detectability of the gravitational wave (GW) signal from an orbiting stellar-mass black hole (BH) with a mass of order 40 $M_{odot}$ around Sgr A* at the center of the Milky Way galaxy. We simulate the sinking BHs to the center through dynamical friction and GW emission. We predict that LISA will detect of order 10 BHs at any given time with a signal-to-noise ratio $S/N > 10$. We consider the detectability of the gravitational wave (GW) signal from an orbiting stellar-mass black holeRead More →

Probing the Cosmological Evolution of Super-massive Black Holes using Tidal Disruption Flares. (arXiv:1903.02584v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pasham_D/0/1/0/all/0/1">Dheeraj R. Pasham</a> (MIT), <a href="http://arxiv.org/find/astro-ph/1/au:+Lin_D/0/1/0/all/0/1">Dacheng Lin</a> (University of New Hampshire), <a href="http://arxiv.org/find/astro-ph/1/au:+Saxton_R/0/1/0/all/0/1">Richard Saxton</a> (Telespazio-Vega), <a href="http://arxiv.org/find/astro-ph/1/au:+Jonker_P/0/1/0/all/0/1">Peter Jonker</a> (SRON), <a href="http://arxiv.org/find/astro-ph/1/au:+Kara_E/0/1/0/all/0/1">Erin Kara</a> (UMD), <a href="http://arxiv.org/find/astro-ph/1/au:+Stone_N/0/1/0/all/0/1">Nicholas Stone</a> (Columbia), <a href="http://arxiv.org/find/astro-ph/1/au:+Maksym_P/0/1/0/all/0/1">Peter Maksym</a> (Harvard), <a href="http://arxiv.org/find/astro-ph/1/au:+Auchettl_K/0/1/0/all/0/1">Katie Auchettl</a> (DARK) The question of how supermassive black holes (SMBHs) grow over cosmic time is a major puzzle in high-energy astrophysics. One promising approach to this problem is via the study of tidal disruption flares (TDFs). These are transient events resulting from the disruption of stars by quiescent supermassive black holes at centers of galaxies. A meter-classRead More →

A High-resolution SZ View of the Warm-Hot Universe. (arXiv:1903.02595v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagai_D/0/1/0/all/0/1">Daisuke Nagai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andreani_P/0/1/0/all/0/1">Paola Andreani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_M/0/1/0/all/0/1">Monique Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartlett_J/0/1/0/all/0/1">James Bartlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nicholas Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_K/0/1/0/all/0/1">Kaustuv Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulbul_E/0/1/0/all/0/1">Esra Bulbul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chluba_J/0/1/0/all/0/1">Jens Chluba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Churazov_E/0/1/0/all/0/1">Eugene Churazov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cicone_C/0/1/0/all/0/1">Claudia Cicone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">Abigail Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeNigris_N/0/1/0/all/0/1">Nat DeNigris</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:+Mascolo_L/0/1/0/all/0/1">Luca Di Mascolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dicker_S/0/1/0/all/0/1">Simon Dicker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaspari_M/0/1/0/all/0/1">Massimo Gaspari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golwala_S/0/1/0/all/0/1">Sunil Golwala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guglielmetti_F/0/1/0/all/0/1">Fabrizia Guglielmetti</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:+Klaassen_P/0/1/0/all/0/1">Pamela Klaassen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kitayama_T/0/1/0/all/0/1">Tetsu Kitayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kneissl_R/0/1/0/all/0/1">R&#xfc;diger Kneissl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">Kotaro Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Komatsu_E/0/1/0/all/0/1">Eiichiro Komatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacy_M/0/1/0/all/0/1">Mark Lacy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_B/0/1/0/all/0/1">Brian Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nyland_K/0/1/0/all/0/1">Kristina Nyland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_C/0/1/0/all/0/1">Charles Romero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sayers_J/0/1/0/all/0/1">Jack Sayers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sehgal_N/0/1/0/all/0/1">Neelima Sehgal</a>,Read More →

The survey of Planetary Nebulae in Andromeda (M31): I. Imaging the disk and halo with MegaCam@CFHT. (arXiv:1903.02597v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bhattacharya_S/0/1/0/all/0/1">Souradeep Bhattacharya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaboldi_M/0/1/0/all/0/1">Magda Arnaboldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartke_J/0/1/0/all/0/1">Johanna Hartke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerhard_O/0/1/0/all/0/1">Ortwin Gerhard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Comte_V/0/1/0/all/0/1">Valentin Comte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McConnachie_A/0/1/0/all/0/1">Alan McConnachie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harris_W/0/1/0/all/0/1">William E. Harris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caldwell_N/0/1/0/all/0/1">Nelson Caldwell</a> The Andromeda (M31) galaxy subtends nearly 100 sq. deg. on the sky, with severe contamination from the Milky Way halo stars whose surface density displays a steep gradient across the entire M31 field-of-view. Planetary Nebulae (PNe) are a population of stars firmly associated with M31, that are excellent tracers of light, chemistry and motion in galaxies. We present a 16 sq. deg.Read More →

An ALMA survey of the SCUBA-2 Cosmology Legacy Survey UKIDSS/UDS field: Source catalogue and properties. (arXiv:1903.02602v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Stach_S/0/1/0/all/0/1">S. M. Stach</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Dudzeviciute_U/0/1/0/all/0/1">U. Dudzevi&#x10d;i&#x16b;t&#x117;</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Smail_I/0/1/0/all/0/1">I. Smail</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Swinbank_A/0/1/0/all/0/1">A. M. Swinbank</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Geach_J/0/1/0/all/0/1">J. E. Geach</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Simpson_J/0/1/0/all/0/1">J. M. Simpson</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+An_F/0/1/0/all/0/1">F. X. An</a> (4 and 1), <a href="http://arxiv.org/find/astro-ph/1/au:+Almaini_O/0/1/0/all/0/1">O. Almaini</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Arumugam_V/0/1/0/all/0/1">V. Arumugam</a> (6 and 7), <a href="http://arxiv.org/find/astro-ph/1/au:+Blain_A/0/1/0/all/0/1">A. W. Blain</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Chapman_S/0/1/0/all/0/1">S. C. Chapman</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C. -C. Chen</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Conselice_C/0/1/0/all/0/1">C. J. Conselice</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Cooke_E/0/1/0/all/0/1">E. A. Cooke</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Coppin_K/0/1/0/all/0/1">K. E. K. Coppin</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_E/0/1/0/all/0/1">E. da Cunha</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Dunlop_J/0/1/0/all/0/1">J. S. Dunlop</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Farrah_D/0/1/0/all/0/1">D.Read More →

Constraining the evolution of stellar rotation using solar twins. (arXiv:1903.02630v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lorenzo_Oliveira_D/0/1/0/all/0/1">Diego Lorenzo-Oliveira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melendez_J/0/1/0/all/0/1">Jorge Mel&#xe9;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galarza_J/0/1/0/all/0/1">Jhon Yana Galarza</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ponte_G/0/1/0/all/0/1">Geisa Ponte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santos_L/0/1/0/all/0/1">Leonardo A. dos Santos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spina_L/0/1/0/all/0/1">Lorenzo Spina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bedell_M/0/1/0/all/0/1">Megan Bedell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_I/0/1/0/all/0/1">Iv&#xe1;n Ram&#xed;rez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_J/0/1/0/all/0/1">Jacob L. Bean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asplund_M/0/1/0/all/0/1">Martin Asplund</a> The stellar Rotation $vs.$ Age relation is commonly considered as a useful tool to derive reliable ages for Sun-like stars. However, in the light of kepler data, the presence of apparently old and fast rotators that do not obey the usual gyrochronology relations led to the hypothesis of weakened magnetic breaking in some stars. In this letter, we constrain theRead More →

Search strategies for long gravitational-wave transients: hidden Markov model tracking and seedless clustering. (arXiv:1903.02638v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Banagiri_S/0/1/0/all/0/1">Sharan Banagiri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_L/0/1/0/all/0/1">Ling Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_M/0/1/0/all/0/1">Michael W. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melatos_A/0/1/0/all/0/1">Andrew Melatos</a> A number of detections have been made in the past few years of gravitational waves from compact binary coalescences. While there exist well-understood waveform models for signals from compact binary coalescences, many sources of gravitational waves are not well modeled, including potential long-transient signals from a binary neutron star post-merger remnant. Searching for these sources requires robust detection algorithms that make minimal assumptions about any potential signals. In this paper, we compare two unmodeled search schemes forRead More →

Spin frequency evolution and pulse profile variations of the recently re-activated radio magnetar XTE J1810-197. (arXiv:1903.02660v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Levin_L/0/1/0/all/0/1">L. Levin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lyne_A/0/1/0/all/0/1">A. G. Lyne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desvignes_G/0/1/0/all/0/1">G. Desvignes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eatough_R/0/1/0/all/0/1">R. P. Eatough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Karuppusamy_R/0/1/0/all/0/1">R. Karuppusamy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kramer_M/0/1/0/all/0/1">M. Kramer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stappers_B/0/1/0/all/0/1">B. W. Stappers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weltevrede_P/0/1/0/all/0/1">P. Weltevrede</a> After spending almost a decade in a radio-quiet state, the Anomalous X-ray Pulsar XTE J1810-197 turned back on in early December 2018. We have observed this radio magnetar at 1.5 GHz with ~daily cadence since the first detection of radio re-activation on 8 December 2018. In this paper, we report on the current timing properties of XTE J1810-197 and find thatRead More →

Axion Dark Matter Detection with CMB Polarization. (arXiv:1903.02666v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Fedderke_M/0/1/0/all/0/1">Michael A. Fedderke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Graham_P/0/1/0/all/0/1">Peter W. Graham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rajendran_S/0/1/0/all/0/1">Surjeet Rajendran</a> We point out two ways to search for low-mass axion dark matter using cosmic microwave background (CMB) polarization measurements. These appear, in particular, to be some of the most promising ways to directly detect fuzzy dark matter. Axion dark matter causes rotation of the polarization of light passing through it. This gives rise to two novel phenomena in the CMB. First, the late-time oscillations of the axion field today cause the CMB polarization to oscillate in phase across the entire sky. Second, the early-time oscillationsRead More →

Resolving the MYSO binaries PDS 27 and PDS 37 with VLTI/PIONIER. (arXiv:1903.02667v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Koumpia_E/0/1/0/all/0/1">E. Koumpia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ababakr_K/0/1/0/all/0/1">K. M. Ababakr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wit_W/0/1/0/all/0/1">W. J. de Wit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oudmaijer_R/0/1/0/all/0/1">R. D. Oudmaijer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garatti_A/0/1/0/all/0/1">A. Caratti o Garatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boley_P/0/1/0/all/0/1">P. Boley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Linz_H/0/1/0/all/0/1">H. Linz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_S/0/1/0/all/0/1">S. Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vink_J/0/1/0/all/0/1">J. S. Vink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouquin_J/0/1/0/all/0/1">J.-B Le Bouquin</a> Binarity and multiplicity appear to be a common outcome in star formation. In particular, the binary fraction of massive (OB-type) stars can be very high. In many cases, the further stellar evolution of these stars is affected by binary interactions at some stage during their lifetime. The origin of this high binarity and theRead More →

Gravitational-wave merging events from the dynamics of stellar mass binary black holes around the massive black hole in a galactic nucleus. (arXiv:1903.02685v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_F/0/1/0/all/0/1">Fupeng Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shao_L/0/1/0/all/0/1">Lijing Shao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_W/0/1/0/all/0/1">Weishan Zhu</a> We study the dynamical evolution of the stellar mass binary black holes (BBHs) in a galactic nucleus that contains a massive black hole (MBH). For a comprehensive study of their merging events, we consider simultaneously the non-resonant and resonant relaxations of the BBHs, the binary-single encounters of the BBHs with the field stars, the Kozai-Lidov (KL) oscillation and the close encounters between the BBHs and the central MBH, which usually lead to binaries’Read More →