RAS_WEB (Page 4,067)

Radiation-mediated shocks: kinetic processes and transition to collisionless shocks. (arXiv:1812.09866v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Derishev_E/0/1/0/all/0/1">Evgeny Derishev</a> We analyze the main features of radiation-mediated shocks at arbitrary shock velocities, both non-relativistic and relativistic. We describe two mechanisms, which may lead to formation of a sharp viscous subshock within otherwise smooth velocity profile at the shock front, even if the radiation pressure in the upstream is overwhelmingly large. These mechanisms are specific to sub-relativistic and relativistic radiation-mediated shocks and set high-velocity shocks apart from their non-relativistic counterparts, which do not develop a subshock if the radiation pressure is high enough. We briefly discuss implications of this finding. We analyzeRead More →

Quasi-periodic pulsations in a solar flare with an unusual phase shift. (arXiv:1812.09868v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kupriyanova_E/0/1/0/all/0/1">Elena G. Kupriyanova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kashapova_L/0/1/0/all/0/1">Larisa K. Kashapova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doorsselaere_T/0/1/0/all/0/1">Tom Van Doorsselaere</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chowdhury_P/0/1/0/all/0/1">Partha Chowdhury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Srivastava_A/0/1/0/all/0/1">Abhishek K. Srivastava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moon_Y/0/1/0/all/0/1">Yong-Jae Moon</a> Two kinds of processes could occur during the flare decay phase: processes of energy release or processes of energy relaxation. Quasi-periodic pulsations (QPPs) of the broadband emission are a good tool for the verification of mechanisms. We aim to study the processes during the decay phase of the X-class solar flare SOL2014-03-29T17:48. The observations in X-ray, microwave, and extreme ultraviolet (EUV) bands are exploited to study the fine temporal, spatial,Read More →

Volatile loss following cooling and accretion of the Moon revealed by chromium isotopes. (arXiv:1812.09881v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Sossi_P/0/1/0/all/0/1">Paolo A. Sossi</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Moynier_F/0/1/0/all/0/1">Fr&#xe9;d&#xe9;ric Moynier</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Zuilen_K/0/1/0/all/0/1">Kirsten van Zuilen</a> (1) ((1) Institut de Physique du Globe de Paris, Paris, France, (2) Institut Universitaire de France, Paris, France) Terrestrial and lunar rocks share chemical and isotopic similarities in refractory elements, suggestive of a common precursor. By contrast, the marked depletion of volatile elements in lunar rocks together with their enrichment in heavy isotopes compared to Earth s mantle suggests that the Moon underwent evaporative loss of volatiles. However, whether equilibrium prevailed during evaporation, and, ifRead More →

The development of lower-atmosphere turbulence early in a solar flare. (arXiv:1812.09906v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Jeffrey_N/0/1/0/all/0/1">N. L. S. Jeffrey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fletcher_L/0/1/0/all/0/1">L. Fletcher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Labrosse_N/0/1/0/all/0/1">N. Labrosse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simoes_P/0/1/0/all/0/1">P. J. A. Sim&#xf5;es</a> We present the first observational study of the onset and evolution of solar flare turbulence in the lower solar atmosphere on an unprecedented time scale of 1.7 s using the Interface Region Imaging Spectrograph observing plasma at a temperature of 80,000 K. At this time resolution, nonthermal spectral line broadening, indicating turbulent velocity fluctuations, precedes the flare onset at this temperature and is coincident with net blue-shifts. The broadening decreases as the flare brightens and then oscillatesRead More →

Accretion geometry of the black-hole binary Cygnus X-1 from X-ray polarimetry. (arXiv:1812.09907v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Chauvin_M/0/1/0/all/0/1">M. Chauvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Floren_H/0/1/0/all/0/1">H.-G. Flor&#xe9;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Friis_M/0/1/0/all/0/1">M. Friis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jackson_M/0/1/0/all/0/1">M. Jackson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kamae_T/0/1/0/all/0/1">T. Kamae</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kataoka_J/0/1/0/all/0/1">J. Kataoka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kawano_T/0/1/0/all/0/1">T. Kawano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kiss_M/0/1/0/all/0/1">M. Kiss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mikhalev_V/0/1/0/all/0/1">V. Mikhalev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mizuno_T/0/1/0/all/0/1">T. Mizuno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohashi_N/0/1/0/all/0/1">N. Ohashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stana_T/0/1/0/all/0/1">T. Stana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tajima_H/0/1/0/all/0/1">H. Tajima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Takahashi_H/0/1/0/all/0/1">H. Takahashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Uchida_N/0/1/0/all/0/1">N. Uchida</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pearce_M/0/1/0/all/0/1">M. Pearce</a> Black-hole binary (BHB) systems comprise a stellar-mass black hole and a closely orbiting companion star. Matter is transferred from the companion to the black hole, forming an accretion disk, corona and jet structures. The resulting release of gravitational energy leads to emission of X-rays.Read More →

A New RASS Galaxy Cluster Catalog with Low Contamination Extending to $zsim1$ in the DES Overlap Region. (arXiv:1812.09956v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Klein_M/0/1/0/all/0/1">Matthias Klein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grandis_S/0/1/0/all/0/1">Sebastian Grandis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohr_J/0/1/0/all/0/1">Joseph Mohr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paulus_M/0/1/0/all/0/1">Maria Paulus</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_DES/0/1/0/all/0/1">DES Collaboration</a> We present the MARD-Y3 catalog of between 1086 and 2171 galaxy clusters produced using multi-component matched filter (MCMF) followup in $5000 ~mathrm{deg}^2$ of DES-Y3 optical data of the ~20000 2RXS X-ray sources. MCMF is used to identify optical counterparts as peaks in galaxy richness as a function of redshift along the line of sight toward each 2RXS source within a search region informed by an X-ray prior. All peaks areRead More →

Impact of the neutron star crust on the tidal polarizability. (arXiv:1812.09974v1 [nucl-th]) <a href="http://arxiv.org/find/nucl-th/1/au:+Piekarewicz_J/0/1/0/all/0/1">J. Piekarewicz</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Fattoyev_F/0/1/0/all/0/1">F.J. Fattoyev</a> The first detection of a binary neutron star merger has opened the brand new era of multimessenger astronomy. This historic detection has been instrumental in providing constraints on the tidal polarizability of neutron stars. In turn, the tidal polarizability has been used to impose limits on stellar radii and ultimately on the equation of state (EOS). The tidal polarizability is also sensitive to the second tidal Love number k2. It is the main purpose of this work to perform a detailed study of k2 which, for aRead More →

The long-term evolution and appearance of Type Iax postgenitor stars. (arXiv:1812.08793v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_M/0/1/0/all/0/1">Michael Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuller_J/0/1/0/all/0/1">Jim Fuller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schwab_J/0/1/0/all/0/1">Josiah Schwab</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foley_R/0/1/0/all/0/1">Ryan Foley</a> Type Iax supernovae may arise from failed explosions of white dwarfs that leave behind a bound remnant (i.e., a “postgenitor” star) that could be identified in wide field surveys. To understand their observational signatures, we simulate these white dwarf (WD) postgenitors from shortly after explosion until they move back down the WD cooling track, and we consider several possible WD masses and explosion energies. To predict the peculiar surface abundances of the WD postgenitors, our models take into account gravitational settlingRead More →

Dark matter amnesia in out-of-equilibrium scenarios. (arXiv:1812.08795v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Berger_J/0/1/0/all/0/1">Joshua Berger</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Croon_D/0/1/0/all/0/1">Djuna Croon</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Hedri_S/0/1/0/all/0/1">Sonia El Hedri</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Jedamzik_K/0/1/0/all/0/1">Karsten Jedamzik</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Perko_A/0/1/0/all/0/1">Ashley Perko</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Walker_D/0/1/0/all/0/1">Devin G. E. Walker</a> Models in which the dark matter is produced at extremely low rates from the annihilation of Standard Model particles in the early Universe allow us to explain the current dark matter relic density while easily evading the traditional experimental constraints. In scenarios where the dark matter interacts with the Standard Model via a new physics mediator, the early Universe dynamics of the dark sector can be particularly complex, as the dark matter and the mediator couldRead More →

Multi-wavelength Analysis of the Merging Galaxy Cluster A115. (arXiv:1812.08797v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_M/0/1/0/all/0/1">Mincheol Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jee_M/0/1/0/all/0/1">M. James Jee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Finner_K/0/1/0/all/0/1">Kyle Finner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golovich_N/0/1/0/all/0/1">Nathan Golovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wittman_D/0/1/0/all/0/1">David M. Wittman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weeren_R/0/1/0/all/0/1">R. J. van Weeren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_W/0/1/0/all/0/1">W. A. Dawson</a> A115 is a merging galaxy cluster at $zsim0.2$ with a number of remarkable features including a giant ($sim2.5$ Mpc) radio relic, two asymmetric X-ray peaks with trailing tails, and a peculiar line-of-sight velocity structure. We present a multi-wavelength study of A115 using optical imaging data from Subaru, X-ray data from $Chandra$, and spectroscopic data from the Keck/DEIMOS and MMT/Hectospec instruments. Our weak-lensing analysis shows that the cluster is comprisedRead More →

Excluding super-soft X-ray sources as progenitors for four Type Ia supernovae in the Large Magellanic Cloud. (arXiv:1812.08799v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kuuttila_J/0/1/0/all/0/1">J. Kuuttila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilfanov_M/0/1/0/all/0/1">M. Gilfanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seitenzahl_I/0/1/0/all/0/1">I. R. Seitenzahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Woods_T/0/1/0/all/0/1">T. E. Woods</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vogt_F/0/1/0/all/0/1">F. P. A. Vogt</a> Type Ia supernovae are vital to our understanding of the Universe due to their use in measuring cosmological distances and their significance in enriching the interstellar medium with heavy elements. They are understood to be the thermonuclear explosions of white dwarfs, but the exact mechanism(s) leading to these explosions remains unclear. The two competing models are the single degenerate scenario, wherein a white dwarf accretes material from aRead More →

A Tapered Gridded Estimator (TGE) for the Multi-Frequency Angular Power Spectrum (MAPS) and the Cosmological HI 21-cm Power Spectrum. (arXiv:1812.08801v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bharadwaj_S/0/1/0/all/0/1">Somnath Bharadwaj</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pal_S/0/1/0/all/0/1">Srijita Pal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choudhuri_S/0/1/0/all/0/1">Samir Choudhuri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dutta_P/0/1/0/all/0/1">Prasun Dutta</a> In this work we present a new approach to estimate the power spectrum $P({bf k})$ of redshifted HI 21-cm brightness temperature fluctuations. The MAPS $C_{ell}(nu_a,nu_b)$ completely quantifies the second order statistics of the sky signal under the assumption that the signal is statistically homogeneous and isotropic on the sky. Here we generalize an already existing visibility based estimator for $C_{ell}$, namely TGE, to develop an estimator for $C_{ell}(nu_a,nu_b)$. The 21-cm power spectrumRead More →

Tracing the Quenching History in Galaxy Clusters in the EAGLE Simulation. (arXiv:1812.08802v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pallero_D/0/1/0/all/0/1">Diego Pallero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_F/0/1/0/all/0/1">Facundo A. G&#xf3;mez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padilla_N/0/1/0/all/0/1">Nelson D. Padilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Torres_Flores_S/0/1/0/all/0/1">S. Torres-Flores</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Demarco_R/0/1/0/all/0/1">R. Demarco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cerulo_P/0/1/0/all/0/1">P. Cerulo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Olave_Rojas_D/0/1/0/all/0/1">D. Olave-Rojas</a> We use the EAGLE hydrodynamical simulation to trace the quenching history of galaxies in its 10 most massive clusters. We use two criteria to identify moments when galaxies suffer significant changes in their star formation activity: {it i)} the instantaneous star formation rate (SFR) strongest drop, $Gamma_{rm SFR}^{rm SD}$, and {it ii)} a “quenching” criterium based on a minimum threshold for the specific SFR $lesssim$ 10$^{-11}rm yr^{-1}$. We findRead More →

Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2$lesssim$$z$$lesssim$0.9. (arXiv:1812.08804v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_Munoz_L/0/1/0/all/0/1">L. Rodr&#xed;guez-Mu&#xf1;oz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodighiero_G/0/1/0/all/0/1">G. Rodighiero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mancini_C/0/1/0/all/0/1">C. Mancini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_Gonzalez_P/0/1/0/all/0/1">P. G. P&#xe9;rez-Gonz&#xe1;lez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rawle_T/0/1/0/all/0/1">T. D. Rawle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Egami_E/0/1/0/all/0/1">E. Egami</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mercurio_A/0/1/0/all/0/1">A. Mercurio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosati_P/0/1/0/all/0/1">P. Rosati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Puglisi_A/0/1/0/all/0/1">A. Puglisi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franceschini_A/0/1/0/all/0/1">A. Franceschini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balestra_I/0/1/0/all/0/1">I. Balestra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baronchelli_I/0/1/0/all/0/1">I. Baronchelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biviano_A/0/1/0/all/0/1">A. Biviano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ebeling_H/0/1/0/all/0/1">H. Ebeling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edge_A/0/1/0/all/0/1">A. C. Edge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Enia_A/0/1/0/all/0/1">A. F. M. Enia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grillo_C/0/1/0/all/0/1">C. Grillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haines_C/0/1/0/all/0/1">C. P. Haines</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iani_E/0/1/0/all/0/1">E. Iani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_T/0/1/0/all/0/1">T. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nonino_M/0/1/0/all/0/1">M. Nonino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Valtchanov_I/0/1/0/all/0/1">I. Valtchanov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">B. Vulcani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zemcov_M/0/1/0/all/0/1">M. Zemcov</a> We quantify the star formation (SF) in the inner cores ($mathcal{R}$/$R_{200}$$leq$0.3)Read More →

Infrared Spectroscopy of Symbiotic Stars. XII. The Neutron Star SyXB System 4U 1700+24 = V934 Herculis. (arXiv:1812.08811v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hinkle_K/0/1/0/all/0/1">K. H. Hinkle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fekel_F/0/1/0/all/0/1">F. C. Fekel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Joyce_R/0/1/0/all/0/1">R. R. Joyce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mikolajewska_J/0/1/0/all/0/1">J. Miko&#x142;ajewska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galan_C/0/1/0/all/0/1">C. Galan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lebzelter_T/0/1/0/all/0/1">T. Lebzelter</a> V934 Her = 4U1700+24 is an M giant-neutron star (NS) X-ray symbiotic (SyXB) system. Employing optical and infrared radial velocities spanning 29 years combined with the extensive velocities in the literature, we compute the spectroscopic orbit of the M giant in that system. We determine an orbital period of 4391 days or 12.0 yr, the longest for any SyXB, and far longer than the 404 dayRead More →

A new method to probe the mass density and the cosmological constant using configuration entropy. (arXiv:1812.08816v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pandey_B/0/1/0/all/0/1">Biswajit Pandey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Das_B/0/1/0/all/0/1">Biswajit Das</a> We study the evolution of the configuration entropy for different combinations of $Omega_{m0}$ and $Omega_{Lambda0}$ in the flat $Lambda$CDM universe and find that the cosmological constant plays a decisive role in controlling the dissipation of the configuration entropy. The configuration entropy dissipates at a slower rate in the models with higher value of $Omega_{Lambda0}$. We find that the entropy rate decays to reach a minimum and then increases with time. The minimum entropy rate occurs at an earlier time for higher valueRead More →

A homogeneous analysis of globular clusters from the APOGEE survey with the BACCHUS code. I. The Northern clusters. (arXiv:1812.08817v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Masseron_T/0/1/0/all/0/1">T. Masseron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Hernandez_D/0/1/0/all/0/1">D.A.Garc&#xed;a-Hern&#xe1;ndez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meszaros_S/0/1/0/all/0/1">Sz. M&#xe9;sz&#xe1;ros</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamora_O/0/1/0/all/0/1">O. Zamora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DellAgli_F/0/1/0/all/0/1">F. Dell&#x27;Agli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_C/0/1/0/all/0/1">C. Allende Prieto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edvardsson_B/0/1/0/all/0/1">B. Edvardsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shetrone_M/0/1/0/all/0/1">M. Shetrone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plez_B/0/1/0/all/0/1">B. Plez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Trincado_J/0/1/0/all/0/1">J. G. Fern&#xe1;ndez-Trincado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_K/0/1/0/all/0/1">K. Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jonsson_H/0/1/0/all/0/1">H. J&#xf6;nsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Geisler_D/0/1/0/all/0/1">D. Geisler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beers_T/0/1/0/all/0/1">T. C. Beers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cohen_R/0/1/0/all/0/1">R. E. Cohen</a> We analyze a large sample of 885 GCs giants from the APOGEE survey. We used the Cannon results to separate the red giant branch and the asymptotic giant branch stars, not only allowing for a refinement ofRead More →

Orbital Motion of the Wide Planetary-Mass Companion GSC 6214-210 b: No Evidence for Dynamical Scattering. (arXiv:1812.08860v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Pearce_L/0/1/0/all/0/1">Logan A. Pearce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_A/0/1/0/all/0/1">Adam L. Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupuy_T/0/1/0/all/0/1">Trent J. Dupuy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ireland_M/0/1/0/all/0/1">Michael J. Ireland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rizzuto_A/0/1/0/all/0/1">Aaron C. Rizzuto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bowler_B/0/1/0/all/0/1">Brendan P. Bowler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birchall_E/0/1/0/all/0/1">Eloise K. Birchall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wallace_A/0/1/0/all/0/1">Alexander L. Wallace</a> Direct-imaging exoplanet surveys have discovered a class of 5-20 Mjupspace substellar companions at separations >100 AU from their host stars, which present a challenge to planet and star formation models. Detailed analysis of the orbital architecture of these systems can provide constraints on possible formation mechanisms, including the possibility they were dynamically ejected onto a wideRead More →