RAS_WEB (Page 4,569)

Signal recognition and background suppression by matched filters and neural networks for Tunka-Rex. (arXiv:1812.03347v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Shipilov_D/0/1/0/all/0/1">D. Shipilov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bezyazeekov_P/0/1/0/all/0/1">P. A. Bezyazeekov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Budnev_N/0/1/0/all/0/1">N. M. Budnev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chernykh_D/0/1/0/all/0/1">D. Chernykh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fedorov_O/0/1/0/all/0/1">O. Fedorov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gress_O/0/1/0/all/0/1">O. A. Gress</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haungs_A/0/1/0/all/0/1">A. Haungs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hiller_R/0/1/0/all/0/1">R. Hiller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huege_T/0/1/0/all/0/1">T. Huege</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kazarina_Y/0/1/0/all/0/1">Y. Kazarina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kleifges_M/0/1/0/all/0/1">M. Kleifges</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Korosteleva_E/0/1/0/all/0/1">E. E. Korosteleva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kostunin_D/0/1/0/all/0/1">D. Kostunin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuzmichev_L/0/1/0/all/0/1">L. A. Kuzmichev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lenok_V/0/1/0/all/0/1">V. Lenok</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lubsandorzhiev_N/0/1/0/all/0/1">N. Lubsandorzhiev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshalkina_T/0/1/0/all/0/1">T. Marshalkina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Monkhoev_R/0/1/0/all/0/1">R. Monkhoev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osipova_E/0/1/0/all/0/1">E. Osipova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pakhorukov_A/0/1/0/all/0/1">A. Pakhorukov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pankov_L/0/1/0/all/0/1">L. Pankov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Prosin_V/0/1/0/all/0/1">V. V. Prosin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schroder_F/0/1/0/all/0/1">F. G. Schr&#xf6;der</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zagorodnikov_A/0/1/0/all/0/1">A. Zagorodnikov</a> The Tunka Radio Extension (Tunka-Rex) is a digital antenna array, whichRead More →

The optical variability of Supermassive Black Hole Binary Candidate PG1302-102: Periodicity and perturbation in the light curve. (arXiv:1812.03370v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Kovacevic_A/0/1/0/all/0/1">Andjelka B. Kovacevic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Popovic_L/0/1/0/all/0/1">Luka C. Popovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simic_S/0/1/0/all/0/1">Sasa Simic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ilic_D/0/1/0/all/0/1">Dragana Ilic</a> The photometric light curve of PG1302-102 shows periodic variability which makes this object one of the most plausible supermassive black hole binary candidate. Interestingly, the most recent study of its updated optical light curve reports a decrease in significance of periodicity which may suggest that the binary model is less favorable. Here, we model the PG 1302-102 light curve, spanning almost 20 years, with a supermassive black hole binary system in whichRead More →

Quasinormal Modes of a Black Hole with Quadrupole Moment. (arXiv:1812.03376v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Allahyari_A/0/1/0/all/0/1">Alireza Allahyari</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Firouzjahi_H/0/1/0/all/0/1">Hassan Firouzjahi</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Mashhoon_B/0/1/0/all/0/1">Bahram Mashhoon</a> We analytically determine the quasinormal mode (QNM) frequencies of a black hole with quadrupole moment in the eikonal limit using the light-ring method. The generalized black holes that are discussed in this work possess arbitrary quadrupole and higher mass moments in addition to mass and angular momentum. In particular, the generalized black hole that we consider for our extensive calculations is a completely collapsed configuration whose exterior gravitational field can be described by the Hartle-Thorne spacetime [Astrophys. J. 153, 807-834 (1968)]. This collapsed system asRead More →

The VLA-COSMOS 3 GHz Large Project: Average radio spectral energy distribution of highly star-forming galaxies. (arXiv:1812.03392v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Tisanic_K/0/1/0/all/0/1">K. Tisani&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smolcic_V/0/1/0/all/0/1">V. Smol&#x10d;i&#x107;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delhaize_J/0/1/0/all/0/1">J. Delhaize</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Novak_M/0/1/0/all/0/1">M. Novak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Intema_H/0/1/0/all/0/1">H. Intema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Delvecchio_I/0/1/0/all/0/1">I. Delvecchio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schinnerer_E/0/1/0/all/0/1">E. Schinnerer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zamorani_G/0/1/0/all/0/1">G. Zamorani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bondi_M/0/1/0/all/0/1">M. Bondi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vardoulaki_E/0/1/0/all/0/1">E. Vardoulaki</a> We construct the average radio spectral energy distribution (SED) of highly star-forming galaxies (HSFGs) up to z~4. Infrared and radio luminosities are bound by a tight correlation that is defined by the so-called q parameter. This infrared-radio correlation provides the basis for the use of radio luminosity as a star-formation tracer. Recent stacking and survival analysis studies findRead More →

Helium variation in four Small Magellanic Cloud GCs. (arXiv:1812.03401v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lagioia_E/0/1/0/all/0/1">E. P. Lagioia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milone_A/0/1/0/all/0/1">A. P. Milone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">A. F. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dotter_A/0/1/0/all/0/1">A. Dotter</a> The multiple stellar populations (MPs) of $sim$11-13 Gyr-old Globular Clusters (GCs) in our Galaxy are characterized by different content of several light elements. These elements describe well-defined patterns like the C-N and the Na-O anticorrelations and the He-N and Na-N correlations. The discovery of the MPs in Magellanic Cloud GCs opened up new paths for the investigation of chemical anomalies in clusters with different age and physical properties. In this context, we used Hubble Space Telescope photometry to investigate theRead More →

Hubble Constant from LSST Strong lens time delays with microlensing systematics. (arXiv:1812.03408v1 [astro-ph.CO]) <a href="http://arxiv.org/find/astro-ph/1/au:+Liao_K/0/1/0/all/0/1">Kai Liao</a> Strong lens time delays have been widely used in cosmological studies, especially to infer $H_0$. The upcoming LSST will provide several hundred well measured time delays from the light curves of lensed quasars. However, due to the inclination of the finite AGN accretion disc and the differential magnification of the coherent temperature fluctuations, the microlensing by the stars can lead to changes in the actual time delay on the light-crossing time scale of the emission region $sim days$. We first study how this would change the uncertainty of $H_0$Read More →

Metric-affine Gravity and Inflation. (arXiv:1812.03420v1 [gr-qc]) <a href="http://arxiv.org/find/gr-qc/1/au:+Shimada_K/0/1/0/all/0/1">Keigo Shimada</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Aoki_K/0/1/0/all/0/1">Katsuki Aoki</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Maeda_K/0/1/0/all/0/1">Kei-ichi Maeda</a> We classify the metric-affine theories of gravitation, in which the metric and the connections are treated as independent variables, by use of several constraints on the connections. Assuming the Einstein-Hilbert action, we find that the equations for the distortion tensor (torsion and non-metricity) become algebraic, which means that those variables are not dynamical. As a result, we can rewrite the basic equations in the form of Riemannian geometry. Although all classified models recover the Einstein gravity in the Palatini formalism (in which we assume there is no coupling between matterRead More →

Very High Energy Ground Based Gamma Ray Telescopy Using TACTIC. (arXiv:1812.03429v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Reddy_M/0/1/0/all/0/1">Manikanta Reddy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_A/0/1/0/all/0/1">Anchal Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padhy_S/0/1/0/all/0/1">Shreyas Padhy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hebbar_P/0/1/0/all/0/1">Pavan R Hebbar</a> This project is a study of VHE gamma ray astronomy using atmospheric Cherenkov technique. The project involved the study of processes of interaction of gamma rays, formation of extensive air showers, imaging of the Cherenkov radiation and data analysis of the observed data of Crab Nebula and MRK421 using TACTIC at Mt. Abu, India. This project is a study of VHE gamma ray astronomy using atmospheric Cherenkov technique. The project involved the study of processes of interaction of gamma rays,Read More →

Evolution of A Magnetic Flux Rope toward Eruption. (arXiv:1812.03437v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_W/0/1/0/all/0/1">Wensi Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_C/0/1/0/all/0/1">Chunming Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Qiu_J/0/1/0/all/0/1">Jiong Qiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_R/0/1/0/all/0/1">Rui Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yang_K/0/1/0/all/0/1">Kai E. Yang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hu_Q/0/1/0/all/0/1">Qiang Hu</a> It is well accepted that a magnetic flux rope (MFR) is a critical component of many coronal mass ejections (CMEs), yet how it evolves toward eruption remains unclear. Here we investigate the continuous evolution of a pre-existing MFR, which is rooted in strong photospheric magnetic fields and electric currents. The evolution of the MFR is observed by the Solar Terrestrial Relations Observatory (STEREO) and the Solar Dynamics Observatory (SDO) from multiple viewpoints. From STEREO’s perspective, theRead More →

Detecting circumbinary exoplanets and hierarchical stellar triples with the LISA gravitational radiation mission. (arXiv:1812.03438v1 [astro-ph.EP]) <a href="http://arxiv.org/find/astro-ph/1/au:+Steffen_J/0/1/0/all/0/1">Jason H. Steffen</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_D/0/1/0/all/0/1">Dong-Hong Wu</a> (1,2), <a href="http://arxiv.org/find/astro-ph/1/au:+Larson_S/0/1/0/all/0/1">Shane L. Larson</a> (3) ((1) University of Nevada, Las Vegas, (2) Nanjing University, (3) CIERA, Northwestern University) We investigate the possibility of detecting planetary or stellar companions orbiting white dwarf binaries using the LISA gravitational radiation detector. Specifically, we consider the acceleration of the barycenter of the white dwarf binary due to the orbiting third body as well as the effect of changes in the tidal field across the binary due to the perturber’s eccentric orbit. We find that theRead More →

Cyclotron lines in highly magnetized neutron stars. (arXiv:1812.03461v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Staubert_R/0/1/0/all/0/1">R. Staubert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trumper_J/0/1/0/all/0/1">J. Tr&#xfc;mper</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kendziorra_E/0/1/0/all/0/1">E. Kendziorra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klochkov_D/0/1/0/all/0/1">D. Klochkov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Postnov_K/0/1/0/all/0/1">K. Postnov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kretschmar_P/0/1/0/all/0/1">P. Kretschmar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pottschmidt_K/0/1/0/all/0/1">K. Pottschmidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haberl_F/0/1/0/all/0/1">F. Haberl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rothschild_R/0/1/0/all/0/1">R.E. Rothschild</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Santangelo_A/0/1/0/all/0/1">A. Santangelo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilms_J/0/1/0/all/0/1">J. Wilms</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreykenbohm_I/0/1/0/all/0/1">I. Kreykenbohm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Furst_F/0/1/0/all/0/1">F. F&#xfc;rst</a> Cyclotron lines, also called cyclotron resonant scattering features (CRSF) are spectral features, generally appearing in absorption, in the X-ray spectra of objects containing highly magnetized neutron stars, allowing the direct measurement of the magnetic field strength in these objects. Cyclotron features are thought to be due to resonant scattering of photons by electrons in the strong magneticRead More →

Early B-type stars with resolved Zeeman split lines. (arXiv:1812.03462v1 [astro-ph.SR]) <a href="http://arxiv.org/find/astro-ph/1/au:+Hubrig_S/0/1/0/all/0/1">S. Hubrig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jarvinen_S/0/1/0/all/0/1">S.P. Jarvinen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scholler_M/0/1/0/all/0/1">M. Sch&#xf6;ller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_J/0/1/0/all/0/1">J.F. Gonzalez</a> Almost three decades ago, Mathys (1990) demonstrated the importance of studying Ap stars showing resolved Zeeman split Fe II 6147.7 and 6149.2 lines. Such Zeeman split lines can be seen in stars whose projected rotational velocity is sufficiently small and whose magnetic field is strong enough to exceed the rotational Doppler broadening. Observations of resolved Zeeman split lines permit the diagnosis of the average of the modulus of the magnetic field over the visible stellar hemisphere. Although Zeeman splitting is not expected inRead More →

Constraining the Braking Index and Energy Partition of Magnetar spin-down with {em Swift}/XRT data. (arXiv:1812.03465v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Lu_H/0/1/0/all/0/1">Hou-Jun L&#xfc;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lan_L/0/1/0/all/0/1">Lin Lan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liang_E/0/1/0/all/0/1">En-Wei Liang</a> Observationally, the long-lasting X-ray plateau emission in long GRBs show evidence for ongoing energy injection which may be from magnetar spin-down due to energy released via magnetic dipole (MD) or gravitational wave (GW) radiation. In this paper, by systematically analyzing the {em Swift}/XRT light curves detected before 2018 July, we find 45 light curves that monotonously decay as smooth broken power-law with redshift measured. By assuming that the central engines of these GRBs are a newly-born magnetar, we measure theRead More →

Modelling the SPARC galaxies using a neo-MOND formalism, and the subsequent derivations of the baryonic Tully-Fisher relation and Freeman’s Law. (arXiv:1812.03490v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Roscoe_D/0/1/0/all/0/1">David Roscoe</a> The SPARC sample consists of 175 nearby galaxies with modern surface photometry at $3.6,mu m$ and high quality rotation curves. The sample has been constructed to span very wide ranges in surface brightness, luminosity, rotation velocity and Hubble type, thereby forming a representative sample on galaxies in the nearby Universe. To date, the SPARC sample is the largest collection of galaxies with both high-quality rotation curves and NIR surface photometry. The neo-MOND model used here to analyse the SPARC sampleRead More →

Optimal subreflector position determination of shaped dual-reflector antennas based on the parameters iteration approach. (arXiv:1812.03497v1 [astro-ph.IM]) <a href="http://arxiv.org/find/astro-ph/1/au:+Xiang_B/0/1/0/all/0/1">Bin-bin Xiang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_C/0/1/0/all/0/1">Cong-si Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lian_P/0/1/0/all/0/1">Pei-yuan Lian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_N/0/1/0/all/0/1">Na Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ban_Y/0/1/0/all/0/1">You Ban</a> A new method based on parameters iteration technique has been developed to determine the optimal subreflector position for shaped Cassegrain antennas to improve the electromagnetic (EM) performance distorted by gravity. Both the features of shaped surface and the relationship between optical path difference (OPD) and far field beam pattern are employed. By describing the shaped dual-reflector surface as a standard discrete parabola set, we can utilize the optical features of the standard Cassegrain systemRead More →

CO multi-line observations of HH 80-81: a two-component molecular outflow associated with the largest protostellar jet in our Galaxy. (arXiv:1812.03501v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Qiu_K/0/1/0/all/0/1">Keping Qiu</a> (NJU), <a href="http://arxiv.org/find/astro-ph/1/au:+Wyrowski_F/0/1/0/all/0/1">Friedrich Wyrowski</a> (MPIfR), <a href="http://arxiv.org/find/astro-ph/1/au:+Menten_K/0/1/0/all/0/1">Karl Menten</a> (MPIfR), <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Q/0/1/0/all/0/1">Qizhou Zhang</a> (CfA), <a href="http://arxiv.org/find/astro-ph/1/au:+Guesten_R/0/1/0/all/0/1">Rolf Guesten</a> (MPIfR) Stretching a length reaching 10 pc projected in the plane of sky, the radio jet associated with Herbig-Haro objects 80 and 81 (HH 80-81) is known as the largest and best collimated protostellar jet in our Galaxy. The nature of the molecular outflow associated with this extraordinary jet remains an unsolved question which is of great interests to our understanding of the relationship betweenRead More →

New mechanism of producing superheavy Dark Matter. (arXiv:1812.03516v1 [hep-ph]) <a href="http://arxiv.org/find/hep-ph/1/au:+Babichev_E/0/1/0/all/0/1">Eugeny Babichev</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Gorbunov_D/0/1/0/all/0/1">Dmitry Gorbunov</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Ramazanov_S/0/1/0/all/0/1">Sabir Ramazanov</a> We study in detail the recently proposed mechanism of generating superheavy Dark Matter with the mass larger than the Hubble rate at the end of inflation. A real scalar field constituting Dark Matter linearly couples to the inflaton. As a result of this interaction, during inflation the scalar is displaced from its zero expectation value. This offset feeds into the energy density of Dark Matter at later stages. This mechanism is universal and can be implemented in a generic inflationary model. Compared to the other known mechanismsRead More →

Vela as the Source of Galactic Cosmic Rays above 100 TeV. (arXiv:1812.03522v1 [astro-ph.HE]) <a href="http://arxiv.org/find/astro-ph/1/au:+Bouyahiaoui_M/0/1/0/all/0/1">M.Bouyahiaoui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kachelriess_M/0/1/0/all/0/1">M.Kachelriess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Semikoz_D/0/1/0/all/0/1">D.V.Semikoz</a> We model the contribution of the nearest young supernova remannt Vela to the local cosmic ray flux taking into account both the influence of the Local Superbubble and the effect of anisotropic diffusion. The dominant contribution of this source in the energy region around the cosmic ray knee can naturally explain the observed fluxes of individual groups of nuclei and their total flux. Adding the CR flux from a 2-3 Myr old local CR source suggested earlier, the CR spectra in the whole energy range betweenRead More →

Towards the first detection of strongly lensed HI emission. (arXiv:1812.03524v1 [astro-ph.GA]) <a href="http://arxiv.org/find/astro-ph/1/au:+Blecher_T/0/1/0/all/0/1">Tariq Blecher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Deane_R/0/1/0/all/0/1">Roger Deane</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heywood_I/0/1/0/all/0/1">Ian Heywood</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Obreschkow_D/0/1/0/all/0/1">Danail Obreschkow</a> We report interferometric observations tuned to the redshifted neutral hydrogen (HI) 21cm emission line in three strongly lensed galaxies at $z sim 0.4$ with the Giant Metrewave Radio Telescope (GMRT). One galaxy spectrum (J1106+5228 at z=0.407) shows evidence of a marginal detection with an integrated signal-to-noise ratio of 3.8, which, if confirmed by follow-up observations, would represent the first strongly lensed and most distant individual galaxy detected in HI emission. Two steps are performed to transcribe the lensed integrated flux measurements intoRead More →

Properties of Neutron Stars with hyperon cores in parameterized hydrostatic conditions. (arXiv:1812.03529v1 [nucl-th]) <a href="http://arxiv.org/find/nucl-th/1/au:+Sen_D/0/1/0/all/0/1">Debashree Sen</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Banerjee_K/0/1/0/all/0/1">Kinjal Banerjee</a>, <a href="http://arxiv.org/find/nucl-th/1/au:+Jha_T/0/1/0/all/0/1">T.K. Jha</a> Models of neutron stars (NSs) with hyperon cores are constructed with an effective chiral model in mean-field approximation. The hyperon couplings are fixed by reproducing their experimentally determined binding energies. The impact of these couplings on population of different particles and the equation of state (EoS) are studied in this work. The global properties of NSs like gravitational mass, radius, baryonic mass and central density are calculated using parameterized Tolman-Oppenheimer-Volkoff equations (PTOV) with special emphasis on two effects of pressure – one contributingRead More →