DOCSLIB.ORG

Rapid Cooling of Magnetized Neutron Stars

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Rapid Cooling of Magnetized Neutron Stars View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Rapid co oling of magnetized neutron stars 1 2;3 2 1 Debades Bandyopadhyay, Somenath Chakrabarty, Prantick Dey, and Subrata Pal 1 Saha Institute of Nuclear Physics, 1/AF Bidhannagar, Calcutta 700 064, India 2 Department of Physics, University of Kalyani, Kalyani 741235, India 3 IUCAA, P.B. 4, Ganeshkhind, Pune 411007, India Abstract The neutrino emissivities resulting from direct URCA pro cesses in neutron stars are calculated in a relativistic Dirac-Hartree approach in presence of a magnetic eld. In a quark or a hyp eron matter environment, the emissivity due to nucleon direct URCA pro cesses is suppressed relative to that from pure nuclear matter. In all the cases studied, the magnetic eld enhances emissivity compared to the eld-free cases. PACS numb ers: 26.60.+c, 21.65.+f, 12.39.Ba, 97.60.Jd Typ eset using REVT X E 1 Neutron stars are b orn in the aftermath of sup ernova explosions with interior temp era- > 11 tures T 10 K, but co ol rapidly in a few seconds by predominant neutrino emission [1] 10 5 6 to T < 10 K. Neutrino co oling then dominates and lasts for t 10 10 yr and sub- < 8 sequently photon emission takes over when T 10 K. Since the long term co oling of the 8 10 young neutron stars (T 10 10 K) pro ceeds via emission of neutrinos primarily from matter at supranuclear densities within the core, the study of the co oling of neutron stars by examination of neutrino emissivities may provide considerable insight into their interior structure and comp osition. For a long time the dominant neutrino co oling mechanism has b een the so-called standard mo del based on the mo di ed URCA pro cesses [2,3] (n; p)+n ! (n; p)+ p + e + ; e (n; p)+p+e ! (n; p)+ n + : (1) e The ROSAT detection [4] of thermal emission from neutron stars indicates the necessity of faster co oling mechanism in some young neutron stars, in particular the Vela pulsar. Faster neutrino emission than the standard mo del was prop osed by invoking pion [3,5] or kaon [6] condensates whichhave neutrino emissivities comparable to that from the -decay of quarks [7] in quark matter (consisting of u, d and s quarks) d ! u + e + ; u + e ! d + : (2) e e A similar relation for s-quark -decaymay o ccur and is obtained by replacing d by s quark in Eq. (2). The most p owerful energy losses, exp ected to date, are pro duced by the so-called direct URCA mechanism involving nucleons [8] n ! p + e + ; p + e ! n + : (3) e e The threshold density of this pro cess is however considerably larger than that of the mo di ed URCA pro cess. 14 Observations of pulsars predict large surface magnetic eld of B 10 G [9]. In the m core the eld may b e considerably ampli ed due to ux conservation from the original weak eld of the progenitor during its core collapse. In fact, the scalar virial theorem [10] predicts 18 large interior eld B 10 G or more [11], and these elds are frozen in the highly m conducting core. It has b een demonstrated [11] that when the eld B is comparable to m (c) or ab ove a critical eld B , the energy of a charged particle changes signi cantly in the m quantum limit; the quantum e ects are most pronounced when the particle moves in the lowest Landau level. The phase space mo di cations stemming from the strong magnetic eld in the core are exp ected to in uence the neutrino emission rate from young neutron stars. In this communication weevaluate the neutrino emissivity for the nucleon direct URCA pro cess of Eq. (3) in presence of a magnetic eld B , and demonstrate that it would lead to m more rapid co oling in the core. (A straightforward extension of the emissivity for nucleons into the quark sector may also be obtained in a magnetic eld.) For this purp ose, we consider a npe matter in -equilibrium within a relativistic Dirac-Hartree approach in the linear -! - mo del [12]. 2 At the neutron star core at temp eratures well b elow the typical Fermi temp erature of 12 T 10 K, the nucleons and electrons participating in neutrino pro ducing pro cesses are all F degenerate (the and are free) and have their momenta close to the Fermi momenta p , e e F i where i = n; p; e. Since neutrino and antineutrino momenta are kT =c p , the nucleon F i direct URCA pro cess is allowed by the momentum conservation when p + p p . Since F F F p e n matter is very close to -equilibrium, the chemical p otentials of the constituents satisfy the condition = + . (Henceforth we set h = c = k = 1.) n p e Employing the Weinb erg-Salam theory for weak interactions, the interaction Lagrangian p cc density for the charged current reaction (3) may b e expressed as L =(G = 2) cos l j , F c W int 49 3 where G ' 1:435 10 erg cm is the Fermi weak coupling constant and the Cabibb o F c angle. The lepton and nucleon charged weak currents are resp ectively, l = (1 ) 5 2 4 and j = (g g ) . Here, and in other formulae to follow, the indices i =14 V A 5 1 3 W refer to the n, , p and e, resp ectively. The vector and axial-vector coupling constants are e g = 1 and g =1:226. V A The emissivity due to the antineutrino emission pro cess in presence of a uniform magnetic eld B along z-axis when b oth the electrons and protons are Landau quantized is given by m Z Z Z Z Z Z 3 3 qB L =2 p qB L =2 p m x m x F F p e Vd p Vd p L dp L dp L dp L dp 1 2 y 3y y 4y z 3z z 4z " (B )=2 m 3 3 (2 ) (2 ) 2 2 2 2 qB L =2 qB L =2 p p m x m x F F p e 0 max max X X E W f (p )[1 f (p )][1 f (p )] ; (4) 2 fi 1 3 4 0 =0 =0 0 where and are resp ectively the maximum number of Landau levels p opulated for max max protons and electrons. The prefactor 2 takes into account the neutron spin degeneracy. The p (E ; p ) are the 4-momenta and E the antineutrino energy. The functions f (E ) denote i i i 2 i the Fermi-Dirac functions for the ith particle. The transition rate per unit volume due to the antineutrino emission pro cess may be derived from Fermi's golden rule and is given by 2 W = hjM j i=(tV ). Here t represents time and V = L L L the normalization volume. fi fi x y z 2 jM j is the squared matrix element and the symbol hi denotes an averaging over initial fi spins and a sum over nal spins. The matrix element for the V A interaction is given by Z G F 4 p M = (X ) (g g ) (X ) (X ) (1 ) (X ) : (5) d X fi V A 5 3 5 4 1 2 2 In presence of a uniform magnetic eld B , the normalized proton wave function is m q (X ) = 1= L L exp (iE t + ip y + ip z ) f (x), where f (x) is the 4- 3 y z 3 3y 3z p ;p p ;p 3y 3z 3y 3z comp onent spinor solution [11]. The form of the spinor in a magnetic eld (see Ref. [11]) restricts the analytical evaluation of the neutrino emissivity to elds strong enough so as to 0 p opulate only the ground state for electrons and protons, i.e. = =0. The only p ositive energy spinor for protons in the chiral representation is then [11,13] 0 1 E + p 3z 3 B C 0 B C =0 f (x)=N B I C (x); (6) =0 =0 ;p 3y p ;p 3y 3z @ A m 0 3 q 2 1=2 H 2 ) is the e ective where N = 1= 2E (E + p ), and E = E U = (p + m =0 3z 3 3 3 3 0;p 3z relativistic Hartree energy. The function I (x) is similar in form as in Ref. [11]. The =0;p 3y nucleon e ective and rest masses are resp ectively, m and m = m = m = 939 MeV. In n p presence of the magnetic eld, the wave functions for free electrons (X ) have the same 4 form as those for protons, but with m and E for protons replaced by the bare mass m and 3 e kinetic energy for electrons, resp ectively. The neutrons and neutrinos/antineutrinos b eing una ected by B , have plane wave functions. m Using these wave functions, it is straightforward to calculate the transition rate p er unit volume and is given by " # 2 2 2 G 1 (p p ) +(p +p ) 1x 2x 3y 4y F W = exp fi 3 E E E E V L L 2qB 2 4 y z m 1 3 h i 2 2 2 2 2 (g + g ) (p p )(p p )+(g g ) (p p )(p p ) (g g )m (p p ) V A 1 2 3 4 V A 1 4 3 2 4 2 V A (E E E E ) (p p p p ) (p p p p ): (7) 1 2 3 4 1y 2y 3y 4y 1z 2z 3z 4z Substituting Eq.
Load more

Recommended publications
  • Chiral Symmetry Restoration by Parity Doubling and the Structure of Neutron Stars
    Chiral symmetry restoration by parity doubling and the structure of neutron stars Micha l Marczenko,1 David Blaschke,1, 2, 3 Krzysztof Redlich,1, 4 and Chihiro Sasaki1 1Institute of Theoretical Physics, University of Wroc law, PL-50204 Wroc law, Poland 2Bogoliubov Laboratory of Theoretical Physics, Joint Institute for Nuclear Research, 141980 Dubna, Russia 3National Research Nuclear University, 115409 Moscow, Russia 4Extreme Matter Institute EMMI, GSI, D-64291 Darmstadt, Germany (Dated: November 14, 2018) We investigate the equation of state for the recently developed hybrid quark-meson-nucleon model under neutron star conditions of β−equilibrium and charge neutrality. The model has the character- istic feature that, at increasing baryon density, the chiral symmetry is restored within the hadronic phase by lifting the mass splitting between chiral partner states, before quark deconfinement takes place. Most important for this study are the nucleon (neutron, proton) and N(1535) states. We present different sets for two free parameters, which result in compact star mass-radius relations in accordance with modern constraints on the mass from PSR J0348+0432 and on the compactness from GW170817. We also consider the threshold for the direct URCA process for which a new relationship is given, and suggest as an additional constraint on the parameter choice of the model that this process shall become operative at best for stars with masses above the range for binary radio pulsars, M > 1:4 M . I. INTRODUCTION neutron stars. However, already before this occurs, a strong phase transition manifests itself by the appearance The investigation of the equation of state (EoS) of com- of an almost horizontal branch on which the hybrid star pact star matter became rather topical within the past solutions lie, as opposed to the merely vertical branch of few years, mainly due to the one-to-one correspondence pure neutron stars.
    [Show full text]
  • Convective Urca Process and Cooling in Dense Stellar Matter
    Convective Urca Process and cooling in dense stellar matter M. Schoenberg: The name Urca was given by us to the process which accompanies the emission of neutrino in supernova because of the following curious situation: In Rio de Janeiro, we went to play at the Casino-da-Urca and Gamow was very impressed with the table in which there was a roulette, in which money disappeared very quickly. With a sense of humor, he said: ‘Well, the energy is being lost in the centre of supernova with almost the same rapidity as money does from these tables!’ (from Grib, Novello: “Gamow in rio and the discovery of the URCA process”, Astronom & Astrophys. Trans. 2000, Vol 19) Feb 10 2010, Advisor-Seminar WS09/10 by Fabian Miczek Urca reactions Urca pairs consist of mother (M) and daughter (D) nuclei Urca reactions A A − - beta decay: Z1M Z De e A − A - electron capture: Z De Z 1Me Central questions: Is a continuous cycling between mother and daugter possible? Both reactions emit a neutrino => possible cooling mechanism? 2 electron captures require a threshold energy Eth=EM−ED−me c beta decays release the threshold energy M We're interested in degenerate stellar matter (ideal gas of ions, Fermi gas of electrons) E th threshold energy can be provided by e- mc2 the Fermi energy of the electrons D Example (E = 4.4 MeV) 23 23 − th Na Nee e 23 − 23 Nee Nae Electron captures in degenerate matter Fermi energy > threshold energy assume zero temperature ( kT << E ) F A − A Z De Z 1 M e energy heat M neutrino Fermi electron threshold e- mc2 density of states D
    [Show full text]
  • On the Theory of Gamma-Ray and Fast Radio Bursts
    On the Theory of Gamma-ray and Fast Radio Bursts D. Skripachov Abstract Gamma-ray bursts are characterized by energy comparable to the rest mass of stars and duration comparable to the time of passage of light of several diameters of star. It means GRBs signal the flares occur when stars fall on supermassive neutron collapsars (SMNC) located at the centers of galaxies. Long, short, very short and weak GRBs are matched the fall of main sequence stars, white dwarfs, neutron stars (NS) and rogue planets, respectively. GRB is the result of heating of star caused by the action of three factors: transverse compression of angular convergence to SMNC, friction of light matter (LM), and volumetric compression of the entry into gravitationally distended space. GRB is a circular flare in the stellar corona. GRB lasts until the star will be hidden under the π- horizon, on which the angle of gravitational deflection of beams is 180°. Multiple peaks are caused by the fall of binary stars and stars with planets, as well as by consecutive bursts of stellar core and overlying layers. Early afterglow is due to the annihilation, and later (x-ray and radio) due to aurora and remanence of LM. FRB precedes very short GRB. Milliseconds before GRB, "magnetic lightning" arises, which is a reconnection of magnetic field lines from NS anterior pole to SMNC. Magnetic dipoles of LM nuclei are aligned along the magnetic lines of force. This is accompanied by radio emission generated strictly perpendicular magnetic tube connecting NS and SMNC. Gravitation bends the plane of FRB in the hyperboloid with the cone angle of 40°.
    [Show full text]
  • Participant List Xiamen-CUSTIPEN Workshop, Xiamen, January 3 to 7, 2019
    Participant list Xiamen-CUSTIPEN Workshop, Xiamen, January 3 to 7, 2019 No. Name Affiliation Email 01 Shunke Ai 艾舜轲 Beijing Normal University, China [email protected]. edu.cn 02 Nils Andersson University of Southampton, UK N.A.Andersson@sot on.ac.uk Contribution Title: Using gravitational waves to constrain matter at extreme densities ​ Abstract: The spectacular GW170817 neutron star merger event provided interesting ​ constraint on neutron star physics (in terms of the tidal deformability). Future detections are expected improve on this. In this talk I will discuss if we can expect to also make progress on issues relating to the composition and state of matter. 03 Zhan Bai 摆展 Peking University, China [email protected] n Contribution Title: Constraining Hadron-Quark Phase Transition Chemical Potential via Astronomical observation 04 Shishao Bao 鲍世绍 Shanxi Normal University, China [email protected] du.cn 05 Andreas Bauswein GSI Darmstadt, Germany Andreas.Bauswein @h-its.org Contribution Title: Neutron star mergers and the high-density equation of state 06 Subrata kumar Biswal Institute of Theoretical Physics, [email protected] Chinese Academy of Sciences, China Contribution Title: Effects of the φ-meson on the hyperon production in the hyperon star ​ Abstract: Using relativistic mean field formalism, we have studied the effects of the strange ​ vector φ-meson on the equation of state and consequently on the maximum mass and radius of the hyperon star. Effects of the hyperon coupling constants on the strangeness content of the hyperon star are discussed with a number of the relativistic parameter set. The canonical mass-radius relationship also discussed with various relativistic parameter set.
    [Show full text]
  • The Single Degenerate Progenitor Scenario for Type Ia Supernovae and the Convective Urca Process
    The Single Degenerate Progenitor Scenario for Type Ia Supernovae and the Convective Urca Process ADissertationpresented by Donald Eugene Willcox to The Graduate School in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Physics Stony Brook University August 2018 Stony Brook University The Graduate School Donald Eugene Willcox We, the dissertation committe for the above candidate for the Doctor of Philosophy degree, hereby recommend acceptance of this dissertation Alan Calder – Dissertation Advisor Associate Professor, Physics and Astronomy Michael Zingale – Chairperson of Defense Associate Professor, Physics and Astronomy Joanna Kiryluk – Committee Member Associate Professor, Physics and Astronomy Matthew Reuter – External Committee Member Assistant Professor, Applied Mathematics and Statistics This dissertation is accepted by the Graduate School Charles Taber Dean of the Graduate School ii Abstract of the Dissertation The Single Degenerate Progenitor Scenario for Type Ia Supernovae and the Convective Urca Process by Donald Eugene Willcox Doctor of Philosophy in Physics Stony Brook University 2018 This dissertation explores the e↵ects of properties of the progenitor massive white dwarf (WD) on thermonuclear (Type Ia) supernovae. It includes a study of explosions from “hy- brid” C/O/Ne progenitors and focuses primarily on the convective Urca process occurring in C/O progenitors shortly before their explosion. Pre-supernova WDs approaching the Chan- drasekhar mass can possess sufficiently high central densities that 23Na synthesized via 12C fusion undergoes electron capture to 23Ne. Convection sweeps 23Ne to regions of lower den- sity where it reverts via beta decay to 23Na, and vice versa. Cyclic weak nuclear processes of this type constitute the convective Urca process in WDs.
    [Show full text]
  • Acknowledgments
    Acknowledgments J. Arons: I have benefitted from many discussions with A. Spitkovsky, P. Chang, N. Bucciantini, E. Amato, R. Blandford, F. Coroniti, D. Backer and E. Quataert. My research efforts on these topics have been supported by NSF grant AST-0507813 and NASA grant NNG06G108G, both to the University of California, Berkeley; by the Department of Energy contract to the Stanford Linear Accelerator Center no. DE-AC3-76SF00515; and by the taxpayers of California. W. Becker: I’m grateful to the Heraeus-Foundation for financing the 363rd Heraeus-Seminar on Neutron Stars and Pulsars which took place in May 2006 at the Physikzentrum in Bad Honnef. A selection of papers presented at this meet- ing and at the IAU Joined Discussion JD02 in Prague in August 2006 became the groundwork to produce this book. I’m further thankful to Joachim Trumper¨ and Harald Lesch for their help and support in organizing the Heraeus-Seminar and to Gunther¨ Hasinger as well as the MPE for additional financial support. Without the great organizational talent and help of Christa Ingram the meetings would not have been what they were. Thanks also for her help in producing this book. Christian Saedtler has spend many days in producing the index of this book. Sincere thanks to him for taking the time. All articles in this book were refereed. I am much obliged to all colleagues who helped in this process. Special thanks goes to Dr. Jaroslaw Dyks, Dr. Ulrich Geppert, Prof. Dr. Yashwant Gupta, Dr. John Kirk, Dr. Maura McLaughlin, Prof. Dr. Andreas Reisenegger and Prof.
    [Show full text]
  • Pos(Confinement8)151
    Cooling of isolated neutron stars as a probe of PoS(Confinement8)151 superdense matter physics Alexander Kaminker∗, Alexander Potekhin and Dmitry Yakovlev Ioffe Physical Technical Institute - Politekhnicheskaya 26, 194021 Saint-Petersburg, Russia E-mail: [email protected], [email protected], [email protected] We review a current state of cooling theory of isolated neutron stars. The main regulators of neutron star cooling are discussed. We outline the sensitivity of cooling models to equation of state of matter in the neutron star core; the presence or absence of enhanced neutrino emission; superfluidity of baryonic component of matter. A comparison of the cooling theory with observa- tions of thermal emission of isolated neutron stars gives a potentially powerful method to study fundamental properties of superdense matter in neutron star interiors. The prospects of studying neutron star parameters and internal structure are outlined. 8th Conference Quark Confinement and the Hadron Spectrum September 1-6, 2008 Mainz. Germany ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ Cooling of isolated neutron stars as a probe of superdense matter physics Alexander Kaminker 1. Introduction Microscopic theories of superdense matter in neutron star cores are model dependent and give a vast scatter of possible equation of states (EOSs) (e.g., [1, 2]) with different composition of neu- tron star cores (nucleons, hyperons, pion or kaon condensates, quarks), and different superfluid properties of baryons. The fundamental properties of supranuclear matter cannot be determined on purely theoretical basis, but viable theoretical models can be selected by comparing their predic- tions with observations of neutron stars.
    [Show full text]
  • Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar
    Article Thermal Spectrum and Neutrino Cooling Rate of the Vela Pulsar Dmitry D. Ofengeim and Dmitry A. Zyuzin Ioffe Institute, 26 Politekhnicheskaya str., St. Petersburg 194021, Russia; [email protected] * Correspondence: [email protected]; Tel.: +7-812-292-7180 Received: 22 June 2018; Accepted: 24 July 2018; Published: 30 July 2018 Abstract: We reanalyse the X-ray spectrum of the PSR B0833–45 (the Vela pulsar) using the data of the Chandra space observatory. In contrast to previous works, we consider a wide range of possible masses ¥ +0.04 and radii of the pulsar. The derived surface temperature of the star Ts = 0.66−0.01 MK (1s level over the entire mass and radius range of our study) is consistent with earlier results. However, the preferable values of Vela’s mass and radius given by the spectral analysis are different from those used previously; they are consistent with modern equation of state models of neutron star matter. In addition, we evaluate the Vela’s surface temperature as a function of assumed values of its mass and radius. This allows us to analyse the neutrino cooling rates consistent with the evaluated surface temperatures and explore the additional restrictions that could be set on the Vela’s mass and radius using different versions of the neutron star cooling theory. Keywords: the Vela pulsar; X-ray spectrum; neutrino cooling rate 1. Introduction In this presentation, we reanalyze the observations of the X-ray surface emission of the Vela pulsar ¥ (PSR B0833-45) and evaluate its effective surface temperature Ts (redshifted for a distant observer), mass M, radius R and the internal neutrino cooling rate using the cooling theory of neutron stars (NSs) [1].
    [Show full text]
  • Jhep06(2018)048
    Published for SISSA by Springer Received: April 13, 2018 Accepted: June 5, 2018 Published: June 8, 2018 Constraining axion-like-particles with hard X-ray emission from magnetars JHEP06(2018)048 Jean-Fran¸coisFortina and Kuver Sinhab aD´epartement de Physique, de G´eniePhysique et d'Optique, Universit´eLaval, 2325 Rue de l'Universit´e,Qu´ebec, QC G1V 0A6, Canada bDepartment of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, U.S.A. E-mail: [email protected], [email protected] Abstract: Axion-like particles (ALPs) produced in the core of a magnetar will convert to photons in the magnetosphere, leading to possible signatures in the hard X-ray band. We perform a detailed calculation of the ALP-to-photon conversion probability in the magneto- sphere, recasting the coupled differential equations that describe ALP-photon propagation into a form that is efficient for large scale numerical scans. We show the dependence of the conversion probability on the ALP energy, mass, ALP-photon coupling, magnetar radius, surface magnetic field, and the angle between the magnetic field and direction of propa- gation. Along the way, we develop an analytic formalism to perform similar calculations in more general n-state oscillation systems. Assuming ALP emission rates from the core that are just subdominant to neutrino emission, we calculate the resulting constraints on the ALP mass versus ALP-photon coupling space, taking SGR 1806-20 as an example. In particular, we take benchmark values for the magnetar radius and core temperature, and constrain the ALP parameter space by the requirement that the luminosity from ALP- to-photon conversion should not exceed the total observed luminosity from the magnetar.
    [Show full text]
  • Magnetic Neutron Star Cooling and Microphysics A
    A&A 609, A74 (2018) Astronomy DOI: 10.1051/0004-6361/201731866 & c ESO 2018 Astrophysics Magnetic neutron star cooling and microphysics A. Y. Potekhin1; 2; 3 and G. Chabrier1; 4 1 Centre de Recherche Astrophysique de Lyon, Université de Lyon, Université Lyon 1, Observatoire de Lyon, École Normale Supérieure de Lyon, CNRS, UMR 5574, 46 allée d’Italie, 69364 Lyon Cedex 07, France 2 Ioffe Institute, Politekhnicheskaya 26, 194021 Saint Petersburg, Russia e-mail: [email protected] 3 Central Astronomical Observatory at Pulkovo, Pulkovskoe Shosse 65, 196140 Saint Petersburg, Russia 4 School of Physics, University of Exeter, Exeter, EX4 4QL, UK Received 31 August 2017 / Accepted 24 October 2017 ABSTRACT Aims. We study the relative importance of several recent updates of microphysics input to the neutron star cooling theory and the effects brought about by superstrong magnetic fields of magnetars, including the effects of the Landau quantization in their crusts. Methods. We use a finite-difference code for simulation of neutron-star thermal evolution on timescales from hours to megayears with an updated microphysics input. The consideration of short timescales (.1 yr) is made possible by a treatment of the heat- blanketing envelope without the quasistationary approximation inherent to its treatment in traditional neutron-star cooling codes. For the strongly magnetized neutron stars, we take into account the effects of Landau quantization on thermodynamic functions and thermal conductivities. We simulate cooling of ordinary neutron stars and magnetars with non-accreted and accreted crusts and compare the results with observations. Results. Suppression of radiative and conductive opacities in strongly quantizing magnetic fields and formation of a condensed radiating surface substantially enhance the photon luminosity at early ages, making the life of magnetars brighter but shorter.
    [Show full text]
  • Book of Abstracts
    PHAROS Conference 2019: the multi-messenger physics and astrophysics of neutron stars Monday 22 April 2019 - Friday 26 April 2019 HOTEL CAP ROIG Book of Abstracts Contents Complex polarisation variability in radio pulsars and the implication for pulsar magneto- spheres ............................................ 1 Gravitational-wave data analysis for constraining the NS EoS ............... 1 The formation of (heavy) magnetars and collapsars ..................... 1 Neutron Star Equation of State after the GW170817 event .................. 2 Superfluidity and glitches .................................... 2 Pulsar glitches: a window on neutron star interior ...................... 3 The role of magnetic field in pulsar glitches .......................... 3 Spindown-powered transients from long-lived BNS merger remnants ........... 3 GW170817: lessons from the observations of a binary neutron star merger . 4 Gamma-ray bursts and magnetars: observational signatures and predictions in the multi- messenger era ........................................ 4 Modeling the strong-field dynamics of binary neutron star merger ............. 5 Thermal evolution of neo-neutron stars. I. Envelopes and Eddington luminosity phase. 5 An eye on two magnetars ................................... 6 Fast Moving Pulsars in the ISM: 3D RMHD modelling of Bow-Shock Pulsar Wind Nebulae 6 Disk formation from the collapse of a rotating neutron star ................. 7 Equation of state for neutron stars employing chiral interactions within the Green’s func- tion approach ........................................ 7 General predictions for the neutron star crustal moment of inertia ............. 7 Magnetic field evolution in neutron star cores ........................ 8 3D instabilities during the Type I bursts ............................ 9 Relativistic r-modes during type-I X-ray bursts ........................ 9 Unified equations of neutron-star interiors: role of the symmetry energy . 10 Multi-wavelength observations of High Mass X-ray Binaries .
    [Show full text]
  • Arxiv:Astro-Ph/0204151V1 9 Apr 2002
    Accepted for Publication in The Astrophysical Journal Letters New Constraints on Neutron Star Cooling from Chandra Observations of 3C58 Patrick Slane1, David J. Helfand2, and Stephen S. Murray1 ABSTRACT 3C58 is a young Crab-like supernova remnant. Historical evidence strongly suggests an association of the remnant with supernova SN 1181, which would make 3C58 younger than the Crab Nebula. Recent Chandra observations have identified the young 65 ms pulsar J0205+6449 at its center, embedded in a com- pact nebula which, we show here, appears to be confined by the pulsar wind termination shock. We present new Chandra observations of this compact nebula and embedded pulsar which set strong upper limits on thermal emission origi- nating from the neutron star surface. These limits fall far below predictions of standard neutron star cooling, requiring the presence of exotic cooling processes in the neutron star core. Subject headings: ISM: individual (3C58), pulsars: individual (PSR J0205+6449), stars: neutron, supernova remnants, X-rays: general arXiv:astro-ph/0204151v1 9 Apr 2002 1. Introduction Neutron stars are macroscopic manifestations of processes that otherwise occur only in individual atomic nuclei. Formed hot in the core collapse that terminates the life of a massive star, they are supported against gravitational implosion by neutron degeneracy pressure. However, details of the interior structure of neutron stars (NSs) remain poorly understood, largely due to our incomplete understanding of the strong interaction at ultrahigh densities. In the early stages of their lives, energy loss is dominated by neutrino emission. However, the neutrino production rate is highly dependent upon the structure of the interior.
    [Show full text]