DOCSLIB.ORG

Rapidly Rotating Pulsar Radiation in Vacuum Nonlinear Electrodynamics

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Rapidly Rotating Pulsar Radiation in Vacuum Nonlinear Electrodynamics View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Springer - Publisher Connector Eur. Phys. J. C (2016) 76:612 DOI 10.1140/epjc/s10052-016-4464-3 Regular Article - Theoretical Physics Rapidly rotating pulsar radiation in vacuum nonlinear electrodynamics V. I. Denisov1,I.P.Denisova2,A.B.Pimenov1,V.A.Sokolov1,a 1 Physics Department, Moscow State University, Moscow 119991, Russia 2 Moscow Aviation Institute (National Research University), Volokolamskoe Highway 4, Moscow 125993, Russia Received: 5 September 2016 / Accepted: 23 October 2016 / Published online: 8 November 2016 © The Author(s) 2016. This article is published with open access at Springerlink.com 13 Abstract In this paper we investigate the corrections of high-field (surface fields more than Bp > 10 G) radio loud vacuum nonlinear electrodynamics on rapidly rotating pulsar pulsars can be explained by pair-production suppression due radiation and spin-down in the perturbative QED approach to photon splitting [19]. (post-Maxwellian approximation). An analytical expression In this paper we calculate vacuum nonlinear electrody- for the pulsar’s radiation intensity has been obtained and ana- namics corrections to electromagnetic radiation of rapidly lyzed. rotating pulsar and analyze pulsar spin-down under these cor- rections. This paper is organized as follows. In Sect. 2, we present 1 Introduction vacuum nonlinear electrodynamics models and discuss their main physical properties and predictions. In Sect. 3 pulsar Vacuum nonlinear electrodynamics effects is an object that radiation in post-Maxwellian approximation is calculated. piques a great interest in contemporary physics [1–4]. First of Section 4 is devoted to an analysis of the pulsar’s spin-down all it is related to the emerging opportunities of experimental vacuum nonlinear electrodynamics influence. In the last sec- research in terrestrial conditions using extreme laser facili- tion we summarize our results. ties like extreme light infrastructure (ELI) [5–7], Helmholtz International Beamline for extreme fields (HIBEF) [8]. It opens up new possibilities in fundamental physics tests [9– 2 Vacuum nonlinear electrodynamics theoretical models 11] with an extremal electromagnetic field intensities and particle accelerations that have never been obtained before. Modern theoretical models of nonlinear vacuum electrody- At the same time the investigation of the effects of vac- namics suppose that the electromagnetic field Lagrange func- uum nonlinear electrodynamics in astrophysics gives us an tion density L = L(I(2), I(4)) depends on both independent ki kl mi additional opportunity to carry out versatile research using invariants I(2) = FikF and I(4) = FikF Flm F of the the natural extreme regimes of strong electromagnetic and electromagnetic field tensor Fik. The specific relationship gravitational fields with intensities unavailable yet in lab- between the Lagrange function and the invariants depends oratory conditions. Compact astrophysical objects with a on the choice of the theoretical model. Nowadays the most strong field, such as pulsars and magnetars, are best suited promising models are Born–Infeld and Heisenberg–Euler for vacuum nonlinear electrodynamics research. Nowadays, electrodynamics. there are many effects of vacuum nonlinear electrodynam- Born–Infeld electrodynamics is a phenomenological the- ics predicted in the pulsar’s neighborhood. For example vac- ory originating from the requirement of self-energy finite- uum electron–positron pair production [12] and photon split- ness for a point-like electrical charge [20]. In subsequent ting [13], photon frequency doubling [14], light by light scat- studies, the attempts of quantization were performed [21,22] tering, and vacuum birefringence [15], transient radiation ray and also it was revealed that Born–Infeld theory describes bending [16,17] and normal waves delay [18]. Some of the the dynamics of electromagnetic fields on D-branes in string predicted effects are indirectly confirmed by astrophysical theory [23–25]. As the main features of Born–Infeld electro- observations. For instance the evidence of the absence of the dynamics one can note the absence of birefringence (how- ever, there are modifications of the Born–Infeld theory [26] a e-mail: [email protected] with the vacuum birefringence predictions) and dichroism for 123 612 Page 2 of 8 Eur. Phys. J. C (2016) 76 :612 electromagnetic waves propagating in external electromag- predictions were experimentally proved in Delbrück light netic field [27]. Furthermore, this theory has a distinctive by light scattering [30], nonlinear Compton scattering [31], feature – the value of electric field depends on the direction Schwinger pair production in multiphoton scattering [1]. At of approach to the point-like charge. This property was noted the same time the recent astrophysical observations [32,33] by the authors of the theory and also eliminated by them in point on the absence of the vacuum birefringence effect the subsequent model development [28]. which favors the Born–Infeld theory prediction. The mea- Lagrangian function in Born–Infeld electrodynamics has surements performed for the speed of light in vacuum show the following form: that it does not depend on wave polarization with the accuracy δc/c < 10−28. So clarification of the vacuum nonlinear elec- ⎧ ⎫ ⎨ ⎬ trodynamics status requires the expansion of the experimen- 1 a2 a4 a4 L =− 1 − I( ) − I( ) + I 2 − 1 , tal test list both in terrestrial and astrophysical conditions. π 2 ⎩ 2 4 (2) ⎭ 4 a 2 4 8 The main hopes as regards this way to proceed are assigned (1) to the experiments with ultra-high intensity laser facilities [4] and astrophysical experiments with X-ray polarimetry [34] where a is a characteristic constant of theory, the inverse in pulsars and magnetars neighborhood. value of which has a meaning of maximum electric field for As follows from the Lagrangians (1)–(2) vacuum non- the point-like charge. For this constant only the following linear electrodynamics’ influence becomes valuable only − − , ∼ / estimation is known: a2 < 1.2 × 10 32 G 2. in strong electromagnetic fields, comparable to E B 1 a , ∼ The other nonlinear vacuum electrodynamics – the Hei- for Born–Infeld theory and E B Bc for Heisenberg– senberg–Euler model [15,29] – was derived in quantum field Euler electrodynamics [35]. In the case of relatively weak , << theory and describes one-loop radiative corrections caused by fields (E B Bc) the exact expressions (1) and (2) can be vacuum polarization in a strong electromagnetic field. Unlike decomposed and written [36] in the form of a unified para- the Born–Infeld electrodynamics, this theoretical model pos- metric post-Maxwellian Lagrangian: sesses vacuum birefringent properties in a strong field. 1 2 The effective Lagrangian function for Heisenberg–Euler L = I( ) + ξ (η − η )I + η I( ) , π 2 2 1 2 2 (2) 4 2 4 (5) theory has the following form: 32 ∞ ξ = / 2 = . × −27 −2 α 2 −σ σ where 1 Bc 0 5 10 G , and the post- I(2) Bc e d 2 L = − xyσ ctg(xσ)cth(yσ) Maxwellian parameters η1 and η2 depend on the choice of 16π 8π 2 σ 3 0 the theoretical model. In the case of Heisenberg–Euler elec- η η σ 2 trodynamics the post-Maxwellian parameters 1 and 2 are + (x2 − y2) − 1 dσ, (2) coupled to the fine structure constant α [37]: 3 2 3 13 where B = m c /eh¯ = 4.41 × 10 G is the value of the α − 7α − c η = = 5.1 × 10 5,η= = 9.0 × 10 5. (6) characteristic field in quantum electrodynamics, e and m are 1 45π 2 180π the electron charge and mass, α = e2/hc¯ is the fine structure constant, and for brevity we use the notations For Born–Infeld electrodynamics these parameters are equal to each other and they can be expressed through the i 1 field induction 1/a typical of this theory [37]: x =−√ (B2 − E2) + i(BE) 2Bc 2 2 2 η = η = a Bc < . × −6. 1 1 2 4 9 10 (7) − (B2 − E2) − i(BE) , (3) 4 2 The electromagnetic field equations for the post-Maxwellian vacuum electrodynamics with the Lagrangian (5) are equiv- 1 1 y = √ (B2 − E2) + i(BE) alent [35] to the equations of Maxwell electrodynamics of 2Bc 2 continuous media, 1 + (B2 − E2) − i(BE) . (4) ∂ F + ∂ F + ∂ F = 0, (8) 2 m ik i km k mi Many attempts to find the experimental status for each ∂ Qki 4π of these theories were made a long time ago, but nowadays =− jk, (9) it still remains ambiguous. There is experimental evidence ∂xi c in favor of each of them. Heisenberg–Euler electrodynamics with the specific nonlinear constitutive relations [18] 123 Eur. Phys. J. C (2016) 76 :612 Page 3 of 8 612 ki = ki + ξ (η − η ) ki + η ki , where Fki is the electromagnetic field tensor of the rotating Q F 1 2 2 I(2) F 4 2 F(3) (10) (0) magnetic dipole m in Maxwell electrodynamics and f ik is ki kn mi the vacuum nonlinear correction. Substituting (13)into(10) where F( ) = F Fnm F is the third power of the elec- 3 and retaining only the terms linear in a small value f ik it can tromagnetic field tensor. The tensor Qik can be separated be found that into two terms Qki = Fki + Mki, one of which, Mki, will have a meaning similar to the matter polarization tensor in Qik f ik + Fik + Mik , (14) electrodynamics of continuous media. (0) (0) Also it should be noted that in a post-Maxwellian approx- ik ik = ik( nj ) imation the stress-energy tensor T and Poynting vector S where M(0) M F(0) is the polarization tensor calcu- have the form lated in the approximation of the Maxwell electrodynamics nj ik field F(0). The electromagnetic field equations (8)–(9) with ik = 1 ( + ξη ) ik − g T 1 1 I(2) F(2) 2I(2) account of (13)–(14) then will take the form 4π 8 (0) (0) (0) + ξ(η + η ) 2 − η ξ , ∂m F + ∂i F + ∂k F + ∂m fik + ∂i fkm + ∂k fmi = 0, 1 2 2 I(2) 4 2 I(4) (11) ik km mi ki ki ∂ f ki ∂ F( ) ∂ M( ) 4π + 0 + 0 =− jk.
Load more

Recommended publications
  • Exploring Pulsars
    High-energy astrophysics Explore the PUL SAR menagerie Astronomers are discovering many strange properties of compact stellar objects called pulsars. Here’s how they fit together. by Victoria M. Kaspi f you browse through an astronomy book published 25 years ago, you’d likely assume that astronomers understood extremely dense objects called neutron stars fairly well. The spectacular Crab Nebula’s central body has been a “poster child” for these objects for years. This specific neutron star is a pulsar that I rotates roughly 30 times per second, emitting regular appar- ent pulsations in Earth’s direction through a sort of “light- house” effect as the star rotates. While these textbook descriptions aren’t incorrect, research over roughly the past decade has shown that the picture they portray is fundamentally incomplete. Astrono- mers know that the simple scenario where neutron stars are all born “Crab-like” is not true. Experts in the field could not have imagined the variety of neutron stars they’ve recently observed. We’ve found that bizarre objects repre- sent a significant fraction of the neutron star population. With names like magnetars, anomalous X-ray pulsars, soft gamma repeaters, rotating radio transients, and compact Long the pulsar poster child, central objects, these bodies bear properties radically differ- the Crab Nebula’s central object is a fast-spinning neutron star ent from those of the Crab pulsar. Just how large a fraction that emits jets of radiation at its they represent is still hotly debated, but it’s at least 10 per- magnetic axis. Astronomers cent and maybe even the majority.
    [Show full text]
  • Brochure Pulsar Multifunction Spectroscopy Service Complete Cased Hole Formation Evaluation and Reservoir Saturation Monitoring from A
    Pulsar Multifunction spectroscopy service Introducing environment-independent, stand-alone cased hole formation evaluation and saturation monitoring 1 APPLICATIONS FEATURES AND BENEFITS ■ Stand-alone formation evaluation for diagnosis of bypassed ■ Environment-independent reservoir saturation monitoring ■ High-performance pulsed neutron generator (PNG) hydrocarbons, depleted reservoirs, and gas zones in any formation water salinity ● Optimized pulsing scheme with multiple square and short ● Differentiation of gas-filled porosity from very low porosity ● Production fluid profile determination for any well pulses for clean separation in measuring both inelastic and formations by using neutron porosity and fast neutron cross inclination: horizontal, deviated, and vertical capture gamma rays 8 section (FNXS) measurements ● Detection of water entry and flow behind casing ● High neutron output of 3.5 × 10 neutron/s for greater ■ measurement precision Petrophysical evaluation with greater accuracy by accounting ● Gravel-pack quality determination by using for grain density and mineral properties in neutron porosity elemental spectroscopy ■ State-of-the-art detectors ■ Total organic carbon (TOC) quantified as the difference ■ Metals for mining exploration ● Near and far detectors: cerium-doped lanthanum bromide between the measured total carbon and inorganic carbon ■ High-resolution determination of reservoir quality (RQ) (LaBr3:Ce) ■ Oil volume from TOC and completion quality (CQ) for formation evaluation ● Deep detector: yttrium aluminum perovskite
    [Show full text]
  • One Or Several Populations of Fast Radio Burst Sources?
    One or several populations of fast radio burst sources? M. Caleb1, L. G. Spitler2 & B. W. Stappers1 1Jodrell Bank Centre for Astrophysics, the University of Manchester, Manchester, UK. 2Max-Planck-Institut fu¨r Radioastronomie, Bonn, Germany. arXiv:1811.00360v1 [astro-ph.HE] 1 Nov 2018 1 To date, one repeating and many apparently non-repeating fast radio bursts have been de- tected. This dichotomy has driven discussions about whether fast radio bursts stem from a single population of sources or two or more different populations. Here we present the arguments for and against. The field of fast radio bursts (FRBs) has increasingly gained momentum over the last decade. Overall, the FRBs discovered to date show a remarkable diversity of observed properties (see ref 1, http://frbcat.org and Fig. 1). Intrinsic properties that tell us something about the source itself, such as polarization and burst profile shape, as well as extrinsic properties that tell us something about the source’s environment, such as the magnitude of Faraday rotation and multi-path propagation effects, do not yet present a coherent picture. Perhaps the most striking difference is between FRB 121102, the sole repeating FRB2, and the more than 60 FRBs that have so far not been seen to repeat. The observed dichotomy suggests that we should consider the existence of multiple source populations, but it does not yet require it. Most FRBs to date have been discovered with single-pixel telescopes with relatively large angular resolutions. As a result, the non-repeating FRBs have typically been localized to no bet- ter than a few to tens of arcminutes on the sky (Fig.
    [Show full text]
  • Central Engines and Environment of Superluminous Supernovae
    Central Engines and Environment of Superluminous Supernovae Blinnikov S.I.1;2;3 1 NIC Kurchatov Inst. ITEP, Moscow 2 SAI, MSU, Moscow 3 Kavli IPMU, Kashiwa with E.Sorokina, K.Nomoto, P. Baklanov, A.Tolstov, E.Kozyreva, M.Potashov, et al. Schloss Ringberg, 26 July 2017 First Superluminous Supernova (SLSN) is discovered in 2006 -21 1994I 1997ef 1998bw -21 -20 56 2002ap Co to 2003jd 56 2007bg -19 Fe 2007bi -20 -18 -19 -17 -16 -18 Absolute magnitude -15 -17 -14 -13 -16 0 50 100 150 200 250 300 350 -20 0 20 40 60 Epoch (days) Superluminous SN of type II Superluminous SN of type I SN2006gy used to be the most luminous SN in 2006, but not now. Now many SNe are discovered even more luminous. The number of Superluminous Supernovae (SLSNe) discovered is growing. The models explaining those events with the minimum energy budget involve multiple ejections of mass in presupernova stars. Mass loss and build-up of envelopes around massive stars are generic features of stellar evolution. Normally, those envelopes are rather diluted, and they do not change significantly the light produced in the majority of supernovae. 2 SLSNe are not equal to Hypernovae Hypernovae are not extremely luminous, but they have high kinetic energy of explosion. Afterglow of GRB130702A with bumps interpreted as a hypernova. Alina Volnova, et al. 2017. Multicolour modelling of SN 2013dx associated with GRB130702A. MNRAS 467, 3500. 3 Our models of LC with STELLA E ≈ 35 foe. First year light ∼ 0:03 foe while for SLSNe it is an order of magnitude larger.
    [Show full text]
  • Pulsars and Supernova Remnants
    1604–2004: SUPERNOVAE AS COSMOLOGICAL LIGHTHOUSES ASP Conference Series, Vol. 342, 2005 M. Turatto, S. Benetti, L. Zampieri, and W. Shea Pulsars and Supernova Remnants Roger A. Chevalier Dept. of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903, USA Abstract. Massive star supernovae can be divided into four categories de- pending on the amount of mass loss from the progenitor star and the star’s ra- dius. Various aspects of the immediate aftermath of the supernova are expected to develop in different ways depending on the supernova category: mixing in the supernova, fallback on the central compact object, expansion of any pul- sar wind nebula, interaction with circumstellar matter, and photoionization by shock breakout radiation. Models for observed young pulsar wind nebulae ex- panding into supernova ejecta indicate initial pulsar periods of 10 − 100 ms and approximate equipartition between particle and magnetic energies. Considering both pulsar nebulae and circumstellar interaction, the observed properties of young supernova remnants allow many of them to be placed in one of the super- nova categories; the major categories are represented. The pulsar properties do not appear to be related to the supernova category. 1. Introduction The association of SN 1054 with the Crab Nebula and its central pulsar can be understood in the context of the formation of the neutron star in the core collapse and the production of a bubble of relativistic particles and magnetic fields at the center of an expanding supernova. Although the finding of more young pulsars and their wind nebulae initially proceeded slowly, there has recently been a rapid set of discoveries of more such pulsars and nebulae (Camilo 2004).
    [Show full text]
  • Astrophysics VLT/UVES Spectroscopy of Wray 977, the Hypergiant
    UvA-DARE (Digital Academic Repository) VLT/UVES spectroscopy of Wray 977, the hypergiant companion to the X-ray pulsar GX301-2 Kaper, L.; van der Meer, A.; Najarro, F. DOI 10.1051/0004-6361:20065393 Publication date 2006 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Kaper, L., van der Meer, A., & Najarro, F. (2006). VLT/UVES spectroscopy of Wray 977, the hypergiant companion to the X-ray pulsar GX301-2. Astronomy & Astrophysics, 457(2), 595- 610. https://doi.org/10.1051/0004-6361:20065393 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:02 Oct 2021 A&A 457, 595–610 (2006) Astronomy DOI: 10.1051/0004-6361:20065393 & c ESO 2006 Astrophysics VLT/UVES spectroscopy of Wray 977, the hypergiant companion to the X-ray pulsar GX301−2 L.
    [Show full text]
  • (NASA/Chandra X-Ray Image) Type Ia Supernova Remnant – Thermonuclear Explosion of a White Dwarf
    Stellar Evolution Card Set Description and Links 1. Tycho’s SNR (NASA/Chandra X-ray image) Type Ia supernova remnant – thermonuclear explosion of a white dwarf http://chandra.harvard.edu/photo/2011/tycho2/ 2. Protostar formation (NASA/JPL/Caltech/Spitzer/R. Hurt illustration) A young star/protostar forming within a cloud of gas and dust http://www.spitzer.caltech.edu/images/1852-ssc2007-14d-Planet-Forming-Disk- Around-a-Baby-Star 3. The Crab Nebula (NASA/Chandra X-ray/Hubble optical/Spitzer IR composite image) A type II supernova remnant with a millisecond pulsar stellar core http://chandra.harvard.edu/photo/2009/crab/ 4. Cygnus X-1 (NASA/Chandra/M Weiss illustration) A stellar mass black hole in an X-ray binary system with a main sequence companion star http://chandra.harvard.edu/photo/2011/cygx1/ 5. White dwarf with red giant companion star (ESO/M. Kornmesser illustration/video) A white dwarf accreting material from a red giant companion could result in a Type Ia supernova http://www.eso.org/public/videos/eso0943b/ 6. Eight Burst Nebula (NASA/Hubble optical image) A planetary nebula with a white dwarf and companion star binary system in its center http://apod.nasa.gov/apod/ap150607.html 7. The Carina Nebula star-formation complex (NASA/Hubble optical image) A massive and active star formation region with newly forming protostars and stars http://www.spacetelescope.org/images/heic0707b/ 8. NGC 6826 (Chandra X-ray/Hubble optical composite image) A planetary nebula with a white dwarf stellar core in its center http://chandra.harvard.edu/photo/2012/pne/ 9.
    [Show full text]
  • Stellar Evolution
    AccessScience from McGraw-Hill Education Page 1 of 19 www.accessscience.com Stellar evolution Contributed by: James B. Kaler Publication year: 2014 The large-scale, systematic, and irreversible changes over time of the structure and composition of a star. Types of stars Dozens of different types of stars populate the Milky Way Galaxy. The most common are main-sequence dwarfs like the Sun that fuse hydrogen into helium within their cores (the core of the Sun occupies about half its mass). Dwarfs run the full gamut of stellar masses, from perhaps as much as 200 solar masses (200 M,⊙) down to the minimum of 0.075 solar mass (beneath which the full proton-proton chain does not operate). They occupy the spectral sequence from class O (maximum effective temperature nearly 50,000 K or 90,000◦F, maximum luminosity 5 × 10,6 solar), through classes B, A, F, G, K, and M, to the new class L (2400 K or 3860◦F and under, typical luminosity below 10,−4 solar). Within the main sequence, they break into two broad groups, those under 1.3 solar masses (class F5), whose luminosities derive from the proton-proton chain, and higher-mass stars that are supported principally by the carbon cycle. Below the end of the main sequence (masses less than 0.075 M,⊙) lie the brown dwarfs that occupy half of class L and all of class T (the latter under 1400 K or 2060◦F). These shine both from gravitational energy and from fusion of their natural deuterium. Their low-mass limit is unknown.
    [Show full text]
  • Neutron Stars to Open Their Heavy Hearts
    NEWS IN FOCUS it arrives at the International Space Station, INSIDE A NEUTON STA NASA’s Neutron Star Interior Composition A NASA mission will use X-ray spectroscopy to gather clues about the interior of neutron Explorer (NICER), a washing-machine-sized stars — the Universe’s densest forms of matter. box, will use X-rays coming from hotspots at the spinning stars’ poles to calculate the size of the stars. Outer crust Size matters, because a bigger star suggests Atomic nuclei, free electrons a stiff core that is relatively able to withstand Inner crust gravity’s compression, which means that it is Heavier atomic nuclei, free probably tightly packed with neutrons jostling neutrons and electrons against each other at higher pressure than that SVS FROM NASA GODDARD SOURCE: ADAPTED Outer core in atomic nuclei. A smaller, more compact Quantum liquid where star, meanwhile, would mean a soft interior, neutrons, protons and electrons exist in a soup in which neutrons could be dissolved in a sea of their constituent quarks. Other, more exotic proposals include the core being made of Inner core ‘hyperons’, which incorporate heavier ‘strange’ Unknown ultra-dense matter. ? Neutrons and protons may quarks within them. remain as particles, break down NICER will pinpoint the stars’ radii by into their constituent quarks, or even become ‘hyperons’. studying how their huge gravitational fields bend the light they emit. Seen from the space station, the light is fainter when the beam points away, but remains visible because the star’s gravitational field diverts some of the light back this way. The extent to which the light dims when the beam faces away tells astrono- Atmosphere mers about this field, and consequently the Hydrogen, helium, carbon star’s mass-to-radius ratio.
    [Show full text]
  • Asymmetric Supernova Explosions : the Missing Link Between Wolf-Rayet Binaries, Run-Away Ob Stars and Pulsars
    ASYMMETRIC SUPERNOVA EXPLOSIONS : THE MISSING LINK BETWEEN WOLF-RAYET BINARIES, RUN-AWAY OB STARS AND PULSARS Jean-Pierre De Cuyper Astrofysisch Instituut, Vrije Universiteit Brussel, Belgium. The WR binary systems, consisting of a WR star and an 0 or B star companion, are supposed to be the progenitors of the massive X-ray binaries. The missing link is generally accepted to be the SN explosion of the WR star which leaves a pulsar remnant. As most pulsars originate from single stars, observations of their proper motions indicate that they receive at their birth a "kick" velocity of about 100 km s We assume this velocity to be due to the asymmetry of the SN explosion. This asymmetry, together with the loss of the SN shell and its impact on the OB star, may cause to disrupt the remaining system. For the ten best known WR binaries we evaluated the survival probability P after an instantaneous SN explosion, leaving a 1.5 M collapsar with a random orientated kick velocity of 75 kms (case a) and 150 kms_1 (case b) respectively. The influence of the impact is found to be marginal. The run-away velocity of the remaining system v and of the disrupted OB star v are comparable and of the same order of magnitude, but smaller than the initial orbital velocity of the OB companion; which decreases for increasing values of the initial orbital period. They are found to be independent of the kick velocity. Systems with an initial period of less than a few weeks stay together for case a and have .
    [Show full text]
  • Detection of a Type Iin Supernova in Optical Follow-Up Observations of Icecube Neutrino Events Magellan Workshop, 17–18 March 2016, DESY Hamburg
    Detection of a Type IIn Supernova in Optical Follow-Up Observations of IceCube Neutrino Events Magellan Workshop, 17{18 March 2016, DESY Hamburg Markus Voge, Nora Linn Strotjohann, Alexander Stasik 17 March 2016 Target: transient sources (< 100 s • neutrino burst): GRBs (Waxman & Bahcall 1997, Murase • & Nagataki 2006) SNe with jets (Razzaque, Meszaros, • Waxman 2005) More exotic phenomena? E.g. Fast • Radio Bursts (FRBs)? (Falcke & Rezzolla 2013) Online Neutrino Analysis Automatic search for interesting IceCube neutrino events • Realtime alerts sent to follow-up instruments • Multi-messenger: Combination with other data fruitful • Follow-up ensures access to data • 2 / 15 Online Neutrino Analysis Automatic search for interesting IceCube neutrino events • Realtime alerts sent to follow-up instruments • Multi-messenger: Combination with other data fruitful • Follow-up ensures access to data • Target: transient sources (< 100 s • neutrino burst): GRBs (Waxman & Bahcall 1997, Murase • & Nagataki 2006) SNe with jets (Razzaque, Meszaros, • Waxman 2005) More exotic phenomena? E.g. Fast • Radio Bursts (FRBs)? (Falcke & Rezzolla 2013) 2 / 15 The OFU and XFU system SN/GRB PTF (optical) Swift (X-ray) Alerts Alerts Madison/Bonn Iridium IceCube arXiv: 1309.6979 (p.40) 3 / 15 Online analysis scheme neutrino purity At least 8 coincident Trigger Level 0:0001% hits 2000 Hz ∼ Basic muon event se- Level 1 35 Hz 0:01% lection (tracks only) ∼ Up-going tracks Level 2 2 Hz 0:1% ∼ Neutrino selection OFU Level 3 mHz 90% (BDT) ∼ Neutrino multiplet ( 2ν): ≥ Time
    [Show full text]
  • Pennsylvania Science Olympiad Southeast Regional Tournament 2013 Astronomy C Division Exam March 4, 2013
    PENNSYLVANIA SCIENCE OLYMPIAD SOUTHEAST REGIONAL TOURNAMENT 2013 ASTRONOMY C DIVISION EXAM MARCH 4, 2013 SCHOOL:________________________________________ TEAM NUMBER:_________________ INSTRUCTIONS: 1. Turn in all exam materials at the end of this event. Missing exam materials will result in immediate disqualification of the team in question. There is an exam packet as well as a blank answer sheet. 2. You may separate the exam pages. You may write in the exam. 3. Only the answers provided on the answer page will be considered. Do not write outside the designated spaces for each answer. 4. Include school name and school code number at the bottom of the answer sheet. Indicate the names of the participants legibly at the bottom of the answer sheet. Be prepared to display your wristband to the supervisor when asked. 5. Each question is worth one point. Tiebreaker questions are indicated with a (T#) in which the number indicates the order of consultation in the event of a tie. Tiebreaker questions count toward the overall raw score, and are only used as tiebreakers when there is a tie. In such cases, (T1) will be examined first, then (T2), and so on until the tie is broken. There are 12 tiebreakers. 6. When the time is up, the time is up. Continuing to write after the time is up risks immediate disqualification. 7. In the BONUS box on the answer sheet, name the gentleman depicted on the cover for a bonus point. 8. As per the 2013 Division C Rules Manual, each team is permitted to bring “either two laptop computers OR two 3-ring binders of any size, or one binder and one laptop” and programmable calculators.
    [Show full text]