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Tuesday, November 17, 2020 | History

4 edition of Supplement to Spectral models of neutron star magnetospheres found in the catalog.

Supplement to Spectral models of neutron star magnetospheres

Supplement to Spectral models of neutron star magnetospheres

final report, NASA NAG5-3231, term--11/15/95-11/14/96

by

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English


Edition Notes

Other titlesSpectral models of neutron star magnetospheres.
Statement[principal investigator], Roger W. Romani.
Series[NASA contractor report] -- NASA-CR-203292., NASA contractor report -- NASA CR-203292.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL17593629M
OCLC/WorldCa40996970

An efficient smooth particle hydro (SPH) code will be used to model the disruption and coalescence of neutron stars in neutron-star black-hole binary systems and in double neutron-star systems. Simulations of expanding fireballs and of shock formation in interstellar medium will also be performed. GRO KNIFFEN. Can a neutron star with 6x Gauss dipolar field, as SGR +, show magnetar-like outburst and flares? Nanda Rea CSIC-IEEC Low field magnetars: they are many! B 0= e14 (B t=5e15) G B 0 = 3e14 G B 0= e15 G (Rea et al. in press; Vigano', et al. , submitted) See J. Pons and D. Vigano' talks! order to study the neutron star magnetospheres. Models radiative cooling, curvature radiation and its conversion into electron-positron pairs Can run on workstation GPUs or on CPU clusters. Tested on the Yeti cluster at Columbia and shows good scaling. A. Y. Chen (Columbia) Purdue May 10 2 / One of the most important discoveries by the Einstein Observatory was that normal stars of nearly all spectral types are unexpectedly strong X-ray emitters. The mechanisms that produce these X-rays are poorly understood and indicate fundamental problems in present theories of stellar evolution, the interiors and atmospheres of stars, and the mechanisms of coronal heating.


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Supplement to Spectral models of neutron star magnetospheres Download PDF EPUB FB2

Supplement to "Spectral models of neutron star magnetospheres": final report, NASA NAG, term/15//14/ Supplement to "Spectral Models of Neutron Star Magnetospheres" Term: 11/15/ 11/14/96,Ph Roger W.

Romani Department of Physics, Stanford University This grant has a somewhat complicated history. The award was nn approved subcontract under James M. Cordes' CGRO grant "OSSE an(t EGRET Observations of Known and New Pulsars". An incomparable reference for astrophysicists studying pulsars and other kinds of neutron stars, Theory of Neutron Star Magnetospheres sums up two decades of astrophysical research.

It provides in one volume the most important findings to date on this topic, essential to astrophysicists faced with a huge and widely scattered by: Curtis Michel, F.,Theory of Neutron Star Magnetospheres, The Univ ersity of Chicago Press de Ona-W ilhelmi, E.

et al.Astroparticle Physics, 43, We revisit the association of unidentified Galactic plane EGRET sources with tracers of recent massive star formation and death.

Up-to-date catalogs of OB. An incomparable reference for astrophysicists studying pulsars and other kinds of neutron stars, Theory of Neutron Star Magnetospheres sums up two decades of astrophysical research. It provides in one volume the most important findings to date on this topic, essential to astrophysicists faced with a huge and widely scattered literature.

Curtis Michel, who was. Detailed spectral analysis of the combined X-ray and optical data rules out the nonmagnetic neutron star atmosphere models with hydrogen, helium, iron and solar compositions. An incomparable reference for astrophysicists studying pulsars and other kinds of neutron stars, Theory of Neutron Star Magnetospheres sums up two decades of astrophysical research.

It provides in one volume the most important findings to date on this topic, essential to astrophysicists faced with a huge and widely scattered literature. creation opacities in inner magnetospheres of neutron stars, applicable to arbitrary colatitudes and a substantial range of altitudes in closed eld line zones above the stellar surface.

The focus on these regions makes for a more pertinent con-nection with physical models of magnetar emission than was a orded with previous expositions. Referring back to Figure 3 we see that, for the most part, the strange stars have higher mean density than the neutron stars.

Recalling the homology transformation at the end of Section 2, we see that it is possible that (for a reasonable, if iarge, choice of d) to make ir,odels of stng-e stars which can Supplement to Spectral models of neutron star magnetospheres book faster than any model neutron star. B = sec in tightest binary neutron star orbit of hours [2].

In addition to testing general relativity, this system provides a truly golden opportunity to verify and advance our models of pulsars magnetospheres, mechanisms of generation of radio emission and properties of their relativistic winds.

collecting area (m 2 at 8keV), high time (10 s) and spectral resolution (eV at 6keV), the LAD will make it possible to fully exploit the diagnostic power of high X-ray time and spectral resolution to determine the characteristics of neutron star magnetic elds, the geometry of their magnetospheres, study the radiation.

model Conclusions Electrodynamics of neutron star magnetospheres An example of non-neutral plasma in astrophysics Jérôme Pétri Centre d’Étude des Environnements Terrestre et Planétaires - Vélizy, FRANCE Laboratoire de Radio Astronomie, École Normale Supérieure - Paris, FRANCE Non Neutral Plasma Workshop, New York - 20/6/   Compact objects are an important class of astronomical objects in current research.

Supermassive black holes play an important role in the understanding of the formation of galaxies in the early Universe. Old white dwarfs are nowadays used to calibrate the age of the Universe. Mergers of neutron stars and black holes are the sources of intense gravitational.

magnetars to refer to neutron stars whose surface field exceeds the QED critical value of x G.]One of the most successful models for the emission from soft-gamma repeaters (SGR) invokes a magnetar with a decaying magnetic field.

In this work we describe a new class of superradiant instabilities of axion bound states in neutron star magnetospheres. The instability arises from the mixing of axion and photon modes in the magnetic field of the neutron star which extract energy from the rotating magnetosphere.

Kinetic magnetospheres of pulsars, black holes and binary neutron stars I: pm: Anatoly Spitkovsky: Kinetic magnetospheres of pulsars, black holes and binary neutron stars II: pm: Discussion: pm: Break: pm: Ioannis Contopoulos: A ring-of-fire in the pulsar magnetosphere: pm: Andrey Timokhin: Physics of Pair Pair.

Abstract. We study the magnetosphere of a slowly rotating magnetized neutron star subject to toroidal oscillations in the relativistic regime. Under the assumption of a zero inclination angle between the magnetic moment and the angular momentum of the star, we analyse the Goldreich–Julian charge density and derive a second-order differential equation for the.

COVID Resources. Reliable information about the coronavirus (COVID) is available from the World Health Organization (current situation, international travel).Numerous and frequently-updated resource results are available from this ’s WebJunction has pulled together information and resources to assist library staff as they consider how to handle.

Abstract. Pulsar magnetospheres are shaped by ultrarelativistic electron/positron plasmas flowing in a strong magnetic field and subject to strong gravitationa.

Neutron stars are compact objects rotating at high speed, up to a substantial fraction of the speed of light (up to 20% for millisecond pulsars) and possessing ultra-strong electromagnetic fields (close to and sometimes above the quantum critical field of × 10 9 T).

Moreover, due to copious e ± pair creation within the magnetosphere, the relativistic plasma surrounding the star. A neutron star is the collapsed core of a massive supergiant star, which had a total mass of between 10 and 25 solar masses, possibly more if the star was especially n stars are the smallest and densest stellar objects, excluding black holes and hypothetical white holes, quark stars, and strange stars.

Neutron stars have a radius on the order of 10. Neutron stars in X-ray binaries have magnetic fields among the highest found in the Universe, spanning at least the range from \({\sim}10^{8}\) to several \(10^{13}\ \mbox{G}\). The magnetospheres around these neutron stars have a strong influence on the accretion process, which powers most of their emission.

In their model, a magnetic dipole aligned with the rotation axis of the star is able to fill the magnetosphere with plasma and produce a variety of inter-esting observational phenomena. Shortly afterwards, other models for rotating magnetospheres were constructed by Michel (a,b, ).

All these models are based on the assumption that the dy. Neutron stars posses the highest rotation rates and strongest magnetic fields among all stars.

They radiate prolifically, in high energy electromagnetic radiation and in the radio band. This book is devoted to the selected lectures presented in the 6 th NATO-ASI series entitled "The Electromagnetic Spectrum of Neutron Stars" in Marmaris, Turkey.

Article: Gençali, Ali Arda and Ertan, Ünal () "Long-term evolution of RRAT J", Monthly Notices of the Royal Astronomical Society, Vol, No.1, (SCI): Ertan, Ünal () "Accretion and propeller torque in the spin-down phase of neutron stars: the case of transitional millisecond pulsar PSR J+", Monthly Notices of the Royal Astronomical.

Magnetospheres of Neutron Stars and Black Holes. A workshop at NASA Goddard Space Flight Center June 10 - 13, Build Room Organizers: Alice Harding, Demos Kazanas, Constantinos Kalapotharakos, Andrey Timokhin, Zorawar Wadiasingh Following the success of our initial workshop on the Physics of Pulsar Magnetospheres in Junewe.

Particle acceleration by electrostatic polarization fields that arise in plasmas streaming across magnetic fields is discussed as a possible acceleration mechanism of highest energy ({approx}>10{sup 20} eV) cosmic rays.

Specifically, plasmoids arising in planetoid impacts onto neutron star magnetospheres are considered. There is an increasing theoretical and observational evidence that the external magnetic field of magnetars may contain a toroidal component, likely of the. Beloborodov proposed that pairs discharge near the neutron star and create the relativistic outflow that further scatters thermal photons to high energies.

This model provided a satisfactory explanation for the hard-X-ray luminosity, spectral slopes, and pulsed profiles (e.g., Hascoët et al. ; Vogel et al. ), and it may also. and the Initial Spin of Neutron Star", Astrophysical Journal Letters,LL D.

Lai and A. Wiseman\Innermost Stable Circular Orbit of Inspiraling Neutron-Star Binaries: Tidal E ects, Post-Newtonian E ects and the Neutron-Star.

The theory of stellar atmospheres is one of the most important branches of modern astrophysics. It is first of all a major tool for understanding all aspects of stars. As the physical properties of their outer layers can now be found with high precision, firm conclusions can be drawn about the internal structure and evolution of stars.

magnetars, isolated cooling neutron stars, central compact objects, accreting X-ray pulsars (particularly millisecond pulsars), neutron stars in low-mass X-ray binaries, X-ray bursts, equation of state, structure and evolution of neutron stars, mechanisms of supernova explosions and neutron star mergers.

It is organized by Ioffe Institute. Albeit weak compared to those in young neutron-star systems, the neutron-star magnetospheres in LMXBs can play an important role in determining the correlations between spectral and temporal properties.

Parallel tracks appearing in the kilohertz (kHz) quasi-periodic oscillation (QPO) frequency versus X-ray flux plane can be used as a tool to. Magnetospheres of neutron stars are commonly modeled as either devoid of plasma in "vacuum'' models or filled with perfectly conducting plasma with negligible inertia in "force-free'' models.

While numerically tractable, neither of these idealized limits can simultaneously account for both the plasma currents and the accelerating electric. Neutron stars are formed when a massive star runs out of fuel and collapses. The very central region of the star – the core – collapses, crushing together every proton and electron into a neutron.

If the core of the collapsing star is between about 1 and 3 solar masses, these newly-created neutrons can stop the collapse, leaving behind a neutron star. In astronomy, stellar classification is the classification of stars based on their spectral characteristics.

Electromagnetic radiation from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with spectral line indicates a particular chemical element or molecule, with the line strength. The neutron is a neutral particle, which is stable only in the confines of the nucleus of the atom.

Outside the nucleus the neutron decays with a mean lifetime of about 15 min. Its mass, like that of the proton, is equivalent to 1 amu (atomic mass unit).

The detection of line features in these bursts, and hence from the surfaces of neutron stars, has been an important goal for high-resolution X-ray spectroscopy. A measurement of the wavelengths of identified line features would yield a measurement of the neutron star's gravitational redshift, which would help constrain current models for the.

The emission from accreting black holes and neutron stars, as well as from the highly magnetized neutron stars called magnetars, is dominated by X-rays. For this reason, spectral and timing studies in the X-rays have been extremely successful in broadening our understanding of compact objects in the past few decades.

Soon, a new observational window will open on. As this material spirals around the neutron star, it is funneled by the magnetic field toward the neutron star magnetic poles.

In the process, the material is heated until it becomes hot enough to radiate X-rays. As the neutron star spins, these hot regions pass through the line of sight from Earth and X-ray telescopes see these as X-ray pulsars.Neutron star, any of a class of extremely dense, compact stars thought to be composed primarily of neutrons.

Neutron stars are typically about 20 km (12 miles) in diameter. Their masses range between and times that of the Sun, but most are times that of the Sun.Quark stars made of strange quark matter are known as strange stars, and they form a subgroup under the quark star category.

Theoretical investigations have revealed that quark stars might not only be produced from neutron stars and powerful supernovas, they could also be created in the early cosmic phase separations following the Big Bang. If these primordial quark stars .