[High time resolution studies of binary X ray pulsars] [semiannual technical report, 1 Sep. 1992 - 1 Aug. 1993]

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

Written in English

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Subjects:

  • Pulsars.

Edition Notes

Book details

Statementprepared by Lynn R. Cominsky.
SeriesNASA contractor report -- NASA CR-194395.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL17680416M

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There were 6 sources originally proposed for analysis: SMC X-1, A, LMC X-1, LMC X-3, (these 3 sources are all located in the Large Magellanic Cloud region), 4UO+63 and 4U Results on these sources are summarized. Get this from a library. [High time resolution studies of binary X ray pulsars]: [semiannual technical report, 1 Sep.

Aug. [Lynn R Cominsky; United. This report covers the period September 1, through August 1, for NASA grant NAG through the Astrophysics Data Program (ADP), for the project 'High Time Resolution Studies of Binary X-ray Pulsars'.

Accreting X-ray pulsars are among the most luminous objects in the X-ray sky. In highly magnetized neutron stars (B~10^12 G), the flow of matter is dominated by the strong magnetic field. The general properties of accreting X-ray binaries are presented, focusing on the spectral characteristics of the systems.

The use of cyclotron lines as a tool to directly measure a neutron star's magnetic Cited by: 3. Watts, David John'X-ray and optical studies of binary x-ray pulsars', PhD thesis, University of : David John Watts. Abstract. As X-ray astronomy enters the Einstein era when faint, distant, and exotic X-ray sources are being investigated, we thought it might be useful to review some of the progress made over the past decade on a class of relatively nearby objects that have contributed richly to our understanding of astrophysics — the binary X-ray pulsars.

Several new features of X-ray binary pulsars are revealed from recent observations with ASCA, RXTE, BeppoSAX and other X-ray observatories. Among these, I will review in this paper some recent progress in spectroscopic studies of accreting X-ray pulsars in binary systems (XBPs).

First, I will discuss soft excess features observed in the energy spectra of XBPs and propose that it is a common. We report on a 39 ks observation of the s low-mass X-ray binary pulsar 4U with the High Energy Transmission Grating Spectrometer (HETGS) on the Chandra X-Ray Observatory.

These include the pulsar with the fastest rotation period (in the globular cluster Terzan 5; Hessels et al. ), the double pulsar system (Burgay et al. ; Lyne et al. ) and its impressive tests of general relativity (Kramer et al.

), the ‘missing link’ between the low-mass X-ray binaries and the MSPs (Archibald et al. X-ray binaries are a class of binary stars that are luminous in X-rays are produced by matter falling from one component, called the donor (usually a relatively normal star), to the other component, called the accretor, which is very compact: a neutron star or black infalling matter releases gravitational potential energy, up to several tenths of its rest mass, as X-rays.

Radio Pulsars in Binary Systems Ren e Paul Breton Department of Physics McGill University Montr eal, Qu ebec Canada December A Thesis submitted to McGill University in partial ful llment of the requirements of the degree of Doctor of Philosophy c Ren e P.

Breton, arXivv1 [] 15 Jul [High time resolution studies of binary X ray pulsars] [microform]: [semiannual technical report, 1 Sep Pulsars / Richard N. Manchester, Joseph H. Taylor Clocks in the sky: the story of pulsars.

CC(94) W-1 =S$' + OXOO X-RAY BINARY PULSARS: PULSE ORBIT AND THE HIGH-ENERGY CONTINUUM M. Maisack Astronomisches Insti der Universitat Tabingen, TUbingen, Germany RACT Pulse period and binary orbit period in X-ray pulsars have been found to be correlated, depending on the nature of the mass-donor.

Available in the National Library of Australia collection. Author: Graham-Smith, Francis, Sir, ; Format: Book; xii, pages: illustrations ; 24 cm. Observational data of pulsing X-ray sources, nonpulsing X-ray sources, and binary radio pulsars are analyzed.

Evolutionary scenarios for Her X-1, MXB4UGX 1 + 4, 1E +   Radio pulsars with millisecond spin periods are thought to have been spun up by the transfer of matter and angular momentum from a low-mass companion star during an x-ray–emitting phase.

The spin periods of the neutron stars in several such low-mass x-ray binary (LMXB) systems have been shown to be in the millisecond regime, but no radio pulsations have been detected. STUDY OF THE SPECTRAL AND TEMPORAL CHARACTERISTICS OF X-RAY EMISSION OF THE GAMMA-RAY BINARY LS WITH SUZAKU LS is a high-mass X-ray binary (Motch et al.

) with extended radio emission (Paredes et al. ). a high-mass binary system containing a nonaccreting pulsar (Johnston et al. ), whereas Cyg X-1 is a well.

Radio pulsars with millisecond spin periods are thought to have been spun up by the transfer of matter and angular momentum from a low-mass companion star during an x-ray–emitting phase. The spin periods of the neutron stars in several such low-mass x-ray binary (LMXB) systems have been.

Pulsars and X-Ray Sources - Volume 55 - F. Pacini. We use cookies to distinguish you from other users and to provide you with a better experience on our websites. The idea for organizing an Advanced Study Institute devoted largely to neutron star timing arose independently in three places, at Istanbul, Garching and Amster­ dam; when we became aware of each other's ideas we decided to join forces.

The choice of a place for the Institute, in Turkey, appealed. Harvard-Smithsonian Center for Astrophysics 60 Garden Street, Cambridge, MA USA Phone: Fax: The present state of X–ray astronomy which has already produced brilliant successes (the observation of powerful X–ray sources – ‘X–ray stars’, including pulsars, and so on) is on the whole in a stage of being established and of fast development and it seems particularly inappropriate to discuss here the available observational data.

Indeed, inthe High Time Resolution Universe survey discovered a radio pulsar whose rotational and X-ray properties identified it as a magnetar (Levin et al.

Here, we present X-ray observations of three high-B radio pulsars: PSRs J−, B−19, and J− These as a group are key sources for X-ray study, as they. THE X-ray properties of pulsars (highly magnetized rotating neutron stars) depend mainly on the age of the star1.

For young (≤ yr) pulsars, virtually all of the X-ray emission is pulsed. ⚠ We understand you may need to change your travel plans. Please be aware that due to the current circumstances, it may take us longer than usual to respond to any queries you send us.

This is the first such measurement of an interacting binary system through the gamma-ray emission of a millisecond pulsar. The scientists make full use of the Fermi-LAT time resolution, which is a.

The authors report the discovery of kHz fluctuations, including quasi-periodic oscillations (QPO) at {approximately} Hz and {approximately} Hz and a broadband kHz continuum in the power density spectrum of the high mass X-ray binary pulsar Centaurus X-3 (Jernigan, Klein and Arons ).

Discovered on Octo as part of the Monitor of All-sky X-ray Image (MAXI) experiment, MAXI J is a transient pulsar in a high-mass X-ray binary (HMXB) system. On Novem The gamma-ray binary system PSR B/LSoriginally discovered in a high-frequency radio survey devoted to the detection of young and short-period pulsars [19], consists of a rapidly rotating neutron star with a spin period of about 48 ms and a spin-down luminosity ∼ 10 35 erg s − 1.

version with high-resolution color figures Hut, P.,in The Evolution of Galactic X-Ray Binaries, eds. Truemper, W. Lewin and W. Brinkmann (Dordrecht: Reidel), pp. [12] Explosive Mass Loss in Binary Stars: the Two Time-Scale Method, Hut.

Via the wonderful site Astrobites I learned about the discovery of an amazing astronomical object: IGR J−, the most compact binary system accreting X-ray millisecond pulsar ever found. Yeah, so OK. That's a lot of jargon. Tell you what: Let's tackle it right to left.

First, what's a pulsar. A pulsar is special kind of neutron star. OK, what's a neutron star. It's the über-dense. Books at Amazon. The Books homepage helps you explore Earth's Biggest Bookstore without ever leaving the comfort of your couch. Here you'll find current best sellers in books, new releases in books, deals in books, Kindle eBooks, Audible audiobooks, and so much more.

Cygnus X-1 is this type of X-ray Binary. They are bright in X-rays not only because of the accretion disc, but also because there is a corona which is much more powerful than the Sun's corona.

Cygnus X-1 is 10, times more powerful than the Sun, and most of it is. Gravitational Redshift. Consider the pulsar stationed at some radius R from its Schwarzchild binary companion.

If the pulsar is emitting light at a frequency &omega *, astronomers on Earth will recieve the signals at a lower frequency, &omega &infin, due to the gravitational redshift effect.

This gravitational time dilation can be read almost directly from the Schwarzchild metric; again, the. It is thought that millisecond pulsars with white dwarf companions are born from X‐ray binaries. The majority of known systems have been studied uniquely in the radio domain, which limits our understanding of such systems.

We present here the X‐ray observations of the millisecond pulsar PSR J+ and the two faint millisecond pulsars PSR J+ and PSR J+, which we. Radio pulsars with millisecond spin periods are thought to have been spun up by transfer of matter and angular momentum from a low-mass companion star during an X-ray-emitting phase.

The spin periods of the neutron stars in several such low-mass X-ray binary (LMXB) systems have been shown to be in the millisecond regime, but no radio pulsations. The magnetic spectrum of X-ray binary pulsars C.

Ferrigno & R. Farinelli ISDC & ESSC, University of Geneva Dublin compMag - no 2 High B-field: an ubiquitous property • High mass X-ray binaries are normally young systems, where NS has a high B-field ( Time [d since 18 Feb ] 0 5 10 15 20 25 ASM rate High and Medium Resolution Spectroscopy of the X-Ray Transient 4U An Investigation into the Nature of the hr Periodic Source 4U An IR, Optical and X-Ray Study of the Two State Behaviour of GX An EXOSAT Observation of the Peculiar X-Ray Binary.

This is a partial list of known accretion-powered pulsars, as of   X-ray binaries are a special class of binary stars.

They are made up of a normal star and a collapsed star (a white dwarf, neutron star, or black hole). These pairs of stars produce X-rays if the stars are in close enough proximity that material is pulled off the normal star by the gravity.

of the dense, collapsed star. The additional material. List of X-ray pulsars. This is a partial list of known accretion-powered pulsars, as of (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S.

National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National.Binary pulsars arise when a neutron star is formed in a binary the system remains bound after the supernova explosion, there exists (for a short time) a normal pulsar in an eccentric orbit around a main sequence star (the secondary).

If the secondary expands at the end of its main sequence lifetime, it can transfer matter to the neutron star companion, causing the system to exist for.Other articles where Binary pulsar is discussed: Arecibo Observatory: Arecibo to discover the first binary pulsar.

They showed that it was losing energy through gravitational radiation at the rate predicted by physicist Albert Einstein’s theory of general relativity, and they won the Nobel Prize for Physics in for their discovery.

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